[{"month":"01","article_type":"original","oa_version":"Published Version","status":"public","ddc":["520"],"article_number":"A147","OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202555596","author":[{"orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"first_name":"Tanya","full_name":"Urrutia, Tanya","last_name":"Urrutia"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"first_name":"Francesco","last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco"},{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"orcid":"0000-0001-8386-3546","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","full_name":"Iani, Edoardo","last_name":"Iani"},{"first_name":"Yuzo","full_name":"Ishikawa, Yuzo","last_name":"Ishikawa"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"full_name":"Kotiwale, Gauri","last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"}],"day":"14","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"EDP Sciences","volume":705,"file":[{"creator":"dernst","checksum":"3782e03bc0843438aae8487f6af779c5","success":1,"file_name":"2026_AstronomyAstrophysics_Torralba.pdf","file_size":2259914,"relation":"main_file","access_level":"open_access","content_type":"application/pdf","file_id":"21224","date_updated":"2026-02-16T07:35:03Z","date_created":"2026-02-16T07:35:03Z"}],"citation":{"chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>.","ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy and Astrophysics. 705, A147.","mla":"Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy and Astrophysics</i>, vol. 705, A147, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy and Astrophysics</i>. 2026;705. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke, M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke, S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa, R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy and Astrophysics 705 (2026).","ieee":"A. Torralba Torregrosa <i>et al.</i>, “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” <i>Astronomy and Astrophysics</i>, vol. 705. EDP Sciences, 2026."},"publication_status":"published","scopus_import":"1","intvolume":"       705","_id":"21045","type":"journal_article","has_accepted_license":"1","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-02-16T07:35:03Z","article_processing_charge":"No","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2026-01-14T00:00:00Z","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"corr_author":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"We thank the anonymous referee for constructive and useful comments. We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge funding from JWST program GO-3516. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #3516. MG thanks the Max Planck Society for support through the MPRG. FDE acknowledges support by the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.","publication":"Astronomy and Astrophysics","date_created":"2026-01-25T23:01:41Z","year":"2026","date_updated":"2026-02-16T07:46:53Z","abstract":[{"text":"The abundant population of little red dots (LRDs), compact objects with red UV to optical colors and broad Balmer lines at high redshift, is revealing new insights into the properties of early active galactic nuclei (AGN). Perhaps the most surprising features of this population are the presence of Balmer absorption and ubiquitous strong Balmer breaks. Recent models link these features to an active supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We present a stringent test of such models using VLT/MUSE observations of A2744-45924, the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744 lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula (h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc. The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα) compared to Lyα nebulae typically observed around quasars of similar luminosity. We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered by star formation. In the environment of A2744-45924, we identified four extended Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations based on Hα emission, and show no evidence for radiation from A2744-45924 affecting its surroundings. The lack of strong, compact, and broad Lyα and the absence of a luminous extended halo, suggest that the UV AGN light is obscured by dense gas cloaking the SMBH with a covering factor close to unity.","lang":"eng"}],"PlanS_conform":"1","external_id":{"arxiv":["2505.09542"]}},{"intvolume":"       706","_id":"21160","type":"journal_article","has_accepted_license":"1","OA_type":"diamond","file_date_updated":"2026-02-16T09:33:56Z","language":[{"iso":"eng"}],"tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"title":"The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy","article_processing_charge":"No","date_published":"2026-02-01T00:00:00Z","department":[{"_id":"IlCa"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank Lars Bildsten for valuable insights and discussions. We acknowledge with thanks the variable star observations from the\r\nAAVSO International Database contributed by observers worldwide and used in this research. We thank the members of the Spanish Observers of Supernovae\r\n(ObSN) group for their valuable photometric contributions. This research was\r\nsupported by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC 2121 “Quantum Universe”\r\n– 390833306. Co-funded by the European Union (ERC, CompactBINARIES,\r\n101078773). Views and opinions expressed are however those of the author(s)\r\nonly and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority\r\ncan be held responsible for them. DB acknowledges support from the São Paulo\r\nResearch Foundation (FAPESP), Brazil, Process Numbers #2024/03736-2 and\r\n#2025/00817-4. MRS is supported by Fondecyt (grant 1221059). MJG acknowledges support from the European Research Council through ERC Advanced\r\nGrant No. 101054731, from the National Aeronautics and Space Administration under grants 80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380,\r\nand from the National Science Foundation under grant AST-2205736. PJG\r\nis supported by NRF SARChI grant 111692. PR-G acknowledges support by\r\nthe Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación\r\n(MCIN/AEI) and the European Regional Development Fund (ERDF) under grant\r\nPID2021–124879NB–I00. DS is supported by the UK Science and Technology Facilities Council (STFC, grant numbers ST/T007184/1, ST/T003103/1,\r\nand ST/T000406/1). OT acknowledges Proyectos Internos USM 2025, PI-LII2025-03. GT was supported by grants IN109723 from the Programa de Apoyo a\r\nProyectos de Investigación e Innovación Tecnológica (PAPIIT). This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057).","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"date_updated":"2026-02-16T09:36:24Z","year":"2026","publication":"Astronomy and Astrophysics","date_created":"2026-02-08T23:02:49Z","abstract":[{"lang":"eng","text":"Context. AM Canum Venaticorum (AM CVn) stars are ultra-compact binary systems composed of a white dwarf primary accreting from a hydrogen-deficient donor. They play a crucial role in astrophysics as potential progenitors of Type Ia supernovae and as laboratories for gravitational wave studies. However, their formation and evolutionary history remain incomplete. Three formation channels have been discussed in the literature: the white dwarf, He-star, and cataclysmic variable channels.\r\n\r\nAims. The chemical composition of the accretor atmosphere reflects the material transferred from the donor. In this work we took the first accurate measurements of the fundamental parameters of the accreting white dwarf in ZTF J225237.05−051917.4, including the abundances of key elements such as carbon, nitrogen, and silicon, by analysing ultraviolet spectra obtained with the Hubble Space Telescope (HST). These measurements provide new insight into the evolutionary history of the system and, together with existing optical observations, establish it as a benchmark to develop our pipeline, paving the way for its application to a larger sample of AM CVn systems.\r\n\r\nMethods. We determined the binary parameters through photometric analysis and constrained the atmospheric parameters of the white dwarf accretor, including its effective temperature, surface gravity, and chemical abundances, by fitting the HST ultraviolet spectrum with synthetic spectral models. We then inferred the system’s formation channel by comparing the results with theoretical evolutionary models.\r\n\r\nResults. According to our measurements, the accretor’s effective temperature (Teff) is 23 300 ± 600 K and the surface gravity (log g) is 8.4 ± 0.3, which imply an accretor mass (MWD) of 0.86 ± 0.16 M⊙. We find a high nitrogen-to-carbon abundance ratio by mass of > 153.\r\n\r\nConclusions. The accretor is significantly hotter than previous estimates based on simplified blackbody fits to the spectral energy distribution, underscoring the importance of detailed spectral modelling for accurately determining system parameters. Our results show that ultraviolet spectroscopy is well suited to constraining the formation channels of AM CVn systems. Of the three proposed formation channels, the He-star channel can be excluded given the high nitrogen-to-carbon ratio. Our results are consistent with both the white dwarf and cataclysmic variable channels."}],"PlanS_conform":"1","external_id":{"arxiv":["2512.04147"]},"article_type":"original","month":"02","oa_version":"Published Version","status":"public","article_number":"A14","ddc":["520"],"OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202557568","author":[{"first_name":"W.","last_name":"Yu","full_name":"Yu, W."},{"first_name":"A. F.","last_name":"Pala","full_name":"Pala, A. F."},{"first_name":"T.","last_name":"Kupfer","full_name":"Kupfer, T."},{"first_name":"B. T.","last_name":"Gänsicke","full_name":"Gänsicke, B. T."},{"first_name":"D.","full_name":"Koester, D.","last_name":"Koester"},{"first_name":"D.","last_name":"Belloni","full_name":"Belloni, D."},{"last_name":"Wong","full_name":"Wong, T. L.S.","first_name":"T. L.S."},{"first_name":"M. R.","full_name":"Schreiber, M. R.","last_name":"Schreiber"},{"first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","last_name":"van Roestel","full_name":"van Roestel, Joannes C"},{"first_name":"A. J.","full_name":"Brown, A. J.","last_name":"Brown"},{"full_name":"Waagen, E. O.","last_name":"Waagen","first_name":"E. O."},{"full_name":"González-Carballo, J. L.","last_name":"González-Carballo","first_name":"J. L."},{"full_name":"Bednarz, S.","last_name":"Bednarz","first_name":"S."},{"first_name":"K.","full_name":"Bernacki, K.","last_name":"Bernacki"},{"last_name":"De Martino","full_name":"De Martino, D.","first_name":"D."},{"last_name":"Fernández Mañanes","full_name":"Fernández Mañanes, E.","first_name":"E."},{"full_name":"González Farfán, R.","last_name":"González Farfán","first_name":"R."},{"first_name":"M. J.","last_name":"Green","full_name":"Green, M. J."},{"first_name":"P. J.","full_name":"Groot, P. J.","last_name":"Groot"},{"last_name":"Hambsch","full_name":"Hambsch, F. J.","first_name":"F. J."},{"full_name":"Knigge, C.","last_name":"Knigge","first_name":"C."},{"last_name":"Martin-Velasco","full_name":"Martin-Velasco, J. L.","first_name":"J. L."},{"last_name":"Morales-Aimar","full_name":"Morales-Aimar, M.","first_name":"M."},{"full_name":"Myers, G.","last_name":"Myers","first_name":"G."},{"first_name":"R.","full_name":"Naves Nogues, R.","last_name":"Naves Nogues"},{"last_name":"Poggiani","full_name":"Poggiani, R.","first_name":"R."},{"first_name":"A.","full_name":"Popowicz, A.","last_name":"Popowicz"},{"first_name":"G.","full_name":"Ramsay, G.","last_name":"Ramsay"},{"full_name":"Reina-Lorenz, E.","last_name":"Reina-Lorenz","first_name":"E."},{"full_name":"Rodríguez-Gil, P.","last_name":"Rodríguez-Gil","first_name":"P."},{"full_name":"Salto-González, J. L.","last_name":"Salto-González","first_name":"J. L."},{"first_name":"E. M.","last_name":"Sion","full_name":"Sion, E. M."},{"first_name":"D.","full_name":"Steeghs, D.","last_name":"Steeghs"},{"last_name":"Szkody","full_name":"Szkody, P.","first_name":"P."},{"first_name":"O.","last_name":"Toloza","full_name":"Toloza, O."},{"last_name":"Tovmassian","full_name":"Tovmassian, G.","first_name":"G."}],"day":"01","publisher":"EDP Sciences","volume":706,"file":[{"creator":"dernst","checksum":"2faec710fd04f927aa43deb57e35c9b2","success":1,"file_name":"2026_AstronomyAstrophysics_Yu.pdf","relation":"main_file","access_level":"open_access","file_size":4020466,"content_type":"application/pdf","date_created":"2026-02-16T09:33:56Z","date_updated":"2026-02-16T09:33:56Z","file_id":"21227"}],"citation":{"ieee":"W. Yu <i>et al.</i>, “The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy,” <i>Astronomy and Astrophysics</i>, vol. 706. EDP Sciences, 2026.","apa":"Yu, W., Pala, A. F., Kupfer, T., Gänsicke, B. T., Koester, D., Belloni, D., … Tovmassian, G. (2026). The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557568\">https://doi.org/10.1051/0004-6361/202557568</a>","short":"W. Yu, A.F. Pala, T. Kupfer, B.T. Gänsicke, D. Koester, D. Belloni, T.L.S. Wong, M.R. Schreiber, J.C. van Roestel, A.J. Brown, E.O. Waagen, J.L. González-Carballo, S. Bednarz, K. Bernacki, D. De Martino, E. Fernández Mañanes, R. González Farfán, M.J. Green, P.J. Groot, F.J. Hambsch, C. Knigge, J.L. Martin-Velasco, M. Morales-Aimar, G. Myers, R. Naves Nogues, R. Poggiani, A. Popowicz, G. Ramsay, E. Reina-Lorenz, P. Rodríguez-Gil, J.L. Salto-González, E.M. Sion, D. Steeghs, P. Szkody, O. Toloza, G. Tovmassian, Astronomy and Astrophysics 706 (2026).","ama":"Yu W, Pala AF, Kupfer T, et al. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. <i>Astronomy and Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557568\">10.1051/0004-6361/202557568</a>","ista":"Yu W, Pala AF, Kupfer T, Gänsicke BT, Koester D, Belloni D, Wong TLS, Schreiber MR, van Roestel JC, Brown AJ, Waagen EO, González-Carballo JL, Bednarz S, Bernacki K, De Martino D, Fernández Mañanes E, González Farfán R, Green MJ, Groot PJ, Hambsch FJ, Knigge C, Martin-Velasco JL, Morales-Aimar M, Myers G, Naves Nogues R, Poggiani R, Popowicz A, Ramsay G, Reina-Lorenz E, Rodríguez-Gil P, Salto-González JL, Sion EM, Steeghs D, Szkody P, Toloza O, Tovmassian G. 2026. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy and Astrophysics. 706, A14.","mla":"Yu, W., et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” <i>Astronomy and Astrophysics</i>, vol. 706, A14, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557568\">10.1051/0004-6361/202557568</a>.","chicago":"Yu, W., A. F. Pala, T. Kupfer, B. T. Gänsicke, D. Koester, D. Belloni, T. L.S. Wong, et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557568\">https://doi.org/10.1051/0004-6361/202557568</a>."},"publication_status":"published","scopus_import":"1"},{"month":"02","article_type":"original","oa_version":"Published Version","status":"public","ddc":["520"],"article_number":"A188","OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202556432","author":[{"last_name":"Cristea","full_name":"Cristea, Andrei-Alexandru","id":"4d500bea-31f8-11ee-a48d-d4904fb363c7","first_name":"Andrei-Alexandru"},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388"},{"first_name":"Tim","last_name":"Cunningham","full_name":"Cunningham, Tim"},{"full_name":"Raymond, John C.","last_name":"Raymond","first_name":"John C."},{"last_name":"Vennes","full_name":"Vennes, Stephane","first_name":"Stephane"},{"full_name":"Kawka, Adela","last_name":"Kawka","first_name":"Adela"},{"id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","first_name":"Aayush A","full_name":"Desai, Aayush A","last_name":"Desai"},{"first_name":"David R.","full_name":"Miller, David R.","last_name":"Miller"},{"last_name":"Hermes","full_name":"Hermes, J. J.","first_name":"J. J."},{"first_name":"Jim","full_name":"Fuller, Jim","last_name":"Fuller"},{"full_name":"Heyl, Jeremy","last_name":"Heyl","first_name":"Jeremy"},{"first_name":"Jan","full_name":"van Roestel, Jan","last_name":"van Roestel"},{"last_name":"Burdge","full_name":"Burdge, Kevin B.","first_name":"Kevin B."},{"full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez","first_name":"Antonio C."},{"full_name":"Pelisoli, Ingrid","last_name":"Pelisoli","first_name":"Ingrid"},{"first_name":"Boris T.","last_name":"Gänsicke","full_name":"Gänsicke, Boris T."},{"first_name":"Paula","full_name":"Szkody, Paula","last_name":"Szkody"},{"first_name":"Scott J.","last_name":"Kenyon","full_name":"Kenyon, Scott J."},{"first_name":"Zach","last_name":"Vanderbosch","full_name":"Vanderbosch, Zach"},{"first_name":"Andrew","full_name":"Drake, Andrew","last_name":"Drake"},{"last_name":"Ferrario","full_name":"Ferrario, Lilia","first_name":"Lilia"},{"last_name":"Wickramasinghe","full_name":"Wickramasinghe, Dayal","first_name":"Dayal"},{"full_name":"Karambelkar, Viraj R.","last_name":"Karambelkar","first_name":"Viraj R."