[{"OA_type":"diamond","quality_controlled":"1","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"oa":1,"_id":"21045","OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"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_status":"published","volume":705,"type":"journal_article","arxiv":1,"month":"01","author":[{"last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","orcid":"0000-0001-5586-6950","first_name":"Alberto"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"first_name":"Tanya","full_name":"Urrutia, Tanya","last_name":"Urrutia"},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","full_name":"Mascia, Sara"},{"full_name":"D’Eugenio, Francesco","first_name":"Francesco","last_name":"D’Eugenio"},{"full_name":"Di Cesare, Claudia","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo"},{"last_name":"Ishikawa","full_name":"Ishikawa, Yuzo","first_name":"Yuzo"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Benjamín","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete"},{"first_name":"Gauri","full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale"}],"doi":"10.1051/0004-6361/202555596","file":[{"file_size":2259914,"file_name":"2026_AstronomyAstrophysics_Torralba.pdf","success":1,"content_type":"application/pdf","file_id":"21224","creator":"dernst","checksum":"3782e03bc0843438aae8487f6af779c5","access_level":"open_access","date_created":"2026-02-16T07:35:03Z","date_updated":"2026-02-16T07:35:03Z","relation":"main_file"}],"article_number":"A147","external_id":{"arxiv":["2505.09542"]},"status":"public","year":"2026","corr_author":"1","publisher":"EDP Sciences","citation":{"apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke, M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy and Astrophysics</i>. EDP Sciences. <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.","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.","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>","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>.","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).","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>."},"PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","file_date_updated":"2026-02-16T07:35:03Z","date_updated":"2026-02-16T07:46:53Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","scopus_import":"1","article_processing_charge":"No","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","intvolume":"       705","language":[{"iso":"eng"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication":"Astronomy and Astrophysics","day":"14","date_published":"2026-01-14T00:00:00Z","ddc":["520"],"abstract":[{"lang":"eng","text":"The abundant population of little red dots (LRDs), compact objects with red UV to optical colors and broad Balmer lines at high redshift, is revealing new insights into the properties of early active galactic nuclei (AGN). Perhaps the most surprising features of this population are the presence of Balmer absorption and ubiquitous strong Balmer breaks. Recent models link these features to an active supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We present a stringent test of such models using VLT/MUSE observations of A2744-45924, the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744 lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula (h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc. The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα) compared to Lyα nebulae typically observed around quasars of similar luminosity. We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered by star formation. In the environment of A2744-45924, we identified four extended Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations based on Hα emission, and show no evidence for radiation from A2744-45924 affecting its surroundings. The lack of strong, compact, and broad Lyα and the absence of a luminous extended halo, suggest that the UV AGN light is obscured by dense gas cloaking the SMBH with a covering factor close to unity."}],"date_created":"2026-01-25T23:01:41Z"},{"PlanS_conform":"1","citation":{"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>","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.","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.","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>","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>.","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).","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>."},"publisher":"EDP Sciences","year":"2026","external_id":{"arxiv":["2512.04147"]},"status":"public","article_processing_charge":"No","article_type":"original","scopus_import":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_updated":"2026-02-16T09:36:24Z","file_date_updated":"2026-02-16T09:33:56Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","language":[{"iso":"eng"}],"intvolume":"       706","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","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."