},{"last_name":"Justham","full_name":"Justham, Stephen","first_name":"Stephen"},{"full_name":"Pakmor, Ruediger","last_name":"Pakmor","first_name":"Ruediger"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"full_name":"Prince, Thomas","last_name":"Prince","first_name":"Thomas"},{"first_name":"S. R.","last_name":"Kulkarni","full_name":"Kulkarni, S. R."},{"last_name":"Graham","full_name":"Graham, Matthew J.","first_name":"Matthew J."},{"last_name":"Masci","full_name":"Masci, Frank J.","first_name":"Frank J."},{"full_name":"Groom, Steven L.","last_name":"Groom","first_name":"Steven L."},{"first_name":"Josiah","full_name":"Purdum, Josiah","last_name":"Purdum"},{"first_name":"Richard","last_name":"Dekany","full_name":"Dekany, Richard"},{"first_name":"Eric C.","last_name":"Bellm","full_name":"Bellm, Eric C."}],"day":"10","related_material":{"link":[{"url":"https://ista.ac.at/en/news/twos-company-new-class-of-star-remnants/","relation":"press_release","description":"News on ISTA website"}]},"publisher":"EDP Sciences","volume":706,"file":[{"file_id":"21350","date_updated":"2026-02-23T12:04:37Z","date_created":"2026-02-23T12:04:37Z","content_type":"application/pdf","access_level":"open_access","file_size":5352853,"relation":"main_file","file_name":"2026_AstronomyAstrophysics_Cristea.pdf","success":1,"checksum":"229b688e6e78cab5bb8e2bac366d1575","creator":"dernst"}],"citation":{"ieee":"A.-A. Cristea <i>et al.</i>, “A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant,” <i>Astronomy &#38; Astrophysics</i>, vol. 706. EDP Sciences, 2026.","mla":"Cristea, Andrei-Alexandru, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” <i>Astronomy &#38; Astrophysics</i>, vol. 706, A188, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556432\">10.1051/0004-6361/202556432</a>.","ista":"Cristea A-A, Caiazzo I, Cunningham T, Raymond JC, Vennes S, Kawka A, Desai AA, Miller DR, Hermes JJ, Fuller J, Heyl J, van Roestel J, Burdge KB, Rodriguez AC, Pelisoli I, Gänsicke BT, Szkody P, Kenyon SJ, Vanderbosch Z, Drake A, Ferrario L, Wickramasinghe D, Karambelkar VR, Justham S, Pakmor R, El-Badry K, Prince T, Kulkarni SR, Graham MJ, Masci FJ, Groom SL, Purdum J, Dekany R, Bellm EC. 2026. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. Astronomy &#38; Astrophysics. 706, A188.","chicago":"Cristea, Andrei-Alexandru, Ilaria Caiazzo, Tim Cunningham, John C. Raymond, Stephane Vennes, Adela Kawka, Aayush A Desai, et al. “A Half Ring of Ionized Circumstellar Material Trapped in the Magnetosphere of a White Dwarf Merger Remnant.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202556432\">https://doi.org/10.1051/0004-6361/202556432</a>.","ama":"Cristea A-A, Caiazzo I, Cunningham T, et al. A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. <i>Astronomy &#38; Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556432\">10.1051/0004-6361/202556432</a>","short":"A.-A. Cristea, I. Caiazzo, T. Cunningham, J.C. Raymond, S. Vennes, A. Kawka, A.A. Desai, D.R. Miller, J.J. Hermes, J. Fuller, J. Heyl, J. van Roestel, K.B. Burdge, A.C. Rodriguez, I. Pelisoli, B.T. Gänsicke, P. Szkody, S.J. Kenyon, Z. Vanderbosch, A. Drake, L. Ferrario, D. Wickramasinghe, V.R. Karambelkar, S. Justham, R. Pakmor, K. El-Badry, T. Prince, S.R. Kulkarni, M.J. Graham, F.J. Masci, S.L. Groom, J. Purdum, R. Dekany, E.C. Bellm, Astronomy &#38; Astrophysics 706 (2026).","apa":"Cristea, A.-A., Caiazzo, I., Cunningham, T., Raymond, J. C., Vennes, S., Kawka, A., … Bellm, E. C. (2026). A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556432\">https://doi.org/10.1051/0004-6361/202556432</a>"},"publication_status":"published","DOAJ_listed":"1","intvolume":"       706","type":"journal_article","_id":"21274","has_accepted_license":"1","OA_type":"gold","language":[{"iso":"eng"}],"file_date_updated":"2026-02-23T12:04:37Z","article_processing_charge":"Yes","title":"A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2026-02-10T00:00:00Z","department":[{"_id":"IlCa"},{"_id":"GradSch"}],"user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","corr_author":"1","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"We thank Lynne Hillenbrand and Soumyadeep Bhattacharjee for helpful discussions, and Kishalay De for his help with the WIRC\r\nreduction pipeline. IC was supported by NASA through grants from the Space\r\nTelescope Science Institute, under NASA contracts NASA.22K1813, NAS5-\r\n26555 and NAS5-03127. TC was supported by NASA through the NASA Hubble\r\nFellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research\r\nin Astronomy, Inc., for NASA, under contract NAS5-26555. This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057). This work was based on observations obtained with the\r\nSamuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar\r\nObservatory as part of the Zwicky Transient Facility project. ZTF is supported\r\nby the National Science Foundation under Grants No. AST-1440341, AST2034437, and currently Award #2407588. ZTF receives additional funding from\r\nthe ZTF partnership. Current members include Caltech, USA; Caltech/IPAC,\r\nUSA; University of Maryland, USA; University of California, Berkeley, USA;\r\nUniversity of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel\r\nUniversity, USA; University of North Carolina at Chapel Hill, USA; Institute\r\nof Science and Technology, Austria; National Central University, Taiwan, and\r\nOKC, University of Stockholm, Sweden. Operations are conducted by Caltech’s\r\nOptical Observatory (COO), Caltech/IPAC, and the University of Washington at\r\nSeattle, USA. This work has made use of data from the European Space Agency\r\n(ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by\r\nthe Gaia Data Processing and Analysis Consortium (DPAC, https://www.\r\ncosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys (PS1)\r\nand the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the PanSTARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck\r\nInstitute for Extraterrestrial Physics, Garching, The Johns Hopkins University,\r\nDurham University, the University of Edinburgh, the Queen’s University Belfast,\r\nthe 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\r\nthe Planetary Science Division of the NASA Science Mission Directorate, the\r\nNational Science Foundation Grant No. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory,\r\nand the Gordon and Betty Moore Foundation. This work made use of Astropy\r\n(http://www.astropy.org): a community-developed core Python package\r\nand an ecosystem of tools and resources for astronomy (Astropy Collaboration\r\n2013, 2018, 2022).","publication":"Astronomy & Astrophysics","date_created":"2026-02-17T08:12:05Z","date_updated":"2026-04-28T12:01:21Z","year":"2026","abstract":[{"lang":"eng","text":"Many white dwarfs are observed in compact double white dwarf binaries, and through the emission of gravitational waves, a large fraction are destined to merge. The merger remnants that do not explode in a Type Ia supernova are expected to initially be rapidly rotating and highly magnetized. In this work, we present our discovery of the variable white dwarf ZTF J200832.79+444939.67, hereafter ZTF J2008+4449, as a likely merger remnant showing signs of circumstellar material without a stellar or substellar companion. The nature of ZTF J2008+4449 as a merger remnant is supported by its physical properties: it is hot (35 500 ± 300 K) and massive (1.12 ± 0.03 M\r\n                    <jats:sub>⊙</jats:sub>\r\n                    ), rapidly rotating with a period of ≈6.6 minutes, and likely possesses exceptionally strong magnetic fields (∼400−600 MG) at its surface. Remarkably, we detect a significant period derivative of (1.80 ± 0.09)×10\r\n                    <jats:sup>−12</jats:sup>\r\n                    s/s, indicating that the white dwarf is spinning down, and a soft X-ray emission that is inconsistent with photospheric emission. As the presence of a mass-transferring stellar or brown dwarf companion is excluded by infrared photometry, the detected spin-down and X-ray emission could be tell-tale signs of a magnetically driven wind or of interaction with circumstellar material, possibly originating from the fallback of gravitationally bound merger ejecta or from the tidal disruption of a planetary object. We also detect Balmer emission, which requires the presence of ionized hydrogen in the vicinity of the white dwarf, showing Doppler shifts as high as ≈2000 km s\r\n                    <jats:sup>−1</jats:sup>\r\n                    . The unusual variability of the Balmer emission on the spin period of the white dwarf is consistent with the trapping of a half ring of ionized gas in the magnetosphere of the white dwarf.\r\n                  </jats:p>"}],"PlanS_conform":"1"},{"date_published":"2026-02-01T00:00:00Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","article_processing_charge":"No","file_date_updated":"2026-02-24T07:46:47Z","language":[{"iso":"eng"}],"OA_type":"diamond","has_accepted_license":"1","type":"journal_article","_id":"21341","intvolume":"       706","PlanS_conform":"1","external_id":{"arxiv":["2510.19959"]},"abstract":[{"lang":"eng","text":"We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies."}],"date_updated":"2026-02-24T07:49:42Z","year":"2026","publication":"Astronomy & Astrophysics","date_created":"2026-02-22T23:01:35Z","acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations were taken under programmes # 1243, # 1933 and # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. GK acknowledges support from the Foundation MERAC. APV acknowledge support from the Sussex Astronomy Centre STFC Consolidated Grant (ST/X001040/1).","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"doi":"10.1051/0004-6361/202556597","quality_controlled":"1","OA_place":"publisher","article_number":"A165","ddc":["520"],"status":"public","oa_version":"Published Version","article_type":"original","month":"02","DOAJ_listed":"1","scopus_import":"1","publication_status":"published","citation":{"ama":"Kotiwale G, Matthee JJ, Kashino D, et al. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>","ista":"Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy &#38; Astrophysics. 706, A165.","chicago":"Kotiwale, Gauri, Jorryt J Matthee, Daichi Kashino, Aswin P. Vijayan, Alberto Torralba Torregrosa, Claudia Di Cesare, Edoardo Iani, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>.","mla":"Kotiwale, Gauri, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 706, A165, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>.","short":"G. Kotiwale, J.J. Matthee, D. Kashino, A.P. Vijayan, A. Torralba Torregrosa, C. Di Cesare, E. Iani, R. Bordoloi, J. Leja, M.V. Maseda, S. Tacchella, I. Shivaei, K.E. Heintz, A.L. Danhaive, S. Mascia, I. Kramarenko, B. Navarrete, R. Mackenzie, R.P. Naidu, D. Sobral, Astronomy &#38; Astrophysics 706 (2026).","apa":"Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa, A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>","ieee":"G. Kotiwale <i>et al.</i>, “Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 706. EDP Sciences, 2026."},"file":[{"content_type":"application/pdf","date_created":"2026-02-24T07:46:47Z","date_updated":"2026-02-24T07:46:47Z","file_id":"21355","file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","access_level":"open_access","relation":"main_file","file_size":6531719,"checksum":"6f5849d29ad43bee32f90152f6fc0294","success":1,"creator":"dernst"}],"volume":706,"publisher":"EDP Sciences","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"day":"01","author":[{"id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","last_name":"Kotiwale","full_name":"Kotiwale, Gauri"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"last_name":"Vijayan","full_name":"Vijayan, Aswin P.","first_name":"Aswin P."},{"full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto","orcid":"0000-0001-5586-6950"},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"last_name":"Iani","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"last_name":"Bordoloi","full_name":"Bordoloi, Rongmon","first_name":"Rongmon"},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"full_name":"Danhaive, A. Lola","last_name":"Danhaive","first_name":"A. Lola"},{"full_name":"Mascia, Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara"},{"first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín","last_name":"Navarrete"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"}]},{"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","department":[{"_id":"JoMa"}],"external_id":{"arxiv":["2512.08484"]},"abstract":[{"text":"Context. Extreme emission line galaxies (EELGs) are believed to significantly contribute to the star formation activity and mass assembly in galaxies. EELGs likely also play a leading role in the cosmic re-ionization as their interstellar medium may allow a significant fraction of their ionizing photons to escape (> 5%). Finding low-redshift analogues of these high-z galaxies is therefore essential to characterizing the physical conditions in the interstellar medium of these galaxies and understanding the processes that re-ionized the Universe.\r\n\r\nAims. We aimed to develop a robust and efficient method for the photometric identification of EELGs using the J-PAS survey. J-PAS will cover approximately 8500 deg2 of the sky with 54 narrow-band filters in the optical range plus i-SDSS, enabling detailed studies of the physical properties of these galaxies. In this work we focused on an initial subset of the survey: a 30 square degree area with complete observations in all bands.\r\n\r\nMethods. We combine equivalent width (EW) measurements from J-PAS narrow-band photometry with artificial intelligence techniques to identify galaxies with emission lines exceeding 300 Å. We validated our selection using spectroscopic data from DESI DR1 and characterized the selected sample through spectral energy distribution fitting with CIGALE.\r\n\r\nResults. We identify 917 EELGs up to z = 0.8 over 30 deg2, achieving a purity of 95% and a completeness of 96% for i-SDSS < 22.5 mag. Importantly, active galactic nucleus contamination was carefully considered and is estimated to be around 5%. Furthermore, a cross-match with DESI yielded 79 counterparts; their redshifts are in excellent agreement with our photometric estimates, thereby confirming the reliability of our redshift determination. In addition, the derived emission line fluxes are in good agreement with spectroscopic measurements. Moreover, the selected sample reveals strong correlations between the ionizing photon production efficiency (ξion) and EW(Hβ), which are consistent with previous observational studies at low and high redshifts and theoretical expectations. Finally, most of the sources surpass the ionizing efficiency threshold required for re-ionization, highlighting their relevance as local analogues of early-Universe galaxies.","lang":"eng"}],"date_updated":"2026-03-02T15:10:27Z","year":"2026","date_created":"2026-03-02T10:06:10Z","publication":"Astronomy & Astrophysics","acknowledgement":"We thank the referee for several helpful suggestions. AGA, MGO and IM acknowledge financial support from the Severo Ochoa grant CEX2021-001131-S, funded by MICIU/AEI/10.13039/501100011033. AGA also acknowledges FPI support under grant code CEX2021-001131-S20-7. Both AGA and MGO acknowledge support from the research grant\r\nPID2022-136598NB-C32 (“Estallidos8”). MGO also acknowledges the support by the project ref. AST22_00001_Subp_11 funded from the EU – NextGenerationEU. RA acknowledges support from PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and ERDF/EU. IM acknowledges support from PID2022-140871NB-C21 funded by MICIU/AEI/10.13039/501100011033 and FEDER/UE. RGD acknowledge financial support from the project PID2022-141755NB-I00, and the Severo Ochoa grant CEX2021-001131-S funded\r\nby MICIU/AEI/ 10.13039/501100011033. JAFO and AE acknowledge support from the Spanish Ministry of Science and Innovation and the EU–NextGenerationEU through the RRF project ICTS-MRR-2021-03-CEFCA. AHC and ALC acknowledge support from MCIN/AEI/10.13039/501100011033, “ERDF A way of making Europe”, and “EU NextGenerationEU/PRTR” through PID2021-124918NB-C44 and CNS2023-145339, as well as from the RRF project ICTS-MRR-2021-03-CEFCA ALC and RPT acknowledge the financial\r\nsupport from the European Union – NextGenerationEU through the RRF program Planes Complementarios con las CCAA de Astrofísica y Física de Altas Energías – LA4. I.B. acknowledges support from the EU Horizon 2020 programme (Marie Sklodowska-Curie Grant 101059532) and the Franziska Seidl Funding Program, University of Vienna. This paper has gone through internal‘ review by the J-PAS collaboration. Based on observations made with the\r\nJST/T250 telescope and JPCam at the Observatorio Astrofísico de Javalambre (OAJ), in Teruel, owned, managed, and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). We acknowledge the OAJ Data Processing and Archiving Unit (UPAD) for reducing and calibrating the OAJ data used in this work. Funding for the J-PAS Project has been provided by the Governments of Spain and Aragón through the Fondo de Inversiones de Teruel; the Aragonese Government through the Research Groups E96, E103, E16_17R, E16_20R, and E16_23R; the Spanish Ministry of Science and Innovation (MCIN/AEI/10.13039/501100011033 y FEDER, Una manera de hacer Europa) with grants PID2021-124918NB-C41, PID2021-124918NB-C42, PID2021-124918NA-C43, and PID2021-124918NB-C44; the Spanish Ministry\r\nof Science, Innovation and Universities (MCIU/AEI/FEDER, UE) with grants\r\nPGC2018-097585-B-C21 and PGC2018-097585-B-C22; the Spanish Ministry of Economy and Competitiveness (MINECO) under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, and AYA2012-30789; and European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685).","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"has_accepted_license":"1","_id":"21380","type":"journal_article","intvolume":"       706","date_published":"2026-02-01T00:00:00Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"No","title":"J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies","file_date_updated":"2026-03-02T14:51:57Z","language":[{"iso":"eng"}],"OA_type":"diamond","volume":706,"publisher":"EDP Sciences","day":"01","author":[{"first_name":"A.","last_name":"Giménez-Alcázar","full_name":"Giménez-Alcázar, A."},{"last_name":"Amorín","full_name":"Amorín, R.","first_name":"R."},{"first_name":"J. M.","full_name":"Vílchez, J. M.","last_name":"Vílchez"},{"first_name":"A.","last_name":"Hernán-Caballero","full_name":"Hernán-Caballero, A."},{"first_name":"M.","last_name":"González-Otero","full_name":"González-Otero, M."},{"first_name":"A.","full_name":"Arroyo-Polonio, A.","last_name":"Arroyo-Polonio"},{"first_name":"J.","last_name":"Iglesias-Páramo","full_name":"Iglesias-Páramo, J."},{"first_name":"A.","last_name":"Lumbreras-Calle","full_name":"Lumbreras-Calle, A."},{"first_name":"J. A.","last_name":"Fernández-Ontiveros","full_name":"Fernández-Ontiveros, J. A."},{"first_name":"C.","full_name":"López-Sanjuan, C.","last_name":"López-Sanjuan"},{"last_name":"Bonatto","full_name":"Bonatto, L.","first_name":"L."},{"first_name":"R. M.","last_name":"González Delgado","full_name":"González Delgado, R. M."},{"first_name":"C.","full_name":"Kehrig, C.","last_name":"Kehrig"},{"first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa"},{"last_name":"Rahna","full_name":"Rahna, P. T.","first_name":"P. T."},{"first_name":"Y.","last_name":"Jiménez-Teja","full_name":"Jiménez-Teja, Y."},{"first_name":"I.","last_name":"Márquez","full_name":"Márquez, I."},{"first_name":"I.","full_name":"Breda, I.","last_name":"Breda"},{"first_name":"A.","last_name":"Álvarez-Candal","full_name":"Álvarez-Candal, A."},{"last_name":"Abramo","full_name":"Abramo, R.","first_name":"R."},{"full_name":"Alcaniz, J.","last_name":"Alcaniz","first_name":"J."},{"first_name":"N.","full_name":"Benitez, N.","last_name":"Benitez"},{"full_name":"Bonoli, S.","last_name":"Bonoli","first_name":"S."},{"first_name":"S.","full_name":"Carneiro, S.","last_name":"Carneiro"},{"full_name":"Cenarro, J.","last_name":"Cenarro","first_name":"J."},{"full_name":"Cristóbal-Hornillos, D.","last_name":"Cristóbal-Hornillos","first_name":"D."},{"first_name":"R.","full_name":"Dupke, R.","last_name":"Dupke"},{"full_name":"Ederoclite, A.","last_name":"Ederoclite","first_name":"A."},{"first_name":"C.","full_name":"Hernández-Monteagudo, C.","last_name":"Hernández-Monteagudo"},{"first_name":"A.","last_name":"Marín-Franch","full_name":"Marín-Franch, A."},{"first_name":"C.","full_name":"Mendes de Oliveira, C.","last_name":"Mendes de Oliveira"},{"first_name":"M.","full_name":"Moles, M.","last_name":"Moles"},{"full_name":"Sodré, L.","last_name":"Sodré","first_name":"L."},{"first_name":"K.","last_name":"Taylor","full_name":"Taylor, K."},{"last_name":"Varela","full_name":"Varela, J.","first_name":"J."},{"first_name":"H.","full_name":"Vázquez Ramió, H.","last_name":"Vázquez Ramió"}],"DOAJ_listed":"1","scopus_import":"1","publication_status":"published","citation":{"apa":"Giménez-Alcázar, A., Amorín, R., Vílchez, J. M., Hernán-Caballero, A., González-Otero, M., Arroyo-Polonio, A., … Vázquez Ramió, H. (2026). J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557358\">https://doi.org/10.1051/0004-6361/202557358</a>","short":"A. Giménez-Alcázar, R. Amorín, J.M. Vílchez, A. Hernán-Caballero, M. González-Otero, A. Arroyo-Polonio, J. Iglesias-Páramo, A. Lumbreras-Calle, J.A. Fernández-Ontiveros, C. López-Sanjuan, L. Bonatto, R.M. González Delgado, C. Kehrig, A. Torralba Torregrosa, P.T. Rahna, Y. Jiménez-Teja, I. Márquez, I. Breda, A. Álvarez-Candal, R. Abramo, J. Alcaniz, N. Benitez, S. Bonoli, S. Carneiro, J. Cenarro, D. Cristóbal-Hornillos, R. Dupke, A. Ederoclite, C. Hernández-Monteagudo, A. Marín-Franch, C. Mendes de Oliveira, M. Moles, L. Sodré, K. Taylor, J. Varela, H. Vázquez Ramió, Astronomy &#38; Astrophysics 706 (2026).","chicago":"Giménez-Alcázar, A., R. Amorín, J. M. Vílchez, A. Hernán-Caballero, M. González-Otero, A. Arroyo-Polonio, J. Iglesias-Páramo, et al. “J-PAS: First Identification, Physical Properties, and Ionization Efficiency of Extreme Emission Line Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557358\">https://doi.org/10.1051/0004-6361/202557358</a>.","ista":"Giménez-Alcázar A, Amorín R, Vílchez JM, Hernán-Caballero A, González-Otero M, Arroyo-Polonio A, Iglesias-Páramo J, Lumbreras-Calle A, Fernández-Ontiveros JA, López-Sanjuan C, Bonatto L, González Delgado RM, Kehrig C, Torralba Torregrosa A, Rahna PT, Jiménez-Teja Y, Márquez I, Breda I, Álvarez-Candal A, Abramo R, Alcaniz J, Benitez N, Bonoli S, Carneiro S, Cenarro J, Cristóbal-Hornillos D, Dupke R, Ederoclite A, Hernández-Monteagudo C, Marín-Franch A, Mendes de Oliveira C, Moles M, Sodré L, Taylor K, Varela J, Vázquez Ramió H. 2026. J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. Astronomy &#38; Astrophysics. 706, A261.","mla":"Giménez-Alcázar, A., et al. “J-PAS: First Identification, Physical Properties, and Ionization Efficiency of Extreme Emission Line Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 706, A261, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557358\">10.1051/0004-6361/202557358</a>.","ama":"Giménez-Alcázar A, Amorín R, Vílchez JM, et al. J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies. <i>Astronomy &#38; Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557358\">10.1051/0004-6361/202557358</a>","ieee":"A. Giménez-Alcázar <i>et al.</i>, “J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 706. EDP Sciences, 2026."},"file":[{"content_type":"application/pdf","date_created":"2026-03-02T14:51:57Z","file_id":"21391","date_updated":"2026-03-02T14:51:57Z","file_name":"2026_AstronomyAstrophysics_GimenezAlcazar.pdf","access_level":"open_access","file_size":1813456,"relation":"main_file","checksum":"cd25a05386ab5638ae5baf8add0ecbee","success":1,"creator":"dernst"}],"article_number":"A261","ddc":["520"],"status":"public","oa_version":"Published Version","article_type":"original","month":"02","doi":"10.1051/0004-6361/202557358","quality_controlled":"1","OA_place":"publisher"},{"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"acknowledgement":"We thank our anonymous referee for carefully reading the manuscript and providing a constructive report with helpful feedback. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #1233. The specific observations analyzed can be accessed via DOI: 10.17909/3c1d-6182. Moreover, this research is based in part on observations made with the NASA/ESA Hubble Space Telescope obtained from the\r\nSpace 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 #13664, GO-10915, and DD-11307. This research was supported in part by grant NSF PHY-2309135 to the Kavli Institute for Theoretical Physics (KITP). LRP acknowledges support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41 funded\r\nby MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. LRP acknowledges support from grant PID2022-140483NB-C22 funded by MCIN/AEI/10.13039/501100011033.","publication":"Astronomy & Astrophysics","date_created":"2026-03-15T23:01:35Z","date_updated":"2026-03-16T09:07:55Z","year":"2026","abstract":[{"lang":"eng","text":"Stellar wind mass loss of massive stars is often assumed to depend on their metallicity Z. Therefore, evolutionary models predict that massive stars in lower-Z environments are able to retain more of their hydrogen-rich layers and evolve into brighter cool supergiants (cool SGs; Teff < 7 kK). Surprisingly, in galaxies in the metallicity range 0.2 ≲ Z/Z⊙ ≲ 1.5, previous studies have not found a metallicity dependence on the upper luminosity limit Lmax of cool SGs. Here, we add four galaxies to the sample studied for this purpose with data from the Hubble Space Telescope and the James Webb Space Telescope (JWST). Observations of the extremely metal-poor dwarf galaxy I Zw 18 from JWST allow us to extend the studied metallicity range down to Z/Z⊙ ≈ 1/40. For cool SGs in all studied galaxies, including I Zw 18, we find a constant value of Lmax ≈ 105.6 L⊙, similar to literature results for 0.2 ≲ Z/Z⊙ ≲ 1.5. In I Zw 18 and the other studied galaxies, the presence of Wolf-Rayet stars has been previously inferred. Although we cannot rule out that some of them become intermediate-temperature objects, this paints a picture in which evolved stars with L > 105.6 L⊙ burn helium as hot, helium-rich stars down to extremely low metallicity. We argue that metallicity-independent late-phase mass loss would be the most likely mechanism responsible for this. Regardless of the exact stripping mechanism (winds or, for example, binary interaction), for the Early Universe our results imply a limitation on black hole masses and a contribution of stars born with M ≳ 30 M⊙ to its surprisingly strong nitrogen enrichment. We propose a scenario in which single stars at low metallicity emit sufficiently hard ionizing radiation to produce He II and C IV lines. In this scenario, late-phase metallicity-independent mass loss produces hot, helium-rich stars. Due to the well-understood metallicity dependence on the radiation-driven winds of hot stars, a window of opportunity would open below 0.2 Z⊙, where self-stripped helium-rich stars can exist without dense Wolf-Rayet winds that absorb hard ionizing radiation."}],"PlanS_conform":"1","external_id":{"arxiv":["2510.12594"]},"department":[{"_id":"YlGo"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-03-16T09:05:06Z","title":"A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2026-03-01T00:00:00Z","intvolume":"       707","type":"journal_article","_id":"21450","has_accepted_license":"1","file":[{"file_id":"21455","date_updated":"2026-03-16T09:05:06Z","date_created":"2026-03-16T09:05:06Z","content_type":"application/pdf","relation":"main_file","file_size":2102107,"access_level":"open_access","file_name":"2026_AstronomyAstrophysics_Schootemeijer.pdf","success":1,"checksum":"02a0cd932340207c96fdd3059490ad29","creator":"dernst"}],"citation":{"short":"A. Schootemeijer, Y.L.L. Götberg, N. Langer, G. Bortolini, A.S. Hirschauer, L. Patrick, Astronomy &#38; Astrophysics 707 (2026).","apa":"Schootemeijer, A., Götberg, Y. L. L., Langer, N., Bortolini, G., Hirschauer, A. S., &#38; Patrick, L. (2026). A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557675\">https://doi.org/10.1051/0004-6361/202557675</a>","chicago":"Schootemeijer, Abel, Ylva Louise Linsdotter Götberg, Norbert Langer, Giacomo Bortolini, Alec S. Hirschauer, and Lee Patrick. “A Constant Upper Luminosity Limit of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557675\">https://doi.org/10.1051/0004-6361/202557675</a>.","ista":"Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick L. 2026. A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. Astronomy &#38; Astrophysics. 707, A116.","mla":"Schootemeijer, Abel, et al. “A Constant Upper Luminosity Limit of Cool Supergiant Stars down to the Extremely Low Metallicity of I Zw 18.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A116, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557675\">10.1051/0004-6361/202557675</a>.","ama":"Schootemeijer A, Götberg YLL, Langer N, Bortolini G, Hirschauer AS, Patrick L. A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557675\">10.1051/0004-6361/202557675</a>","ieee":"A. Schootemeijer, Y. L. L. Götberg, N. Langer, G. Bortolini, A. S. Hirschauer, and L. Patrick, “A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026."},"publication_status":"published","scopus_import":"1","DOAJ_listed":"1","author":[{"first_name":"Abel","full_name":"Schootemeijer, Abel","last_name":"Schootemeijer"},{"last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"full_name":"Langer, Norbert","last_name":"Langer","first_name":"Norbert"},{"first_name":"Giacomo","full_name":"Bortolini, Giacomo","last_name":"Bortolini"},{"first_name":"Alec S.","last_name":"Hirschauer","full_name":"Hirschauer, Alec S."},{"first_name":"Lee","last_name":"Patrick","full_name":"Patrick, Lee"}],"day":"01","publisher":"EDP Sciences","volume":707,"OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202557675","month":"03","article_type":"original","oa_version":"Published Version","status":"public","ddc":["520"],"article_number":"A116"},{"volume":707,"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"EDP Sciences","day":"01","author":[{"orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"last_name":"Ishikawa","full_name":"Ishikawa, Yuzo","first_name":"Yuzo"},{"last_name":"Brammer","full_name":"Brammer, Gabriel B.","first_name":"Gabriel B."},{"first_name":"Seok Jun","full_name":"Chang, Seok Jun","last_name":"Chang"},{"last_name":"Chisholm","full_name":"Chisholm, John","first_name":"John"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"Francesco","last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco"},{"full_name":"Di Cesare, Claudia","last_name":"Di Cesare","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Iani, Edoardo","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"first_name":"Vasily","full_name":"Kokorev, Vasily","last_name":"Kokorev"},{"first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","last_name":"Kotiwale"},{"orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"full_name":"Ma, Yilun","last_name":"Ma","first_name":"Yilun"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara"},{"full_name":"Navarrete, Benjamín","last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"last_name":"Nelson","full_name":"Nelson, Erica","first_name":"Erica"},{"first_name":"Pascal","last_name":"Oesch","full_name":"Oesch, Pascal"},{"first_name":"Robert A.","last_name":"Simcoe","full_name":"Simcoe, Robert A."},{"full_name":"Wuyts, Stijn","last_name":"Wuyts","first_name":"Stijn"}],"DOAJ_listed":"1","scopus_import":"1","publication_status":"published","file":[{"date_updated":"2026-03-16T10:57:49Z","file_id":"21460","date_created":"2026-03-16T10:57:49Z","content_type":"application/pdf","relation":"main_file","access_level":"open_access","file_size":2510157,"file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","success":1,"checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","creator":"dernst"}],"citation":{"ieee":"A. Torralba Torregrosa <i>et al.</i>, “The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>.","ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy &#38; Astrophysics. 707, A75.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>","mla":"Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A75, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>.","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa, Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa, G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko, Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy &#38; Astrophysics 707 (2026)."