}],"ddc":["520"],"date_published":"2026-02-01T00:00:00Z","day":"01","publication":"Astronomy and Astrophysics","department":[{"_id":"IlCa"}],"quality_controlled":"1","OA_type":"diamond","OA_place":"publisher","oa":1,"_id":"21160","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","file":[{"file_size":4020466,"content_type":"application/pdf","success":1,"file_name":"2026_AstronomyAstrophysics_Yu.pdf","file_id":"21227","creator":"dernst","checksum":"2faec710fd04f927aa43deb57e35c9b2","access_level":"open_access","date_created":"2026-02-16T09:33:56Z","date_updated":"2026-02-16T09:33:56Z","relation":"main_file"}],"article_number":"A14","doi":"10.1051/0004-6361/202557568","author":[{"last_name":"Yu","full_name":"Yu, W.","first_name":"W."},{"last_name":"Pala","full_name":"Pala, A. F.","first_name":"A. F."},{"last_name":"Kupfer","full_name":"Kupfer, T.","first_name":"T."},{"last_name":"Gänsicke","first_name":"B. T.","full_name":"Gänsicke, B. T."},{"last_name":"Koester","first_name":"D.","full_name":"Koester, D."},{"first_name":"D.","full_name":"Belloni, D.","last_name":"Belloni"},{"last_name":"Wong","first_name":"T. L.S.","full_name":"Wong, T. L.S."},{"first_name":"M. R.","full_name":"Schreiber, M. R.","last_name":"Schreiber"},{"full_name":"van Roestel, Joannes C","first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","last_name":"van Roestel"},{"last_name":"Brown","first_name":"A. J.","full_name":"Brown, A. J."},{"last_name":"Waagen","full_name":"Waagen, E. O.","first_name":"E. O."},{"last_name":"González-Carballo","first_name":"J. L.","full_name":"González-Carballo, J. L."},{"last_name":"Bednarz","full_name":"Bednarz, S.","first_name":"S."},{"full_name":"Bernacki, K.","first_name":"K.","last_name":"Bernacki"},{"last_name":"De Martino","full_name":"De Martino, D.","first_name":"D."},{"full_name":"Fernández Mañanes, E.","first_name":"E.","last_name":"Fernández Mañanes"},{"last_name":"González Farfán","full_name":"González Farfán, R.","first_name":"R."},{"last_name":"Green","first_name":"M. J.","full_name":"Green, M. J."},{"last_name":"Groot","full_name":"Groot, P. J.","first_name":"P. J."},{"first_name":"F. J.","full_name":"Hambsch, F. J.","last_name":"Hambsch"},{"last_name":"Knigge","full_name":"Knigge, C.","first_name":"C."},{"first_name":"J. L.","full_name":"Martin-Velasco, J. L.","last_name":"Martin-Velasco"},{"first_name":"M.","full_name":"Morales-Aimar, M.","last_name":"Morales-Aimar"},{"last_name":"Myers","first_name":"G.","full_name":"Myers, G."},{"first_name":"R.","full_name":"Naves Nogues, R.","last_name":"Naves Nogues"},{"first_name":"R.","full_name":"Poggiani, R.","last_name":"Poggiani"},{"full_name":"Popowicz, A.","first_name":"A.","last_name":"Popowicz"},{"first_name":"G.","full_name":"Ramsay, G.","last_name":"Ramsay"},{"full_name":"Reina-Lorenz, E.","first_name":"E.","last_name":"Reina-Lorenz"},{"first_name":"P.","full_name":"Rodríguez-Gil, P.","last_name":"Rodríguez-Gil"},{"last_name":"Salto-González","full_name":"Salto-González, J. L.","first_name":"J. L."},{"full_name":"Sion, E. M.","first_name":"E. M.","last_name":"Sion"},{"last_name":"Steeghs","full_name":"Steeghs, D.","first_name":"D."},{"first_name":"P.","full_name":"Szkody, P.","last_name":"Szkody"},{"last_name":"Toloza","first_name":"O.","full_name":"Toloza, O."},{"full_name":"Tovmassian, G.","first_name":"G.","last_name":"Tovmassian"}],"month":"02","arxiv":1,"type":"journal_article","volume":706,"publication_status":"published","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":{"issn":["0004-6361"],"eissn":["1432-0746"]},"file_date_updated":"2026-02-24T07:46:47Z","date_updated":"2026-02-24T07:49:42Z","article_processing_charge":"No","article_type":"original","scopus_import":"1","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","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>","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.","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.","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>","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>.","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).","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>."},"PlanS_conform":"1","status":"public","external_id":{"arxiv":["2510.19959"]},"corr_author":"1","year":"2026","ddc":["520"],"date_published":"2026-02-01T00:00:00Z","date_created":"2026-02-22T23:01:35Z","abstract":[{"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.","lang":"eng"}],"day":"01","publication":"Astronomy & Astrophysics","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"language":[{"iso":"eng"}],"intvolume":"       706","title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","OA_place":"publisher","oa":1,"_id":"21341","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"OA_type":"diamond","quality_controlled":"1","author":[{"last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","full_name":"Kotiwale, Gauri"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Kashino","first_name":"Daichi","full_name":"Kashino, Daichi"},{"last_name":"Vijayan","full_name":"Vijayan, Aswin P.","first_name":"Aswin P."