},"article_number":"A75","ddc":["520"],"status":"public","oa_version":"Published Version","article_type":"original","month":"03","doi":"10.1051/0004-6361/202557537","quality_controlled":"1","OA_place":"publisher","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","department":[{"_id":"JoMa"}],"PlanS_conform":"1","external_id":{"arxiv":["2510.00103"]},"abstract":[{"lang":"eng","text":"The population of the little red dots (LRDs) may represent a key phase of supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging as a key component to explain the most striking properties of LRDs, such as strong Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission. We revealed a forest of optical [Fe II] lines, which we argue are emerging from a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K. The broad wings of Hα and Hβ have an exponential profile due to electron scattering in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an indicator of collisional excitation and resonant scattering dominating the Balmer line emission. A narrow Hγ component, unseen in the other two Balmer lines due to outshining by the broad components, could trace the ISM of a normal host galaxy with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer transitions, producing a characteristic P Cygni profile in the line centers suggesting outflowing motions. This same layer is responsible for shaping the Balmer break. The broadband spectrum can be reasonably matched by a simple photoionized slab model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy that could explain the narrow [O III], with only a subdominant contribution to the UV continuum. Our findings indicate that Balmer lines are not directly tracing the gas kinematics near the SMBH and that the BH mass scale is likely much lower than virial indicators suggest."}],"year":"2026","date_updated":"2026-03-16T10:59:16Z","date_created":"2026-03-15T23:01:36Z","publication":"Astronomy & Astrophysics","acknowledgement":"We thank the scientific referee for useful and constructive comments. We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics of gaseous envelopes and accretion into black holes. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #5664. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"has_accepted_license":"1","type":"journal_article","_id":"21451","intvolume":"       707","date_published":"2026-03-01T00:00:00Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"No","title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","language":[{"iso":"eng"}],"file_date_updated":"2026-03-16T10:57:49Z","OA_type":"diamond"},{"publication_status":"published","file":[{"file_size":1821411,"relation":"main_file","access_level":"open_access","file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","date_updated":"2026-03-16T10:48:07Z","file_id":"21459","date_created":"2026-03-16T10:48:07Z","content_type":"application/pdf","creator":"dernst","success":1,"checksum":"c056b00ce7324849754521fde10fb7ca"}],"citation":{"apa":"Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko, I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>","short":"C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko, J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak, K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella, Astronomy &#38; Astrophysics 707 (2026).","ista":"Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I, Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy &#38; Astrophysics. 707, A129.","mla":"Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A129, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>.","ama":"Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>","chicago":"Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba, Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>.","ieee":"C. Di Cesare <i>et al.</i>, “The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026."},"scopus_import":"1","DOAJ_listed":"1","day":"01","author":[{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Alberto","full_name":"Torralba, Alberto","last_name":"Torralba"},{"last_name":"Kotiwale","full_name":"Kotiwale, Gauri","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"},{"first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"last_name":"Blaizot","full_name":"Blaizot, Jeremy","first_name":"Jeremy"},{"last_name":"Rosdahl","full_name":"Rosdahl, Joakim","first_name":"Joakim"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Iani, Edoardo","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz","first_name":"Alba"},{"first_name":"Lukas J.","full_name":"Furtak, Lukas J.","last_name":"Furtak"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"full_name":"Mascia, Sara","last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"last_name":"Navarrete","full_name":"Navarrete, Benjamín","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"first_name":"Michael","last_name":"Romano","full_name":"Romano, Michael"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"},{"first_name":"Sandro","last_name":"Tacchella","full_name":"Tacchella, Sandro"}],"volume":707,"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"EDP Sciences","OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202557790","oa_version":"Published Version","month":"03","article_type":"original","ddc":["520"],"article_number":"A129","status":"public","publication":"Astronomy & Astrophysics","date_created":"2026-03-15T23:01:36Z","year":"2026","date_updated":"2026-03-16T10:52:44Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion, Pierluigi Rinaldi for his help with data handling and Luca Graziani and William McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program # 3516. We acknowledge funding from JWST program GO-3516. Software used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant 2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy Collaboration 2013).","PlanS_conform":"1","external_id":{"arxiv":["2510.19044"]},"abstract":[{"text":"Galaxies exhibit a tight correlation between their star formation rate (SFR) and stellar mass over a wide redshift range known as the star-forming main sequence (SFMS). With JWST, the SFMS can now be investigated at high redshifts down to masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα emission, which allow us to probe the variability in the star formation histories. We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5 with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell 2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α, with α = 0.45). After we corrected this for the Hα-flux limited nature of our survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09, whereas current data on their own are inconclusive on the mass dependence of the scatter. These slopes differ significantly from the slope of ∼1 that is expected from the observed evolution of the galaxy stellar mass function and from simulations. When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010 M⊙). This difference might be explained by a (combination of) luminosity-dependent SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated dust attenuation in high-mass galaxies. Future deep observations with different facilities can quantify these processes, which will enable us to achieve better insights into the variability of the star formation histories.","lang":"eng"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","oa":1,"file_date_updated":"2026-03-16T10:48:07Z","language":[{"iso":"eng"}],"OA_type":"diamond","date_published":"2026-03-01T00:00:00Z","title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":"       707","has_accepted_license":"1","_id":"21452","type":"journal_article"},{"file":[{"checksum":"7429076b381dd498084f40ffd199e714","success":1,"creator":"dernst","content_type":"application/pdf","date_updated":"2026-03-23T15:44:09Z","file_id":"21492","date_created":"2026-03-23T15:44:09Z","file_name":"2026_AstronomyAstrophysics_Kramarenko.pdf","relation":"main_file","file_size":904565,"access_level":"open_access"}],"citation":{"ieee":"I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare, “H α as a tracer of star formation in the SPHINX cosmological simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","short":"I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy &#38; Astrophysics 707 (2026).","apa":"Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., &#38; Di Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>","mla":"Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A184, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>.","ama":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>","ista":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026. H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy &#38; Astrophysics. 707, A184.","chicago":"Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>."},"publication_status":"published","DOAJ_listed":"1","author":[{"orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan"},{"first_name":"J.","last_name":"Rosdahl","full_name":"Rosdahl, J."},{"full_name":"Blaizot, J.","last_name":"Blaizot","first_name":"J."},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"first_name":"H.","last_name":"Katz","full_name":"Katz, H."},{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"}],"day":"05","publisher":"EDP Sciences","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"volume":707,"OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202557114","article_type":"original","month":"03","oa_version":"Published Version","status":"public","article_number":"A184","ddc":["520"],"acknowledgement":"We thank the anonymous referee for the insightful comments that helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala for useful comments and productive discussions. We gratefully acknowledge support from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work made extensive use of several open-source software packages, and we gratefully acknowledge the efforts of their authors: numpy (Harris et al. 2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez & Granger 2007), and scikit-learn (Pedregosa et al. 2011).","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"year":"2026","date_updated":"2026-03-23T15:46:31Z","date_created":"2026-03-23T14:58:03Z","publication":"Astronomy & Astrophysics","abstract":[{"text":"The Hα emission line in galaxies is a powerful tracer of their recent star formation activity. With the advent of JWST, we are now able to routinely observe Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs leads to biased results because high-redshift galaxies are commonly characterized by low metallicities and bursty star formation histories, affecting the conversion factor between the Hα luminosity (LHα) and the SFR. We developed a set of new SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3 with very little error. We used the SPHINX cosmological simulations to select a sample of star-forming galaxies representative of the Hα-emitter population observed with JWST. We then derived linear corrections to the classical SFR(Hα) calibrations that took variations in the physical properties (e.g., stellar metallicities) among individual galaxies into account. We obtained two new SFR(Hα) calibrations that compared to the classical calibrations reduce the root mean squared error (RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively. Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show that the new calibrations affect the high-redshift galaxy population statistics: (i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.","lang":"eng"}],"external_id":{"arxiv":["2509.05403"]},"PlanS_conform":"1","department":[{"_id":"JoMa"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-03-23T15:44:09Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"No","title":"H α as a tracer of star formation in the SPHINX cosmological simulations","date_published":"2026-03-05T00:00:00Z","intvolume":"       707","_id":"21481","type":"journal_article","has_accepted_license":"1"},{"OA_place":"publisher","doi":"10.1051/0004-6361/202558023","quality_controlled":"1","month":"03","article_type":"original","oa_version":"Published Version","status":"public","ddc":["520"],"article_number":"A321","file":[{"file_id":"21664","date_updated":"2026-04-07T09:00:50Z","date_created":"2026-04-07T09:00:50Z","content_type":"application/pdf","access_level":"open_access","file_size":12287607,"relation":"main_file","file_name":"2026_AstronomyAstrophysics_Liagre.pdf","success":1,"checksum":"560cac19dc70184626b85e71a26ee22e","creator":"dernst"}],"citation":{"chicago":"Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>.","ama":"Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. <i>Astronomy and Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202558023\">10.1051/0004-6361/202558023</a>","ista":"Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy and Astrophysics. 707, A321.","mla":"Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” <i>Astronomy and Astrophysics</i>, vol. 707, A321, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202558023\">10.1051/0004-6361/202558023</a>.","short":"B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics 707 (2026).","apa":"Liagre, B. R. B., Desai, A. A., Einramhof, L., &#38; Bugnet, L. A. (2026). Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>","ieee":"B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting,” <i>Astronomy and Astrophysics</i>, vol. 707. EDP Sciences, 2026."},"publication_status":"published","scopus_import":"1","DOAJ_listed":"1","author":[{"last_name":"Liagre","full_name":"Liagre, Bastien Raymond Bernard","id":"662f1873-cab4-11f0-a719-8087d302868d","first_name":"Bastien Raymond Bernard"},{"full_name":"Desai, Aayush A","last_name":"Desai","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","first_name":"Aayush A"},{"full_name":"Einramhof, Lukas","last_name":"Einramhof","first_name":"Lukas","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c"},{"first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"}],"day":"01","publisher":"EDP Sciences","volume":707,"OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-04-07T09:00:50Z","title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2026-03-01T00:00:00Z","intvolume":"       707","_id":"21658","type":"journal_article","has_accepted_license":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"arxiv":1,"acknowledgement":"We thank the referee for their careful and constructive report, which has substantially enhanced both the quality and clarity of the manuscript. L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N°101165631). While partially funded by the European Union, views and opinions expressed are, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. The authors acknowledge the great support and feedback provided during the redaction of this article by Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt for her insights on uncertainty estimates. The authors also thank the members of the Asteroseismology and Stellar Dynamics group of the Institute of Science and Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K. Smith. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013, 2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017), slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011), sloscillations (Kuszlewicz et al. 2019, 2023).","date_created":"2026-04-05T22:01:32Z","publication":"Astronomy and Astrophysics","date_updated":"2026-04-07T09:01:44Z","year":"2026","abstract":[{"lang":"eng","text":"Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes."}],"external_id":{"arxiv":["2511.05314 "]},"PlanS_conform":"1","department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","oa":1},{"status":"public","article_number":"L16","ddc":["520"],"article_type":"letter_editor","month":"03","oa_version":"Published Version","quality_controlled":"1","doi":"10.1051/0004-6361/202659309","OA_place":"publisher","project":[{"_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"publisher":"Wiley","volume":707,"author":[{"last_name":"Breton","full_name":"Breton, S. N.","first_name":"S. N."},{"first_name":"C.","last_name":"Pezzotti","full_name":"Pezzotti, C."},{"full_name":"Mathis, S.","last_name":"Mathis","first_name":"S."},{"full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle"},{"full_name":"Di Mauro, M. P.","last_name":"Di Mauro","first_name":"M. P."},{"last_name":"Joergensen","full_name":"Joergensen, J.","first_name":"J."},{"last_name":"Zwintz","full_name":"Zwintz, K.","first_name":"K."},{"first_name":"A. F.","full_name":"Lanza, A. F.","last_name":"Lanza"}],"day":"01","DOAJ_listed":"1","scopus_import":"1","file":[{"access_level":"open_access","relation":"main_file","file_size":1535506,"file_name":"2026_AstronomyAstrophysics_Breton.pdf","date_created":"2026-04-07T09:20:02Z","file_id":"21666","date_updated":"2026-04-07T09:20:02Z","content_type":"application/pdf","creator":"dernst","success":1,"checksum":"a7fd798bf450d67d4166fdf54ff2c70c"}],"citation":{"apa":"Breton, S. N., Pezzotti, C., Mathis, S., Bugnet, L. A., Di Mauro, M. P., Joergensen, J., … Lanza, A. F. (2026). Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>. Wiley. <a href=\"https://doi.org/10.1051/0004-6361/202659309\">https://doi.org/10.1051/0004-6361/202659309</a>","short":"S.N. Breton, C. Pezzotti, S. Mathis, L.A. Bugnet, M.P. Di Mauro, J. Joergensen, K. Zwintz, A.F. Lanza, Astronomy &#38; Astrophysics 707 (2026).","mla":"Breton, S. N., et al. “Core-Envelope Coupling of Gravito-Inertial Waves in Pre-Main-Sequence Solar-Type Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, L16, Wiley, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202659309\">10.1051/0004-6361/202659309</a>.","ama":"Breton SN, Pezzotti C, Mathis S, et al. Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202659309\">10.1051/0004-6361/202659309</a>","chicago":"Breton, S. N., C. Pezzotti, S. Mathis, Lisa Annabelle Bugnet, M. P. Di Mauro, J. Joergensen, K. Zwintz, and A. F. Lanza. “Core-Envelope Coupling of Gravito-Inertial Waves in Pre-Main-Sequence Solar-Type Stars.” <i>Astronomy &#38; Astrophysics</i>. Wiley, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202659309\">https://doi.org/10.1051/0004-6361/202659309</a>.","ista":"Breton SN, Pezzotti C, Mathis S, Bugnet LA, Di Mauro MP, Joergensen J, Zwintz K, Lanza AF. 2026. Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars. Astronomy &#38; Astrophysics. 707, L16.","ieee":"S. N. Breton <i>et al.</i>, “Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. Wiley, 2026."},"publication_status":"published","_id":"21659","type":"journal_article","has_accepted_license":"1","intvolume":"       707","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"title":"Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars","article_processing_charge":"No","date_published":"2026-03-01T00:00:00Z","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-04-07T09:20:02Z","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","department":[{"_id":"LiBu"}],"abstract":[{"lang":"eng","text":"The recent detection of solar equatorial Rossby waves has renewed interest in the study of gravito-inertial waves propagating in the convective envelope of solar-type stars. In particular, the ability of these envelope gravito-inertial modes to couple with those trapped in the radiative interior could open up new opportunities for probing the deep-layer dynamics of solar-type stars. The possibility for such a coupling to occur is particularly favoured among pre-main-sequence (PMS) solar-type stars. Indeed, due to the contraction of the protostellar object, they are able to reach high rotation frequencies before nuclear reactions are ignited and magnetic braking becomes the driving mechanism for their rotational evolution. In this work, we studied the coupling between the envelope inertial waves and the radiative interior g modes in PMS stars, focussing on the case of prograde dipolar modes. We considered the cases of 0.5 M⊙ and 1 M⊙ PMS models, each with three different scenarios of rotational evolution. We show that for stars that have formed with a sufficient amount of angular momentum, this coupling can occur in frequency ranges that are accessible to space-borne photometry, creating inertial dips in the period spacing pattern. Using an asymptotic analysis, we characterised the shape of these inertial dips to show that they depend on rotation and on the stiffness of the convective-radiative interface."}],"PlanS_conform":"1","external_id":{"arxiv":["2603.01979"]},"acknowledgement":"The authors want to thank the anonymous referee for useful comments. SNB acknowledges support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase D”. SNB and AFL acknowledge support from the INAF grant MASTODINT. CP thanks the Belgian Federal Science Policy Office (BELSPO) for the financial support in the framework of the PRODEX Program of the European Space Agency (ESA) under contract number 4000141194. S.M acknowledges support from the CNES GOLF-SOHO and PLATO grants at CEA/DAp. LB and SM gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe programme (LB: Calcifer; Starting Grant agreement N°101165631; SM: 4D-STAR; Synergy Grant agreement N°101071505). While partially funded by the European Union, views and opinions expressed are, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. The authors acknowledge G. Buldgen, H. Dhouib, and M.A. Dupret for fruitful discussions.","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_updated":"2026-04-07T09:23:27Z","year":"2026","publication":"Astronomy & Astrophysics","date_created":"2026-04-05T22:01:32Z"},{"abstract":[{"text":"Context. Beta Pictoris is an A-type star that hosts a complex planetary system with two massive gas giants and a prominent debris disc. Variable absorption lines in its stellar spectrum have been interpreted as signatures of exocomets – comet-like bodies transiting the star. Stellar flybys can gravitationally perturb objects in the outer comet reservoir, altering their orbits and potentially injecting them into the inner system, thereby triggering exocomet showers.\r\nAims. We assessed the contribution of stellar flybys to the observed exocomet activity by reconstructing the stellar encounter history of β Pictoris in the past and future.\r\nMethods. We used Gaia DR3 data, supplemented with radial velocities from complementary spectroscopic surveys, to compile a catalogue of stars currently within 80 pc of β Pictoris. Their orbits were integrated backwards and forwards in time in an axisymmetric Galactic potential (via the GALA package) to identify encounters within 2 pc of the system.\r\nResults. We identified 99 416 stars currently within 80 pc of β Pictoris with resolved kinematics. Among these, 49 stars (including the eight components of five binaries) encounter β Pictoris within 2 pc between –1.5 Myr and +2 Myr. For four of the binaries, the centre-of-mass trajectories also pass within 2 pc. We estimated the sample to be more than 60% complete within 0.5 Myr of today.\r\nConclusions. Despite β Pictoris being the eponym of its famous moving group, none of the identified encounters involved its moving group members; all are unrelated field stars. We found no encounter capable of shaping the observed disc structures, although stellar flybys may contribute to the long-term evolution of an Oort Cloud-like structure. Our catalogue constitutes the most complete reconstruction of the β Pictoris encounter history to date and provides a robust foundation for future dynamical simulations.","lang":"eng"}],"external_id":{"arxiv":["2510.02509"]},"PlanS_conform":"1","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"We thank the referee for their suggestions and comments, which helped us improve the quality and clarity of the paper. JLGM and EV acknowledge the support from the Spanish Ministry of Science and Innovation/State Agency of Research (MCIN/AEI) under the grant PID2021-127289-NB-I00. ST acknowledges the funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413. AJM acknowledges support from the Swedish National Space Agency (Career Grant 2023-00146) and from the Swedish Research Council (Project Grant 2022-04043). JLGM also sincerely thanks AMP for his careful final reading of this manuscript. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We acknowledge the use of the public data products from RAVE (https://www.rave-survey.org), GALAH (https://galah-survey.org), APOGEE ((https://www.sdss.org) and LAMOST (http://www.lamost.org) surveys. This research has also made use of the SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg, France, as well as the NASA Astrophysics Data System Bibliographic Services and the arXiv pre-print server operated by Cornell University. Computational analyses in this work relied extensively on the NumPy and SciPy libraries for numerical computing, matplotlib and seaborn for data visualization, and the Gala package for Galactic dynamics. This work also made use of Astropy, a community-developed core PYTHON package and an ecosystem of tools and resources for astronomy. We thank the developers and maintainers of these open-source resources for their invaluable contributions to the astronomical community.","publication":"Astronomy & Astrophysics","date_created":"2026-01-04T23:01:34Z","date_updated":"2026-02-16T12:15:07Z","year":"2025","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"department":[{"_id":"LiBu"}],"title":"A kinematic history of stellar encounters with Beta Pictoris","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-12-01T00:00:00Z","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-01-05T11:06:16Z","_id":"20930","type":"journal_article","has_accepted_license":"1","intvolume":"       704","ec_funded":1,"scopus_import":"1","DOAJ_listed":"1","citation":{"ieee":"J. L. Gragera-Más, S. Torres Rodriguez, A. J. Mustill, and E. Villaver, “A kinematic history of stellar encounters with Beta Pictoris,” <i>Astronomy &#38; Astrophysics</i>, vol. 704. EDP Sciences, 2025.","chicago":"Gragera-Más, J. L., Santiago Torres Rodriguez, A. J. Mustill, and E. Villaver. “A Kinematic History of Stellar Encounters with Beta Pictoris.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202555940\">https://doi.org/10.1051/0004-6361/202555940</a>.","ista":"Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. 2025. A kinematic history of stellar encounters with Beta Pictoris. Astronomy &#38; Astrophysics. 704, A237.","mla":"Gragera-Más, J. L., et al. “A Kinematic History of Stellar Encounters with Beta Pictoris.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A237, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202555940\">10.1051/0004-6361/202555940</a>.","ama":"Gragera-Más JL, Torres Rodriguez S, Mustill AJ, Villaver E. A kinematic history of stellar encounters with Beta Pictoris. <i>Astronomy &#38; Astrophysics</i>. 2025;704. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555940\">10.1051/0004-6361/202555940</a>","short":"J.L. Gragera-Más, S. Torres Rodriguez, A.J. Mustill, E. Villaver, Astronomy &#38; Astrophysics 704 (2025).","apa":"Gragera-Más, J. L., Torres Rodriguez, S., Mustill, A. J., &#38; Villaver, E. (2025). A kinematic history of stellar encounters with Beta Pictoris. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555940\">https://doi.org/10.1051/0004-6361/202555940</a>"},"file":[{"checksum":"2fb4d5a1603043aa7931a31f2c180877","success":1,"creator":"dernst","content_type":"application/pdf","date_created":"2026-01-05T11:06:16Z","file_id":"20942","date_updated":"2026-01-05T11:06:16Z","file_name":"2025_AstronomyAstrophysics_GrageraMas.pdf","relation":"main_file","access_level":"open_access","file_size":11021467}],"publication_status":"published","project":[{"_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020","grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program"}],"publisher":"EDP Sciences","volume":704,"author":[{"first_name":"J. L.","last_name":"Gragera-Más","full_name":"Gragera-Más, J. L."},{"last_name":"Torres Rodriguez","full_name":"Torres Rodriguez, Santiago","orcid":"0000-0002-3150-8988","first_name":"Santiago","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2"},{"first_name":"A. J.","last_name":"Mustill","full_name":"Mustill, A. J."},{"full_name":"Villaver, E.","last_name":"Villaver","first_name":"E."}],"day":"01","doi":"10.1051/0004-6361/202555940","quality_controlled":"1","OA_place":"publisher","status":"public","ddc":["520"],"article_number":"A237","month":"12","article_type":"original","oa_version":"Published Version"},{"publisher":"EDP Sciences","project":[{"name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","grant_number":"101034413","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"},{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","grant_number":"101165631","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9"}],"volume":704,"author":[{"full_name":"Mombarg, J. S.G.","last_name":"Mombarg","first_name":"J. S.G."},{"last_name":"Vanlaer","full_name":"Vanlaer, V.","first_name":"V."},{"full_name":"Das, Srijan B","last_name":"Das","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","first_name":"Srijan B","orcid":"0000-0003-0896-7972"},{"full_name":"Rieutord, M.","last_name":"Rieutord","first_name":"M."},{"first_name":"C.","full_name":"Aerts, C.","last_name":"Aerts"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"},{"first_name":"S.","full_name":"Mathis, S.","last_name":"Mathis"},{"last_name":"Reese","full_name":"Reese, D. R.","first_name":"D. R."},{"last_name":"Ballot","full_name":"Ballot, J.","first_name":"J."}],"day":"19","related_material":{"record":[{"id":"20936","status":"public","relation":"research_data"}]},"ec_funded":1,"scopus_import":"1","DOAJ_listed":"1","citation":{"ista":"Mombarg JSG, Vanlaer V, Das SB, Rieutord M, Aerts C, Bugnet LA, Mathis S, Reese DR, Ballot J. 2025. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. Astronomy &#38; Astrophysics. 704, A336.","ama":"Mombarg JSG, Vanlaer V, Das SB, et al. Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>. 2025;704. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557247\">10.1051/0004-6361/202557247</a>","chicago":"Mombarg, J. S.G., V. Vanlaer, Srijan B Das, M. Rieutord, C. Aerts, Lisa Annabelle Bugnet, S. Mathis, D. R. Reese, and J. Ballot. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202557247\">https://doi.org/10.1051/0004-6361/202557247</a>.","mla":"Mombarg, J. S. G., et al. “Is a 1D Perturbative Method Sufficient for Asteroseismic Modelling of β Cephei Pulsators? Implications for Measurements of Rotation and Internal Magnetic Fields.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A336, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557247\">10.1051/0004-6361/202557247</a>.","apa":"Mombarg, J. S. G., Vanlaer, V., Das, S. B., Rieutord, M., Aerts, C., Bugnet, L. A., … Ballot, J. (2025). Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557247\">https://doi.org/10.1051/0004-6361/202557247</a>","short":"J.S.G. Mombarg, V. Vanlaer, S.B. Das, M. Rieutord, C. Aerts, L.A. Bugnet, S. Mathis, D.R. Reese, J. Ballot, Astronomy &#38; Astrophysics 704 (2025).","ieee":"J. S. G. Mombarg <i>et al.</i>, “Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields,” <i>Astronomy &#38; Astrophysics</i>, vol. 704. EDP Sciences, 2025."},"file":[{"file_name":"2025_AstronomyAstrophysics_Mombarg.pdf","relation":"main_file","access_level":"open_access","file_size":2620909,"content_type":"application/pdf","date_updated":"2026-01-05T08:36:28Z","file_id":"20937","date_created":"2026-01-05T08:36:28Z","creator":"dernst","checksum":"d838b4783920c43b7cc866e9cf08b383","success":1}],"publication_status":"published","status":"public","ddc":["520"],"article_number":"A336","month":"12","article_type":"original","oa_version":"Published Version","quality_controlled":"1","doi":"10.1051/0004-6361/202557247","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"department":[{"_id":"LiBu"}],"abstract":[{"text":"Context. Asymmetries in the observed rotational splittings of a multiplet contain information about the star’s rotation profile and internal magnetic field. Moreover, the frequency regularities of multiplets can be used for mode identification. However, to exploit this information, highly accurate theoretical predictions are needed.\r\n\r\nAims. We aim to quantify the difference in the predicted mode asymmetries between a 1D perturbative method and a 2D method that includes a 2D stellar structure model, which takes rotation into account. We then place these differences between 1D and 2D methods in the context of asteroseismic measurements of internal magnetic fields. We only focus on the asymmetries and not on possible additional frequency peaks that can arise when the magnetic and rotation axis are misaligned.\r\n\r\nMethods. We coupled the 1D pulsation codes GYRE and StORM to the 2D stellar structure code ESTER and compared the oscillation predictions with the results from the 2D TOP pulsation code. We focused on zero-age main-sequence models representative of rotating β Cephei pulsators spinning at up to 20 per cent of the critical Keplerian rotation rate. Specifically, we investigated low-radial-order gravity and pressure modes.\r\n\r\nResults. We find a generally good agreement between the oscillation frequencies resulting from the 1D and 2D pulsation codes. We report differences in predicted mode multiplet asymmetries of mostly below 0.06 d−1. Since the magnetic asymmetries are small compared to the differences in the rotational asymmetries resulting from the 1D and 2D predictions, accurate measurements of the magnetic field are in most cases challenging.