},{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","first_name":"Alberto","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto"},{"last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","full_name":"Di Cesare, Claudia"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo"},{"full_name":"Bordoloi, Rongmon","first_name":"Rongmon","last_name":"Bordoloi"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"full_name":"Danhaive, A. Lola","first_name":"A. Lola","last_name":"Danhaive"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara"},{"first_name":"Ivan","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko"},{"full_name":"Navarrete, Benjamín","first_name":"Benjamín","last_name":"Navarrete","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"}],"article_number":"A165","file":[{"access_level":"open_access","creator":"dernst","checksum":"6f5849d29ad43bee32f90152f6fc0294","file_id":"21355","file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","success":1,"content_type":"application/pdf","file_size":6531719,"relation":"main_file","date_updated":"2026-02-24T07:46:47Z","date_created":"2026-02-24T07:46:47Z"}],"doi":"10.1051/0004-6361/202556597","publication_status":"published","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).","DOAJ_listed":"1","month":"02","arxiv":1,"type":"journal_article","volume":706,"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version"},{"oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","arxiv":1,"volume":706,"DOAJ_listed":"1","month":"02","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).","publication_status":"published","doi":"10.1051/0004-6361/202557358","article_number":"A261","file":[{"date_created":"2026-03-02T14:51:57Z","date_updated":"2026-03-02T14:51:57Z","relation":"main_file","file_id":"21391","creator":"dernst","checksum":"cd25a05386ab5638ae5baf8add0ecbee","access_level":"open_access","file_size":1813456,"content_type":"application/pdf","success":1,"file_name":"2026_AstronomyAstrophysics_GimenezAlcazar.pdf"}],"author":[{"last_name":"Giménez-Alcázar","full_name":"Giménez-Alcázar, A.","first_name":"A."},{"first_name":"R.","full_name":"Amorín, R.","last_name":"Amorín"},{"full_name":"Vílchez, J. M.","first_name":"J. M.","last_name":"Vílchez"},{"first_name":"A.","full_name":"Hernán-Caballero, A.","last_name":"Hernán-Caballero"},{"last_name":"González-Otero","full_name":"González-Otero, M.","first_name":"M."},{"first_name":"A.","full_name":"Arroyo-Polonio, A.","last_name":"Arroyo-Polonio"},{"first_name":"J.","full_name":"Iglesias-Páramo, J.","last_name":"Iglesias-Páramo"},{"first_name":"A.","full_name":"Lumbreras-Calle, A.","last_name":"Lumbreras-Calle"},{"full_name":"Fernández-Ontiveros, J. A.","first_name":"J. A.","last_name":"Fernández-Ontiveros"},{"last_name":"López-Sanjuan","first_name":"C.","full_name":"López-Sanjuan, C."},{"first_name":"L.","full_name":"Bonatto, L.","last_name":"Bonatto"},{"first_name":"R. M.","full_name":"González Delgado, R. M.","last_name":"González Delgado"},{"first_name":"C.","full_name":"Kehrig, C.","last_name":"Kehrig"},{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa","first_name":"Alberto","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto"},{"last_name":"Rahna","first_name":"P. T.","full_name":"Rahna, P. T."},{"last_name":"Jiménez-Teja","full_name":"Jiménez-Teja, Y.","first_name":"Y."},{"full_name":"Márquez, I.","first_name":"I.","last_name":"Márquez"},{"first_name":"I.","full_name":"Breda, I.","last_name":"Breda"},{"last_name":"Álvarez-Candal","full_name":"Álvarez-Candal, A.","first_name":"A."},{"full_name":"Abramo, R.","first_name":"R.","last_name":"Abramo"},{"last_name":"Alcaniz","first_name":"J.","full_name":"Alcaniz, J."},{"first_name":"N.","full_name":"Benitez, N.","last_name":"Benitez"},{"first_name":"S.","full_name":"Bonoli, S.","last_name":"Bonoli"},{"first_name":"S.","full_name":"Carneiro, S.","last_name":"Carneiro"},{"full_name":"Cenarro, J.","first_name":"J.","last_name":"Cenarro"},{"first_name":"D.","full_name":"Cristóbal-Hornillos, D.","last_name":"Cristóbal-Hornillos"},{"last_name":"Dupke","full_name":"Dupke, R.","first_name":"R."},{"last_name":"Ederoclite","first_name":"A.","full_name":"Ederoclite, A."},{"last_name":"Hernández-Monteagudo","first_name":"C.","full_name":"Hernández-Monteagudo, C."},{"last_name":"Marín-Franch","first_name":"A.","full_name":"Marín-Franch, A."},{"first_name":"C.","full_name":"Mendes de Oliveira, C.","last_name":"Mendes de Oliveira"},{"last_name":"Moles","first_name":"M.","full_name":"Moles, M."},{"first_name":"L.","full_name":"Sodré, L.","last_name":"Sodré"},{"full_name":"Taylor, K.","first_name":"K.","last_name":"Taylor"},{"last_name":"Varela","full_name":"Varela, J.","first_name":"J."