\r\n\r\nConclusions. Differences in the predicted mode asymmetries of a rotating star between 1D perturbative methods and 2D non-perturbative methods can greatly hinder accurate measurements of internal magnetic fields in main-sequence pulsators with low-order modes. Nevertheless, reasonably accurate measurements could be possible with npg ≥ 2 modes if the internal rotation is roughly below 10 per cent of the Keplerian critical rotation frequency for (aligned) magnetic fields of the order of a few hundred kilogauss. While the differences between the 1D and 2D frequency predictions are mostly too large for internal magnetic field detections, the rotational asymmetries predicted by StORM are in general accurate enough for asteroseismic modelling of the stellar rotation in main-sequence stars with identified low-order modes.","lang":"eng"}],"external_id":{"arxiv":["2511.09617"]},"PlanS_conform":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"acknowledgement":"We thank the anonymous referee for their comments on the manuscript, Dario Fritzewski for providing the distribution of fractions of critical rotation for the β Cephei sample, and Zhao Guo for the discussions. The research leading to these results has received funding from the European Research Council (ERC) under the Horizon Europe programme (Synergy Grant agreement N°101071505: 4D-STAR). While partially funded by the European Union, views and opinions expressed are however those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. V.V. acknowledges support from the Research Foundation Flanders (FWO) under grant agreement N°1156923N (PhD Fellowship). S.B.D. acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement N°101034413. L.B. gratefully acknowledges support from the European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N°101165631). J.B., M.R., S.M. and J.S.G.M have been supported by CNES, focused on the preparation of the PLATO mission. Computations with ESTER and TOP have made use of the HPC resources from the CALMIP supercomputing centre (Grant 2023-P0107). This research made use of the numpy (Harris et al. 2020) and matplotlib (Hunter 2007) Python software packages.","publication":"Astronomy & Astrophysics","date_created":"2026-01-04T23:01:35Z","date_updated":"2026-02-16T12:14:36Z","year":"2025","type":"journal_article","_id":"20931","has_accepted_license":"1","intvolume":"       704","article_processing_charge":"No","title":"Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators? Implications for measurements of rotation and internal magnetic fields","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-12-19T00:00:00Z","OA_type":"diamond","file_date_updated":"2026-01-05T08:36:28Z","language":[{"iso":"eng"}]},{"DOAJ_listed":"1","scopus_import":"1","publication_status":"published","file":[{"creator":"dernst","checksum":"3e6061f3c4bfb521b3333ea4913c241a","success":1,"file_name":"2025_AstronomyAstrophysics_Liu.pdf","file_size":4642530,"relation":"main_file","access_level":"open_access","content_type":"application/pdf","date_updated":"2026-01-05T09:26:17Z","file_id":"20938","date_created":"2026-01-05T09:26:17Z"}],"citation":{"apa":"Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P., … Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556410\">https://doi.org/10.1051/0004-6361/202556410</a>","short":"Y. Liu, S. Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, A. Calabrò, K. Glazebrook, A. Henry, M. Llerena, E. Merlin, B. Metha, T. Nanayakkara, L. Napolitano, N. Roy, B. Siana, E. Vanzella, B. Vulcani, X. Wang, Astronomy &#38; Astrophysics 704 (2025).","ista":"Liu Y, Mascia S, Pentericci L, Watson P, Alavi A, Bergamini P, Bradač M, Calabrò A, Glazebrook K, Henry A, Llerena M, Merlin E, Metha B, Nanayakkara T, Napolitano L, Roy N, Siana B, Vanzella E, Vulcani B, Wang X. 2025. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy &#38; Astrophysics. 704, A328.","chicago":"Liu, Y., Sara Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202556410\">https://doi.org/10.1051/0004-6361/202556410</a>.","mla":"Liu, Y., et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A328, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556410\">10.1051/0004-6361/202556410</a>.","ama":"Liu Y, Mascia S, Pentericci L, et al. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>. 2025;704. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556410\">10.1051/0004-6361/202556410</a>","ieee":"Y. Liu <i>et al.</i>, “A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field,” <i>Astronomy &#38; Astrophysics</i>, vol. 704. EDP Sciences, 2025."},"volume":704,"publisher":"EDP Sciences","day":"01","author":[{"full_name":"Liu, Y.","last_name":"Liu","first_name":"Y."},{"full_name":"Mascia, Sara","last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"full_name":"Pentericci, L.","last_name":"Pentericci","first_name":"L."},{"full_name":"Watson, P.","last_name":"Watson","first_name":"P."},{"last_name":"Alavi","full_name":"Alavi, A.","first_name":"A."},{"last_name":"Bergamini","full_name":"Bergamini, P.","first_name":"P."},{"first_name":"M.","full_name":"Bradač, M.","last_name":"Bradač"},{"last_name":"Calabrò","full_name":"Calabrò, A.","first_name":"A."},{"full_name":"Glazebrook, K.","last_name":"Glazebrook","first_name":"K."},{"full_name":"Henry, A.","last_name":"Henry","first_name":"A."},{"first_name":"M.","last_name":"Llerena","full_name":"Llerena, M."},{"first_name":"E.","last_name":"Merlin","full_name":"Merlin, E."},{"first_name":"B.","full_name":"Metha, B.","last_name":"Metha"},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"first_name":"L.","full_name":"Napolitano, L.","last_name":"Napolitano"},{"first_name":"N.","full_name":"Roy, N.","last_name":"Roy"},{"first_name":"B.","last_name":"Siana","full_name":"Siana, B."},{"last_name":"Vanzella","full_name":"Vanzella, E.","first_name":"E."},{"full_name":"Vulcani, B.","last_name":"Vulcani","first_name":"B."},{"first_name":"X.","last_name":"Wang","full_name":"Wang, X."}],"doi":"10.1051/0004-6361/202556410","quality_controlled":"1","OA_place":"publisher","article_number":"A328","ddc":["520"],"status":"public","oa_version":"Published Version","article_type":"original","month":"12","PlanS_conform":"1","external_id":{"arxiv":["2507.11045"]},"abstract":[{"text":"Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial for understanding the properties of cosmic reionizers because the opacity of the intergalactic medium (IGM) prevents the direct detection of LyC emission from sources during the Epoch of Reionization (EoR). In this study, we confirm two new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03 and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively. These two LyC candidate leakers were detected in a catalog of 91 spectroscopically confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed properties that were proposed as indirect indicators of LyC emission, such as Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according to these properties, stacked the LyC observations of this subsample, and assessed the limits of the escape fractions in the stacks. We aim to enhance our understanding of LyC escape mechanisms and improve our predictions of the LyC fesc during the EoR by analyzing the individual candidates and the stacks in the context of the currently limited sample of known LyC leakers at z ∼ 3.","lang":"eng"}],"date_updated":"2026-02-16T12:14:52Z","year":"2025","publication":"Astronomy & Astrophysics","date_created":"2026-01-04T23:01:35Z","acknowledgement":"We acknowledge support from the National Science Foundation of China – 12225301, INAF Large grant “Spectroscopic survey with JWST” jand from PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and Postgraduate Scholarship Program under the grant of China Scholarship Council. P.W. and B.V. acknowledge support from the INAF Mini Grant ‘1.05.24.07.01 RSN1: Spatially Resolved Near-IR Emission of Intermediate-Redshift Jellyfish Galaxies’ (PI Watson). We acknowledge A. Acebron, C. Grillo, and P. Rosati for their fundamental contribution to the strong lensing analysis and results. We also extend our gratitude to the JWST and HST teams for their efforts in designing, building, and operating these transformative missions.","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","department":[{"_id":"JoMa"}],"date_published":"2025-12-01T00:00:00Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"No","title":"A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field","language":[{"iso":"eng"}],"file_date_updated":"2026-01-05T09:26:17Z","OA_type":"diamond","has_accepted_license":"1","type":"journal_article","_id":"20932","intvolume":"       704"},{"intvolume":"       701","type":"journal_article","_id":"21060","has_accepted_license":"1","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2026-02-09T07:28:08Z","article_processing_charge":"No","title":"Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-09-01T00:00:00Z","department":[{"_id":"JoMa"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","corr_author":"1","oa":1,"arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"acknowledgement":"This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GTO 1243, ERS 1345, DDT 2750, and GTO 1180, 1181, 3215, 1210, 1286. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge support from the INAF Large Grant 2022 “Extragalactic Surveys with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project 2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. RA acknowledges support of Grant PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results received the support of a fellowship from the “la Caixa” Foundation (ID 100010434). The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”.","publication":"Astronomy & Astrophysics","date_created":"2026-01-28T15:24:24Z","year":"2025","date_updated":"2026-02-09T07:33:46Z","abstract":[{"lang":"eng","text":"Compact, star-forming galaxies with high star formation rate surface densities (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigated the influence of galaxy morphology on LyC production and escape at redshifts 5 ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15 M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent with canonical expectations. Since direct measurements of fesc are not possible during the Epoch of  Reionization (EoR), we predicted fesc for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit, on average, modest predicted escape fractions (∼0.04). In addition, we evaluated the correlation between morphological features and LyC emission. Our findings indicate that neither ξion nor the predicted fesc values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape. "}],"external_id":{"arxiv":["2501.08268"]},"PlanS_conform":"1","month":"09","article_type":"original","oa_version":"Published Version","status":"public","ddc":["520"],"article_number":"A122","OA_place":"publisher","doi":"10.1051/0004-6361/202553760","quality_controlled":"1","author":[{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara"},{"first_name":"L.","last_name":"Pentericci","full_name":"Pentericci, L."},{"first_name":"M.","full_name":"Llerena, M.","last_name":"Llerena"},{"last_name":"Calabrò","full_name":"Calabrò, A.","first_name":"A."},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Flury","full_name":"Flury, S.","first_name":"S."},{"last_name":"Pacucci","full_name":"Pacucci, F.","first_name":"F."},{"last_name":"Jaskot","full_name":"Jaskot, A.","first_name":"A."},{"last_name":"Amorín","full_name":"Amorín, R. O.","first_name":"R. O."},{"full_name":"Bhatawdekar, R.","last_name":"Bhatawdekar","first_name":"R."},{"full_name":"Castellano, M.","last_name":"Castellano","first_name":"M."},{"first_name":"N.","full_name":"Cleri, N.","last_name":"Cleri"},{"first_name":"L.","last_name":"Costantin","full_name":"Costantin, L."},{"last_name":"Davis","full_name":"Davis, K.","first_name":"K."},{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"last_name":"Dickinson","full_name":"Dickinson, M.","first_name":"M."},{"first_name":"A.","full_name":"Fontana, A.","last_name":"Fontana"},{"last_name":"Guo","full_name":"Guo, Y.","first_name":"Y."},{"first_name":"M.","full_name":"Giavalisco, M.","last_name":"Giavalisco"},{"last_name":"Holwerda","full_name":"Holwerda, B. W.","first_name":"B. W."},{"first_name":"W.","last_name":"Hu","full_name":"Hu, W."},{"last_name":"Huertas-Company","full_name":"Huertas-Company, M.","first_name":"M."},{"first_name":"Intae","last_name":"Jung","full_name":"Jung, Intae"},{"first_name":"J.","last_name":"Kartaltepe","full_name":"Kartaltepe, J."},{"full_name":"Kashino, D.","last_name":"Kashino","first_name":"D."},{"first_name":"A. M.","last_name":"Koekemoer","full_name":"Koekemoer, A. M."},{"last_name":"Lucas","full_name":"Lucas, R. A.","first_name":"R. A."},{"first_name":"J.","full_name":"Lotz, J.","last_name":"Lotz"},{"first_name":"L.","last_name":"Napolitano","full_name":"Napolitano, L."},{"full_name":"Jogee, S.","last_name":"Jogee","first_name":"S."},{"full_name":"Wilkins, S.","last_name":"Wilkins","first_name":"S."}],"day":"01","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"EDP Sciences","volume":701,"file":[{"success":1,"checksum":"990e384ca19e14b35296712d3b9e2919","creator":"dernst","date_created":"2026-02-09T07:28:08Z","date_updated":"2026-02-09T07:28:08Z","file_id":"21166","content_type":"application/pdf","file_size":9994234,"access_level":"open_access","relation":"main_file","file_name":"2025_AstronomyAstrophysics_Mascia.pdf"}],"citation":{"ieee":"S. Mascia <i>et al.</i>, “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.","apa":"Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury, S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>","short":"S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury, F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L. Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco, B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino, A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy &#38; Astrophysics 701 (2025).","ama":"Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>","mla":"Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 701, A122, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>.","chicago":"Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee, S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>.","ista":"Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W, Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy &#38; Astrophysics. 701, A122."},"publication_status":"published","scopus_import":"1","DOAJ_listed":"1"},{"has_accepted_license":"1","type":"journal_article","_id":"21252","intvolume":"       700","date_published":"2025-08-01T00:00:00Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"Yes","title":"The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators","language":[{"iso":"eng"}],"file_date_updated":"2026-02-17T13:07:45Z","OA_type":"gold","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","department":[{"_id":"LiBu"}],"PlanS_conform":"1","abstract":[{"text":"Context. Recent observational results from asteroseismic studies show that an important fraction of solar-like stars do not present detectable stochastically excited acoustic oscillations. This non-detectability seems to correlate with a high rotation rate in the convective envelope and a high surface magnetic activity. At the same time, the properties of stellar convection are affected by rotation and magnetism.\r\nAims. We investigate the role of rotation in the excitation of acoustic modes in the convective envelope of solar-like stars, to evaluate its impact on the energy injected in the oscillations.\r\nMethods. We derived theoretical prescriptions for the excitation of acoustic waves in the convective envelope of rotating solar-like stars. We adopted the rotating mixing-length Theory to model the influence of rotation on convection. We used the MESA stellar evolution code and the GYRE stellar oscillation code to estimate the power injected in the oscillations from our theoretical prescriptions.\r\nResults. We demonstrate that the power injected in the acoustic modes is insensitive to rotation if a Gaussian time-correlation function is assumed, while it can decrease by up to 60% for a Lorentzian time-correlation function, for a 20 Ω⊙ rotation rate. We show that the modification of the excitation rate by rotation depends not only on the rotation rate but also on the radial and angular orders of the considered oscillation mode. This result can allow for better constraints on the properties of stellar convection by studying observationally acoustic mode excitation.\r\nConclusions. These results demonstrate how important it is to take into account the modification of stellar convection by rotation when evaluating the amplitude of the stellar oscillations it stochastically excites. They open the path for understanding the large variety of observed acoustic-mode amplitudes at the surface of solar-like stars as a function of surface rotation rates.","lang":"eng"}],"date_updated":"2026-02-17T13:10:18Z","year":"2025","publication":"Astronomy & Astrophysics","date_created":"2026-02-16T15:46:59Z","acknowledgement":"The authors thank the referee for detailed comments that allow them to improve their work. The authors thank Jordan Philidet and Kevin Belkacem for fruitful discussions. L.B. and Stéphane M. acknowledge 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 PNPS (CNRS/INSU). While partially funded by the European Union, views and opinions expressed are however those of the author only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Savita M. acknowledges support from the Spanish Ministry of Science and Innovation with the grant no. PID2019-107061GB-C66 and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S).","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_number":"A25","ddc":["520"],"status":"public","oa_version":"Published Version","article_type":"original","month":"08","quality_controlled":"1","doi":"10.1051/0004-6361/202452093","OA_place":"publisher","volume":700,"publisher":"EDP Sciences","day":"01","author":[{"last_name":"Bessila","full_name":"Bessila, L.","first_name":"L."