},{"first_name":"H.","full_name":"Vázquez Ramió, H.","last_name":"Vázquez Ramió"}],"quality_controlled":"1","OA_type":"diamond","_id":"21380","oa":1,"OA_place":"publisher","title":"J-PAS: First identification, physical properties, and ionization efficiency of extreme emission line galaxies","intvolume":"       706","language":[{"iso":"eng"}],"department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","day":"01","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_created":"2026-03-02T10:06:10Z","date_published":"2026-02-01T00:00:00Z","ddc":["520"],"year":"2026","external_id":{"arxiv":["2512.08484"]},"status":"public","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>","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.","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.","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>","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>.","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>.","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)."},"publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","article_type":"original","scopus_import":"1","article_processing_charge":"No","date_updated":"2026-03-02T15:10:27Z","file_date_updated":"2026-03-02T14:51:57Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"file_date_updated":"2026-03-16T10:57:49Z","date_updated":"2026-03-16T10:59:16Z","article_processing_charge":"No","scopus_import":"1","article_type":"original","external_id":{"arxiv":["2510.00103"]},"status":"public","year":"2026","corr_author":"1","publisher":"EDP Sciences","PlanS_conform":"1","citation":{"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>","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.","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.","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>.","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).","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>."},"day":"01","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","ddc":["520"],"date_published":"2026-03-01T00:00:00Z","date_created":"2026-03-15T23:01:36Z","abstract":[{"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.","lang":"eng"}],"title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","intvolume":"       707","language":[{"iso":"eng"}],"_id":"21451","oa":1,"OA_place":"publisher","OA_type":"diamond","quality_controlled":"1","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"publication_status":"published","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.","DOAJ_listed":"1","month":"03","type":"journal_article","arxiv":1,"volume":707,"author":[{"full_name":"Torralba Torregrosa, Alberto","orcid":"0000-0001-5586-6950","first_name":"Alberto","last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Yuzo","full_name":"Ishikawa, Yuzo","last_name":"Ishikawa"},{"full_name":"Brammer, Gabriel B.","first_name":"Gabriel B.","last_name":"Brammer"},{"last_name":"Chang","full_name":"Chang, Seok Jun","first_name":"Seok Jun"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"last_name":"De Graaff","full_name":"De Graaff, Anna","first_name":"Anna"},{"last_name":"D’Eugenio","first_name":"Francesco","full_name":"D’Eugenio, Francesco"},{"full_name":"Di Cesare, Claudia","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare"},{"last_name":"Eilers","first_name":"Anna Christina","full_name":"Eilers, Anna Christina"},{"last_name":"Greene","first_name":"Jenny E.","full_name":"Greene, Jenny E."},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","first_name":"Edoardo"},{"last_name":"Kokorev","first_name":"Vasily","full_name":"Kokorev, Vasily"},{"id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale","first_name":"Gauri","full_name":"Kotiwale, Gauri"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","first_name":"Ivan"},{"last_name":"Ma","full_name":"Ma, Yilun","first_name":"Yilun"},{"last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","full_name":"Mascia, Sara"},{"full_name":"Navarrete, Benjamín","first_name":"Benjamín","last_name":"Navarrete","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"last_name":"Nelson","first_name":"Erica","full_name":"Nelson, Erica"},{"first_name":"Pascal","full_name":"Oesch, Pascal","last_name":"Oesch"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"full_name":"Wuyts, Stijn","first_name":"Stijn","last_name":"Wuyts"}],"file":[{"date_created":"2026-03-16T10:57:49Z","relation":"main_file","date_updated":"2026-03-16T10:57:49Z","file_size":2510157,"success":1,"content_type":"application/pdf","file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","file_id":"21460","creator":"dernst","checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","access_level":"open_access"}],"article_number":"A75","doi":"10.1051/0004-6361/202557537","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"}},{"corr_author":"1","year":"2026","status":"public","external_id":{"arxiv":["2510.19044"]},"PlanS_conform":"1","citation":{"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>.","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>.","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).","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>","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.","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.","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>"},"publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","article_processing_charge":"No","article_type":"original","scopus_import":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"file_date_updated":"2026-03-16T10:48:07Z","date_updated":"2026-03-16T10:52:44Z","title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","intvolume":"       