},{"first_name":"A.","last_name":"Deckx van Ruys","full_name":"Deckx van Ruys, A."},{"full_name":"Buriasco, V.","last_name":"Buriasco","first_name":"V."},{"first_name":"S.","full_name":"Mathis, S.","last_name":"Mathis"},{"last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000"},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."}],"DOAJ_listed":"1","publication_status":"published","citation":{"ieee":"L. Bessila <i>et al.</i>, “The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators,” <i>Astronomy &#38; Astrophysics</i>, vol. 700. EDP Sciences, 2025.","ista":"Bessila L, Deckx van Ruys A, Buriasco V, Mathis S, Bugnet LA, García RA, Mathur S. 2025. The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. Astronomy &#38; Astrophysics. 700, A25.","ama":"Bessila L, Deckx van Ruys A, Buriasco V, et al. The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. <i>Astronomy &#38; Astrophysics</i>. 2025;700. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452093\">10.1051/0004-6361/202452093</a>","mla":"Bessila, L., et al. “The Impact of Rotation on the Stochastic Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” <i>Astronomy &#38; Astrophysics</i>, vol. 700, A25, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452093\">10.1051/0004-6361/202452093</a>.","chicago":"Bessila, L., A. Deckx van Ruys, V. Buriasco, S. Mathis, Lisa Annabelle Bugnet, R. A. García, and S. Mathur. “The Impact of Rotation on the Stochastic Excitation of Stellar Acoustic Modes in Solar-like Pulsators.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452093\">https://doi.org/10.1051/0004-6361/202452093</a>.","apa":"Bessila, L., Deckx van Ruys, A., Buriasco, V., Mathis, S., Bugnet, L. A., García, R. A., &#38; Mathur, S. (2025). The impact of rotation on the stochastic excitation of stellar acoustic modes in solar-like pulsators. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452093\">https://doi.org/10.1051/0004-6361/202452093</a>","short":"L. Bessila, A. Deckx van Ruys, V. Buriasco, S. Mathis, L.A. Bugnet, R.A. García, S. Mathur, Astronomy &#38; Astrophysics 700 (2025)."},"file":[{"success":1,"checksum":"b8a0927307c1d82025bcb5af47b20b26","creator":"dernst","file_id":"21306","date_updated":"2026-02-17T13:07:45Z","date_created":"2026-02-17T13:07:45Z","content_type":"application/pdf","relation":"main_file","file_size":7161755,"access_level":"open_access","file_name":"2025_AstronomyAstrophysics_Bessila.pdf"}]},{"OA_type":"diamond","file_date_updated":"2025-01-20T09:57:00Z","language":[{"iso":"eng"}],"title":"Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-01-07T00:00:00Z","intvolume":"       693","type":"journal_article","_id":"18852","has_accepted_license":"1","arxiv":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"This project was originally started as part of the Kavli Summer Program which took place in the Max Planck Institute for Astrophysics in Garching in July 2023, supported by the Kavli Foundation. We are grateful to Stephen Justham, Selma de Mink, and Jim Fuller for enriching discussions. We would like to thank the anonymous referee for their helpful report. A.B. was supported by the Deutsche Forschungsgemeinschaft (DFG) through grant GE2506/18-1. K.J.S. was supported by NASA through the Astrophysics Theory Program (80NSSC20K0544) and by NASA/ESA Hubble Space Telescope programs #15871 and #15918. W.E.K. was supported by NSF Grants OAC-2311323, AST-2206523, and NASA/ESA HST-AR-Theory HSTAR-16613.002-A. K.E. was supported in part by HST-GO-17441.001-A. AB and ASR would like to thank Rob Farmer for his support with PyMESA.","date_created":"2025-01-19T23:01:51Z","publication":"Astronomy & Astrophysics","date_updated":"2026-02-16T12:08:05Z","year":"2025","abstract":[{"text":"Recent observations have found a growing number of hypervelocity stars with speeds of ≈1500 − 2500 km s−1 that could have only been produced through thermonuclear supernovae in white dwarf binaries. Most of the observed hypervelocity runaways in this class display a surprising inflated structure: their current radii are roughly an order of magnitude greater than they would have been as white dwarfs filling their Roche lobe. While many simulations exist studying the dynamical phase leading to supernova detonation in these systems, no detailed calculations of the long-term structure of the runaways have yet been performed. We used an existing AREPO hydrodynamical simulation of a supernova in a white dwarf binary as a starting point for the evolution of these stars with the one-dimensional stellar evolution code MESA. We show that the supernova shock is not energetic enough to inflate the white dwarf over timescales longer than a few thousand years, significantly shorter than the 105 − 6 year lifetimes inferred for observed hypervelocity runaways. Although they experience a shock from a supernova less than ≈0.02 R⊙ away, our models do not experience significant interior heating, and all contract back to radii of around 0.01 R⊙ within about 104 years. Explaining the observed inflated states requires either an additional source of significant heating or some other physics that is not yet accounted for in the subsequent evolution.","lang":"eng"}],"external_id":{"isi":["001406577300001"],"arxiv":["2407.03424"]},"department":[{"_id":"IlCa"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"OA_place":"publisher","quality_controlled":"1","doi":"10.1051/0004-6361/202451371","month":"01","article_type":"original","oa_version":"Published Version","status":"public","issue":"1","ddc":["520"],"article_number":"A114","citation":{"ieee":"A. Bhat <i>et al.</i>, “Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries,” <i>Astronomy &#38; Astrophysics</i>, vol. 693, no. 1. EDP Sciences, 2025.","chicago":"Bhat, Aakash, Evan B. Bauer, Rüdiger Pakmor, Ken J. Shen, Ilaria Caiazzo, Abinaya Swaruba Rajamuthukumar, Kareem El-Badry, and Wolfgang E. Kerzendorf. “Supernova Shocks Cannot Explain the Inflated State of Hypervelocity Runaways from White Dwarf Binaries.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202451371\">https://doi.org/10.1051/0004-6361/202451371</a>.","mla":"Bhat, Aakash, et al. “Supernova Shocks Cannot Explain the Inflated State of Hypervelocity Runaways from White Dwarf Binaries.” <i>Astronomy &#38; Astrophysics</i>, vol. 693, no. 1, A114, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451371\">10.1051/0004-6361/202451371</a>.","ista":"Bhat A, Bauer EB, Pakmor R, Shen KJ, Caiazzo I, Rajamuthukumar AS, El-Badry K, Kerzendorf WE. 2025. Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. Astronomy &#38; Astrophysics. 693(1), A114.","ama":"Bhat A, Bauer EB, Pakmor R, et al. Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. <i>Astronomy &#38; Astrophysics</i>. 2025;693(1). doi:<a href=\"https://doi.org/10.1051/0004-6361/202451371\">10.1051/0004-6361/202451371</a>","apa":"Bhat, A., Bauer, E. B., Pakmor, R., Shen, K. J., Caiazzo, I., Rajamuthukumar, A. S., … Kerzendorf, W. E. (2025). Supernova shocks cannot explain the inflated state of hypervelocity runaways from white dwarf binaries. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451371\">https://doi.org/10.1051/0004-6361/202451371</a>","short":"A. Bhat, E.B. Bauer, R. Pakmor, K.J. Shen, I. Caiazzo, A.S. Rajamuthukumar, K. El-Badry, W.E. Kerzendorf, Astronomy &#38; Astrophysics 693 (2025)."},"isi":1,"file":[{"success":1,"checksum":"e532b9c8123c29cfb0ee758e6d00453c","creator":"dernst","file_id":"18861","date_updated":"2025-01-20T09:57:00Z","date_created":"2025-01-20T09:57:00Z","content_type":"application/pdf","access_level":"open_access","file_size":1692527,"relation":"main_file","file_name":"2025_AstronomyAstrophysics_Bhat.pdf"}],"publication_status":"published","scopus_import":"1","author":[{"last_name":"Bhat","full_name":"Bhat, Aakash","first_name":"Aakash"},{"last_name":"Bauer","full_name":"Bauer, Evan B.","first_name":"Evan B."},{"first_name":"Rüdiger","full_name":"Pakmor, Rüdiger","last_name":"Pakmor"},{"full_name":"Shen, Ken J.","last_name":"Shen","first_name":"Ken J."},{"orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"first_name":"Abinaya Swaruba","last_name":"Rajamuthukumar","full_name":"Rajamuthukumar, Abinaya Swaruba"},{"first_name":"Kareem","last_name":"El-Badry","full_name":"El-Badry, Kareem"},{"first_name":"Wolfgang E.","last_name":"Kerzendorf","full_name":"Kerzendorf, Wolfgang E."}],"day":"07","publisher":"EDP Sciences","volume":693},{"quality_controlled":"1","doi":"10.1051/0004-6361/202450243","OA_place":"publisher","ddc":["520"],"article_number":"A60","status":"public","oa_version":"Published Version","month":"01","article_type":"original","scopus_import":"1","publication_status":"published","citation":{"apa":"Heintz, K. E., Brammer, G. B., Watson, D., Oesch, P. A., Keating, L. C., Hayes, M. J., … Witstok, J. (2025). The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450243\">https://doi.org/10.1051/0004-6361/202450243</a>","short":"K.E. Heintz, G.B. Brammer, D. Watson, P.A. Oesch, L.C. Keating, M.J. Hayes, U. Abdurro’Uf, K.Z. Arellano-Córdova, A.C. Carnall, C.R. Christiansen, F. Cullen, R. Davé, P. Dayal, A. Ferrara, K. Finlator, J.P.U. Fynbo, S.R. Flury, V. Gelli, S. Gillman, R. Gottumukkala, K. Gould, T.R. Greve, S.E. Hardin, T.Y.Y. Hsiao, A. Hutter, P. Jakobsson, M. Killi, N. Khosravaninezhad, P. Laursen, M.M. Lee, G.E. Magdis, J.J. Matthee, R.P. Naidu, D. Narayanan, C. Pollock, M.K.M. Prescott, V. Rusakov, M. Shuntov, A. Sneppen, R. Smit, N.R. Tanvir, C. Terp, S. Toft, F. Valentino, A.P. Vijayan, J.R. Weaver, J.H. Wise, J. Witstok, Astronomy &#38; Astrophysics 693 (2025).","ama":"Heintz KE, Brammer GB, Watson D, et al. The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>. 2025;693. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450243\">10.1051/0004-6361/202450243</a>","mla":"Heintz, K. E., et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600 Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 693, A60, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450243\">10.1051/0004-6361/202450243</a>.","chicago":"Heintz, K. E., G. B. Brammer, D. Watson, P. A. Oesch, L. C. Keating, M. J. Hayes, Unknown Abdurro’Uf, et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600 Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202450243\">https://doi.org/10.1051/0004-6361/202450243</a>.","ista":"Heintz KE, Brammer GB, Watson D, Oesch PA, Keating LC, Hayes MJ, Abdurro’Uf U, Arellano-Córdova KZ, Carnall AC, Christiansen CR, Cullen F, Davé R, Dayal P, Ferrara A, Finlator K, Fynbo JPU, Flury SR, Gelli V, Gillman S, Gottumukkala R, Gould K, Greve TR, Hardin SE, Hsiao TYY, Hutter A, Jakobsson P, Killi M, Khosravaninezhad N, Laursen P, Lee MM, Magdis GE, Matthee JJ, Naidu RP, Narayanan D, Pollock C, Prescott MKM, Rusakov V, Shuntov M, Sneppen A, Smit R, Tanvir NR, Terp C, Toft S, Valentino F, Vijayan AP, Weaver JR, Wise JH, Witstok J. 2025. The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy &#38; Astrophysics. 693, A60.","ieee":"K. E. Heintz <i>et al.</i>, “The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 693. EDP Sciences, 2025."},"isi":1,"file":[{"date_updated":"2025-01-20T09:17:33Z","file_id":"18858","date_created":"2025-01-20T09:17:33Z","content_type":"application/pdf","file_size":4513466,"relation":"main_file","access_level":"open_access","file_name":"2025_AstronomyAstrophysics_Heintz.pdf","success":1,"checksum":"67a791080ade9bfb449d249de2af7456","creator":"dernst"}],"volume":693,"publisher":"EDP Sciences","day":"06","author":[{"first_name":"K. E.","full_name":"Heintz, K. E.","last_name":"Heintz"},{"full_name":"Brammer, G. B.","last_name":"Brammer","first_name":"G. B."},{"first_name":"D.","last_name":"Watson","full_name":"Watson, D."},{"first_name":"P. A.","last_name":"Oesch","full_name":"Oesch, P. A."},{"first_name":"L. C.","last_name":"Keating","full_name":"Keating, L. C."},{"first_name":"M. J.","last_name":"Hayes","full_name":"Hayes, M. J."},{"first_name":"Unknown","last_name":"Abdurro'Uf","full_name":"Abdurro'Uf, Unknown"},{"first_name":"K. Z.","full_name":"Arellano-Córdova, K. Z.","last_name":"Arellano-Córdova"},{"first_name":"A. C.","last_name":"Carnall","full_name":"Carnall, A. C."},{"first_name":"C. R.","last_name":"Christiansen","full_name":"Christiansen, C. R."},{"last_name":"Cullen","full_name":"Cullen, F.","first_name":"F."},{"first_name":"R.","full_name":"Davé, R.","last_name":"Davé"},{"last_name":"Dayal","full_name":"Dayal, P.","first_name":"P."},{"last_name":"Ferrara","full_name":"Ferrara, A.","first_name":"A."},{"first_name":"K.","full_name":"Finlator, K.","last_name":"Finlator"},{"last_name":"Fynbo","full_name":"Fynbo, J. P.U.","first_name":"J. P.U."},{"full_name":"Flury, S. R.","last_name":"Flury","first_name":"S. R."},{"first_name":"V.","full_name":"Gelli, V.","last_name":"Gelli"},{"first_name":"S.","full_name":"Gillman, S.","last_name":"Gillman"},{"full_name":"Gottumukkala, R.","last_name":"Gottumukkala","first_name":"R."},{"first_name":"K.","full_name":"Gould, K.","last_name":"Gould"},{"last_name":"Greve","full_name":"Greve, T. R.","first_name":"T. R."},{"last_name":"Hardin","full_name":"Hardin, S. E.","first_name":"S. E."},{"full_name":"Hsiao, T. Y.Y.","last_name":"Hsiao","first_name":"T. Y.Y."},{"full_name":"Hutter, A.","last_name":"Hutter","first_name":"A."},{"first_name":"P.","full_name":"Jakobsson, P.","last_name":"Jakobsson"},{"last_name":"Killi","full_name":"Killi, M.","first_name":"M."},{"last_name":"Khosravaninezhad","full_name":"Khosravaninezhad, N.","first_name":"N."},{"first_name":"P.","full_name":"Laursen, P.","last_name":"Laursen"},{"full_name":"Lee, M. M.","last_name":"Lee","first_name":"M. M."},{"first_name":"G. E.","last_name":"Magdis","full_name":"Magdis, G. E."},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"R. P.","full_name":"Naidu, R. P.","last_name":"Naidu"},{"full_name":"Narayanan, D.","last_name":"Narayanan","first_name":"D."},{"first_name":"C.","last_name":"Pollock","full_name":"Pollock, C."},{"last_name":"Prescott","full_name":"Prescott, M. K.M.","first_name":"M. K.M."},{"first_name":"V.","full_name":"Rusakov, V.","last_name":"Rusakov"},{"first_name":"M.","full_name":"Shuntov, M.","last_name":"Shuntov"},{"first_name":"A.","last_name":"Sneppen","full_name":"Sneppen, A."},{"first_name":"R.","last_name":"Smit","full_name":"Smit, R."},{"first_name":"N. R.","full_name":"Tanvir, N. R.","last_name":"Tanvir"},{"full_name":"Terp, C.","last_name":"Terp","first_name":"C."},{"first_name":"S.","last_name":"Toft","full_name":"Toft, S."},{"full_name":"Valentino, F.","last_name":"Valentino","first_name":"F."},{"first_name":"A. P.","last_name":"Vijayan","full_name":"Vijayan, A. P."},{"full_name":"Weaver, J. R.","last_name":"Weaver","first_name":"J. R."},{"last_name":"Wise","full_name":"Wise, J. H.","first_name":"J. H."},{"full_name":"Witstok, J.","last_name":"Witstok","first_name":"J."}],"date_published":"2025-01-06T00:00:00Z","article_processing_charge":"No","title":"The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"language":[{"iso":"eng"}],"file_date_updated":"2025-01-20T09:17:33Z","OA_type":"diamond","has_accepted_license":"1","_id":"18854","type":"journal_article","intvolume":"       693","external_id":{"isi":["001390856800001"]},"abstract":[{"lang":"eng","text":"Context. One of the surprising early findings with JWST has been the discovery of a strong “roll-over” or a softening of the absorption edge of Lyα in a large number of galaxies at z ≳ 6, in addition to systematic offsets from photometric redshift estimates and fundamental galaxy scaling relations. This has been interpreted as strong cumulative damped Lyα absorption (DLA) wings from high column densities of neutral atomic hydrogen (H I), signifying major gas accretion events in the formation of these galaxies.\r\nAims. To explore this new phenomenon systematically, we assembled the JWST/NIRSpec PRImordial gas Mass AssembLy (PRIMAL) legacy survey of 584 galaxies at z = 5.0 − 13.4, designed to study the physical properties and gas in and around galaxies during the reionization epoch.\r\nMethods. We characterized this benchmark sample in full and spectroscopically derived the galaxy redshifts, metallicities, star formation rates, and ultraviolet (UV) slopes. We defined a new diagnostic, the Lyα damping parameter DLyα, to measure and quantify the net effect of Lyα emission strength, the H I fraction in the intergalactic medium, or the local H I column density for each source. The JWST-PRIMAL survey is based on the spectroscopic DAWN JWST Archive (DJA-Spec). We describe DJA-Spec in this paper, detailing the reduction methods, the post-processing steps, and basic analysis tools. All the software, reduced spectra, and spectroscopically derived quantities and catalogs are made publicly available in dedicated repositories.