707","language":[{"iso":"eng"}],"day":"01","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication":"Astronomy & Astrophysics","date_created":"2026-03-15T23:01:36Z","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"}],"ddc":["520"],"date_published":"2026-03-01T00:00:00Z","quality_controlled":"1","OA_type":"diamond","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"_id":"21452","oa":1,"OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"DOAJ_listed":"1","month":"03","type":"journal_article","arxiv":1,"volume":707,"publication_status":"published","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).","file":[{"date_updated":"2026-03-16T10:48:07Z","relation":"main_file","date_created":"2026-03-16T10:48:07Z","success":1,"file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","content_type":"application/pdf","file_size":1821411,"access_level":"open_access","file_id":"21459","checksum":"c056b00ce7324849754521fde10fb7ca","creator":"dernst"}],"article_number":"A129","doi":"10.1051/0004-6361/202557790","author":[{"first_name":"Claudia","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Torralba, Alberto","first_name":"Alberto","last_name":"Torralba"},{"last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","first_name":"Gauri"},{"last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","first_name":"Ivan"},{"last_name":"Blaizot","full_name":"Blaizot, Jeremy","first_name":"Jeremy"},{"last_name":"Rosdahl","full_name":"Rosdahl, Joakim","first_name":"Joakim"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"first_name":"Edoardo","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"first_name":"Alba","full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz"},{"full_name":"Furtak, Lukas J.","first_name":"Lukas J.","last_name":"Furtak"},{"first_name":"Kasper E.","full_name":"Heintz, Kasper E.","last_name":"Heintz"},{"first_name":"Sara","full_name":"Mascia, Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete","full_name":"Navarrete, Benjamín","first_name":"Benjamín"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"last_name":"Romano","first_name":"Michael","full_name":"Romano, Michael"},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"}]},{"publication":"Astronomy & Astrophysics","department":[{"_id":"YlGo"}],"day":"01","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."}],"date_created":"2026-03-15T23:01:35Z","date_published":"2026-03-01T00:00:00Z","ddc":["520"],"title":"A constant upper luminosity limit of cool supergiant stars down to the extremely low metallicity of I Zw 18","intvolume":"       707","language":[{"iso":"eng"}],"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_type":"original","scopus_import":"1","article_processing_charge":"No","date_updated":"2026-03-16T09:07:55Z","file_date_updated":"2026-03-16T09:05:06Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"year":"2026","external_id":{"arxiv":["2510.12594"]},"status":"public","citation":{"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.","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>","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>","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.","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>.","short":"A. Schootemeijer, Y.L.L. Götberg, N. Langer, G. Bortolini, A.S. Hirschauer, L. Patrick, Astronomy &#38; Astrophysics 707 (2026).","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>."},"PlanS_conform":"1","publisher":"EDP Sciences","arxiv":1,"type":"journal_article","volume":707,"month":"03","DOAJ_listed":"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_status":"published","doi":"10.1051/0004-6361/202557675","file":[{"access_level":"open_access","creator":"dernst","checksum":"02a0cd932340207c96fdd3059490ad29","file_id":"21455","content_type":"application/pdf","success":1,"file_name":"2026_AstronomyAstrophysics_Schootemeijer.pdf","file_size":2102107,"relation":"main_file","date_updated":"2026-03-16T09:05:06Z","date_created":"2026-03-16T09:05:06Z"}],"article_number":"A116","author":[{"first_name":"Abel","full_name":"Schootemeijer, Abel","last_name":"Schootemeijer"},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Langer, Norbert","first_name":"Norbert","last_name":"Langer"},{"last_name":"Bortolini","full_name":"Bortolini, Giacomo","first_name":"Giacomo"},{"last_name":"Hirschauer","first_name":"Alec S.","full_name":"Hirschauer, Alec S."},{"last_name":"Patrick","first_name":"Lee","full_name":"Patrick, Lee"}],"oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa":1,"_id":"21450","OA_place":"publisher","quality_controlled":"1","OA_type":"diamond"},{"status":"public","external_id":{"arxiv":["2509.05403"]},"corr_author":"1","year":"2026","publisher":"EDP Sciences","PlanS_conform":"1","citation":{"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>","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.","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>","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>.","short":"I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy &#38; Astrophysics 707 (2026).","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>."