\r\nResults. We find that the fraction of galaxies showing strong integrated DLAs with NHI > 1021 cm−2 only increases slightly from ≈60% at z ≈ 6 up to ≈65 − 90% at z > 8. Similarly, the prevalence and prominence of Lyα emission is found to increase with decreasing redshift, in qualitative agreement with previous observational results. Strong Lyα emitters (LAEs) are predominantly found to be associated with low-metallicity and UV faint galaxies. By contrast, strong DLAs are observed in galaxies with a variety of intrinsic physical properties, but predominantly at high redshifts and low metallicities.\r\nConclusions. Our results indicate that strong DLAs likely reflect a particular early assembly phase of reionization-era galaxies, at which point they are largely dominated by pristine H I gas accretion. At z = 8 − 10, this gas gradually cools and forms into stars that ionize their local surroundings, forming large ionized bubbles and producing strong observed Lyα emission at z < 8."}],"date_created":"2025-01-19T23:01:52Z","publication":"Astronomy & Astrophysics","date_updated":"2026-02-16T12:07:37Z","year":"2025","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"We would like to thank the referee for a detailed and constructive report, greatly improving the presentation of the results in this work. We would like to thank Peter Jakobsen for his vision and heroic endeavor in optimally designing the JWST/NIRSpec instrument and some of its first on-sky observations and for enlightening discussions about the intricacies of the NIRSpec data. Further, we would like to thank John Chisholm for helpful clarifications and discussions related to the escape fraction of ionizing photons and Aayush Saxena for enlightening conversations on the escape and absorption of Lyman-α photons. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. The data products presented herein were retrieved from the DAWN JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center, which is funded by the Danish National Research Foundation under grant DNRF140. P.D. acknowledge support from the NWO grant 016.VIDI.189.162 (“ODIN\") and warmly thanks the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. Support from the ERC Advanced Grant INTERSTELLAR H2020/740120 is kindly acknowledged (A.F.). S.G. acknowledges financial support from the Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. M.K. was supported by the ANID BASAL project FB210003. G.E.M. acknowledges financial support from the Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. J.W. acknowledges support from the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, by the UKRI Frontier Research grant RISEandFALL. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. F.C. acknowledges support from a UKRI Frontier Research Guarantee Grant (PI Cullen; grant reference EP/X021025/1). J.H.W. acknowledges support by NSF grant AST-2108020 and NASA grants 80NSSC20K0520 and 80NSSC21K1053. NRT acknowledges support through STFC consolidated grant ST/W000857/1. M.J.H. is supported by the Swedish Research Council, VetenskapsrÅdet, and is fellow of the Knut & Alice Wallenberg foundation. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. Software: This work made use of and acknowledge the following software: NumPy (Harris et al. 2020), Matplotlib (Hunter 2007), LMfit (Newville et al. 2014), SciPy (Virtanen et al. 2020), grizli (Brammer 2023a), Astrodrizzle (Gonzaga et al. 2012), and MsaExp (v0.3; Brammer 2023b).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"department":[{"_id":"JoMa"}]},{"isi":1,"citation":{"ista":"Scalco M, Gerasimov R, Bedin LR, Vesperini E, Correnti M, Nardiello D, Burgasser A, Richer H, Caiazzo I, Heyl J, Libralato M, Anderson J, Griggio M. 2025. JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition. Astronomy &#38; Astrophysics. 694, A68.","mla":"Scalco, M., et al. “JWST Photometry and Astrometry of 47 Tucanae. Discontinuity in the Stellar Sequence at the Star--Brown Dwarf Transition.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A68, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452907\">10.1051/0004-6361/202452907</a>.","ama":"Scalco M, Gerasimov R, Bedin LR, et al. JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452907\">10.1051/0004-6361/202452907</a>","chicago":"Scalco, M., R. Gerasimov, L. R. Bedin, E. Vesperini, M. Correnti, D. Nardiello, A. Burgasser, et al. “JWST Photometry and Astrometry of 47 Tucanae. Discontinuity in the Stellar Sequence at the Star--Brown Dwarf Transition.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452907\">https://doi.org/10.1051/0004-6361/202452907</a>.","apa":"Scalco, M., Gerasimov, R., Bedin, L. R., Vesperini, E., Correnti, M., Nardiello, D., … Griggio, M. (2025). JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452907\">https://doi.org/10.1051/0004-6361/202452907</a>","short":"M. Scalco, R. Gerasimov, L.R. Bedin, E. Vesperini, M. Correnti, D. Nardiello, A. Burgasser, H. Richer, I. Caiazzo, J. Heyl, M. Libralato, J. Anderson, M. Griggio, Astronomy &#38; Astrophysics 694 (2025).","ieee":"M. Scalco <i>et al.</i>, “JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025."},"file":[{"file_id":"19569","date_updated":"2025-04-16T07:13:31Z","date_created":"2025-04-16T07:13:31Z","content_type":"application/pdf","access_level":"open_access","relation":"main_file","file_size":18080704,"file_name":"2025_AstronomyAstrophysics_Scalco.pdf","success":1,"checksum":"db765ce222df60a1e7c19da1968906a8","creator":"dernst"}],"publication_status":"published","scopus_import":"1","author":[{"first_name":"M.","last_name":"Scalco","full_name":"Scalco, M."},{"full_name":"Gerasimov, R.","last_name":"Gerasimov","first_name":"R."},{"first_name":"L. R.","full_name":"Bedin, L. R.","last_name":"Bedin"},{"full_name":"Vesperini, E.","last_name":"Vesperini","first_name":"E."},{"last_name":"Correnti","full_name":"Correnti, M.","first_name":"M."},{"first_name":"D.","last_name":"Nardiello","full_name":"Nardiello, D."},{"full_name":"Burgasser, A.","last_name":"Burgasser","first_name":"A."},{"first_name":"H.","full_name":"Richer, H.","last_name":"Richer"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"full_name":"Heyl, J.","last_name":"Heyl","first_name":"J."},{"full_name":"Libralato, M.","last_name":"Libralato","first_name":"M."},{"first_name":"J.","last_name":"Anderson","full_name":"Anderson, J."},{"first_name":"M.","full_name":"Griggio, M.","last_name":"Griggio"}],"day":"04","publisher":"EDP Sciences","volume":694,"OA_place":"publisher","doi":"10.1051/0004-6361/202452907","quality_controlled":"1","article_type":"original","month":"02","oa_version":"Published Version","status":"public","article_number":"A68","ddc":["520"],"acknowledgement":"We dedicate this paper to the memory of our colleague Prof. Harvey Richer (⋆ April 1944 —† 13 November 2023), a highly accomplished astronomer and expert in stellar populations and in particular within globular clusters, who passed away during this project. Harvey grew up in Montreal and was at least the second star man to graduate from his high school, having been preceded by William Shatner by more than a decade. He worked at the University of British Columbia for most of his career, and his focus was the late stages of stellar evolution, in particular carbon stars and white dwarfs. We thank the referee for his valuable suggestions and comments, which helped improve the paper, as well as for his prompt revision.","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"arxiv":1,"date_updated":"2025-07-10T11:51:28Z","year":"2025","date_created":"2025-01-21T15:29:36Z","publication":"Astronomy & Astrophysics","abstract":[{"lang":"eng","text":"Using JWST Near Infrared Camera (NIRCam) images of the globular cluster 47,Tucanæ, (or NGC,104), taken at two epochs just 7 months apart, we derived proper-motion membership down to F322W2 ∼ 27. We identified an intriguing feature at the very low-mass end of the main sequence, around ∼ 0.08,M_⋅, at magnitudes F322W2 ∼ 24 and m_ F150W2 ∼ 25. This feature, dubbed 'kink', is characterized by a prominent discontinuity in the slope of the main sequence. A similar discontinuity is seen in theoretical isochrones with oxygen-poor chemistries, related to the rapid onset of absorption. We therefore hypothesize that the cluster hosts disproportionately more oxygen-poor stars near the bottom of the main sequence compared to the upper main sequence and the red giant branch. Our results show no strong or conclusive evidence of a rise in the brown dwarf luminosity function at faint magnitudes, in contrast to previous findings likely affected by faint red background galaxies. In our analysis, we accounted for this contamination by using proper motion membership."}],"external_id":{"arxiv":["2501.04446"],"isi":["001414753300007"]},"department":[{"_id":"IlCa"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"diamond","language":[{"iso":"eng"}],"file_date_updated":"2025-04-16T07:13:31Z","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_processing_charge":"Yes","title":"JWST photometry and astrometry of 47 Tucanae. Discontinuity in the stellar sequence at the star--brown dwarf transition","date_published":"2025-02-04T00:00:00Z","intvolume":"       694","_id":"18866","type":"journal_article","has_accepted_license":"1"},{"quality_controlled":"1","doi":"10.1051/0004-6361/202450426","OA_place":"publisher","status":"public","ddc":["520"],"article_number":"A100","month":"02","article_type":"original","oa_version":"Published Version","scopus_import":"1","isi":1,"file":[{"access_level":"open_access","relation":"main_file","file_size":3444203,"file_name":"2025_AstronomyAstrophysics_Vitte.pdf","date_created":"2025-02-25T07:19:34Z","date_updated":"2025-02-25T07:19:34Z","file_id":"19087","content_type":"application/pdf","creator":"dernst","success":1,"checksum":"ed2a5bba313e54ed250be348bd8c1d95"}],"citation":{"apa":"Vitte, E., Verhamme, A., Hibon, P., Leclercq, F., Alcalde Pampliega, B., Kerutt, J., … Contini, T. (2025). The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450426\">https://doi.org/10.1051/0004-6361/202450426</a>","short":"E. Vitte, A. Verhamme, P. Hibon, F. Leclercq, B. Alcalde Pampliega, J. Kerutt, H. Kusakabe, J.J. Matthee, Y. Guo, R. Bacon, M. Maseda, J. Richard, J. Pharo, J. Schaye, L. Boogaard, T. Nanayakkara, T. Contini, Astronomy &#38; Astrophysics 694 (2025).","chicago":"Vitte, Eloïse, Anne Verhamme, Pascale Hibon, Floriane Leclercq, Belén Alcalde Pampliega, Josephine Kerutt, Haruka Kusakabe, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202450426\">https://doi.org/10.1051/0004-6361/202450426</a>.","ista":"Vitte E, Verhamme A, Hibon P, Leclercq F, Alcalde Pampliega B, Kerutt J, Kusakabe H, Matthee JJ, Guo Y, Bacon R, Maseda M, Richard J, Pharo J, Schaye J, Boogaard L, Nanayakkara T, Contini T. 2025. The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. Astronomy &#38; Astrophysics. 694, A100.","ama":"Vitte E, Verhamme A, Hibon P, et al. The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450426\">10.1051/0004-6361/202450426</a>","mla":"Vitte, Eloïse, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A100, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450426\">10.1051/0004-6361/202450426</a>.","ieee":"E. Vitte <i>et al.</i>, “The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025."},"publication_status":"published","publisher":"EDP Sciences","volume":694,"author":[{"last_name":"Vitte","full_name":"Vitte, Eloïse","first_name":"Eloïse"},{"last_name":"Verhamme","full_name":"Verhamme, Anne","first_name":"Anne"},{"last_name":"Hibon","full_name":"Hibon, Pascale","first_name":"Pascale"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"first_name":"Belén","last_name":"Alcalde Pampliega","full_name":"Alcalde Pampliega, Belén"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Guo","full_name":"Guo, Yucheng","first_name":"Yucheng"},{"last_name":"Bacon","full_name":"Bacon, Roland","first_name":"Roland"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"last_name":"Pharo","full_name":"Pharo, John","first_name":"John"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Thierry","last_name":"Contini","full_name":"Contini, Thierry"}],"day":"01","title":"The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies","article_processing_charge":"No","tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-02-01T00:00:00Z","OA_type":"hybrid","language":[{"iso":"eng"}],"file_date_updated":"2025-02-25T07:19:34Z","type":"journal_article","_id":"19069","has_accepted_license":"1","intvolume":"       694","abstract":[{"text":"Context. The hydrogen Lyman-alpha (Lyα) line, the brightest rest-frame ultraviolet line of high-redshift galaxies, exhibits a large variety of shapes, which is due to factors at different scales, from the interstellar medium to the intergalactic medium (IGM).\r\nAims. The aim of this work is to provide a systematic inventory and classification of the spectral shapes of Lyα emission lines to better understand the general population of high-redshift Lyα emitting galaxies (LAEs).\r\nMethods. Using the unprecedentedly deep data from the MUSE eXtremely Deep Field (MXDF; up to 140 hour exposure time), we selected 477 galaxies observed in the ∼2.8−6.6 redshift range, 15 of which have a systemic redshift from nebular lines. We developed a method to classify Lyα emission lines in four spectral and three spatial categories by combining a pure spectral analysis with a narrow-band image analysis. We measured spectral properties, such as the peak separation and the blue-to-total flux ratio for the double-peaked galaxies.\r\nResults. To ensure a robust sample for statistical analysis, we define two unbiased subsets, inclusive and restrictive, by applying thresholds for signal-to-noise ratio, peak separation, and Lyα luminosity, yielding a final unbiased sample of 206 galaxies. Our analysis reveals that between 32% and 51% of the galaxies exhibit double-peaked profiles, with peak separations ranging from 150 km s−1 to nearly 1600 km s−1. The fraction of double-peaked galaxies seems to evolve dependently with the Lyα luminosity, while we do not see a severe decrease in this fraction with redshift, which is expected given the IGM attenuation at high redshift. An artificial increase in the number of double-peaked galaxies at the highest redshifts may cause the observation of a plateau instead of a decrease. A notable number of these double-peaked profiles show blue-dominated spectra, suggesting unique gas dynamics and inflow characteristics in some high-redshift galaxies. The consequent fraction of blue-dominated spectra needs to be confirmed by obtaining new systemic redshift measurements. Among the double-peaked galaxies, 4% are spurious detections, that is, the blue and red peaks do not come from the same spatial location. Around 20% out of the 477 sources of the parent sample lie in a complex environment, meaning there are other clumps or galaxies at the same redshift within a distance of 30 kpc.\r\nConclusions. Our results suggest that the double-peaked LAE fraction may trace the evolution of IGM attenuation, but the faintest galaxies must be observed at high redshift. We also need more data to confirm the trend seen at low redshift. In addition, it is crucial to obtain secure systemic redshifts for LAEs to better constrain the nature of the Lyα double-peaked lines. Statistical samples of double-peaked and triple-peaked galaxies are a promising probe of the evolution of the physical properties of galaxies across cosmic time.","lang":"eng"}],"external_id":{"isi":["001417357000009"]},"publication_identifier":{"issnl":["0004-6361"],"eissn":["1432-0746"],"issn":["0004-6361"]},"acknowledgement":"EV and AV acknowledges the support from the SNF grants PP00P2 176808 and 211023. HK acknowledges support from Japan Society for the Promotion of Science (JSPS) Overseas Research Fellowship as well as JSPS Research Fellowships for Young Scientists. JP acknowledges funding by the Deutsche Forschungsgemeinschaft, Grant Wi 1369/31-1. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of ASTROPY, which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018, 2022), and other software and packages: MPDAF (Piqueras et al. 2019), PHOTUTILS (Bradley 2023), NUMPY (van der Walt et al. 2011), SCIPY (Virtanen et al. 2020). The plots in this paper were created using MATPLOTLIB (Hunter 2007).","date_created":"2025-02-23T23:01:56Z","publication":"Astronomy & Astrophysics","year":"2025","date_updated":"2026-02-16T12:08:40Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"department":[{"_id":"JoMa"}]}]