},"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2026-03-23T15:46:31Z","file_date_updated":"2026-03-23T15:44:09Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","article_processing_charge":"No","intvolume":"       707","title":"H α as a tracer of star formation in the SPHINX cosmological simulations","language":[{"iso":"eng"}],"department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","day":"05","date_published":"2026-03-05T00:00:00Z","ddc":["520"],"abstract":[{"lang":"eng","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."}],"date_created":"2026-03-23T14:58:03Z","OA_type":"diamond","quality_controlled":"1","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"_id":"21481","oa":1,"OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"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).","publication_status":"published","volume":707,"arxiv":1,"type":"journal_article","month":"03","DOAJ_listed":"1","author":[{"full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","first_name":"Ivan","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"first_name":"J.","full_name":"Rosdahl, J.","last_name":"Rosdahl"},{"first_name":"J.","full_name":"Blaizot, J.","last_name":"Blaizot"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Katz","full_name":"Katz, H.","first_name":"H."},{"first_name":"Claudia","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare"}],"doi":"10.1051/0004-6361/202557114","article_number":"A184","file":[{"file_id":"21492","creator":"dernst","checksum":"7429076b381dd498084f40ffd199e714","access_level":"open_access","file_size":904565,"file_name":"2026_AstronomyAstrophysics_Kramarenko.pdf","success":1,"content_type":"application/pdf","date_created":"2026-03-23T15:44:09Z","date_updated":"2026-03-23T15:44:09Z","relation":"main_file"}]},{"quality_controlled":"1","OA_type":"diamond","OA_place":"publisher","_id":"21658","oa":1,"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","doi":"10.1051/0004-6361/202558023","file":[{"access_level":"open_access","checksum":"560cac19dc70184626b85e71a26ee22e","creator":"dernst","file_id":"21664","file_name":"2026_AstronomyAstrophysics_Liagre.pdf","success":1,"content_type":"application/pdf","file_size":12287607,"relation":"main_file","date_updated":"2026-04-07T09:00:50Z","date_created":"2026-04-07T09:00:50Z"}],"article_number":"A321","author":[{"id":"662f1873-cab4-11f0-a719-8087d302868d","last_name":"Liagre","first_name":"Bastien Raymond Bernard","full_name":"Liagre, Bastien Raymond Bernard"},{"id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","last_name":"Desai","full_name":"Desai, Aayush A","first_name":"Aayush A"},{"id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","last_name":"Einramhof","first_name":"Lukas","full_name":"Einramhof, Lukas"},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"}],"type":"journal_article","volume":707,"arxiv":1,"month":"03","DOAJ_listed":"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).","publication_status":"published","PlanS_conform":"1","citation":{"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>","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.","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.","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>","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>.","short":"B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy and Astrophysics 707 (2026).","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>."},"publisher":"EDP Sciences","corr_author":"1","year":"2026","external_id":{"arxiv":["2511.05314 "]},"status":"public","article_type":"original","scopus_import":"1","article_processing_charge":"No","date_updated":"2026-04-07T09:01:44Z","file_date_updated":"2026-04-07T09:00:50Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","intvolume":"       707","abstract":[{"text":"Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.","lang":"eng"}],"date_created":"2026-04-05T22:01:32Z","date_published":"2026-03-01T00:00:00Z","ddc":["520"],"publication":"Astronomy and Astrophysics","department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"day":"01"},{"OA_type":"diamond","quality_controlled":"1","project":[{"_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631","name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology"}],"oa":1,"_id":"21659","OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"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.","publication_status":"published","type":"journal_article","arxiv":1,"volume":707,"month":"03","DOAJ_listed":"1","author":[{"first_name":"S. N.","full_name":"Breton, S. N.","last_name":"Breton"},{"last_name":"Pezzotti","full_name":"Pezzotti, C.","first_name":"C."},{"first_name":"S.","full_name":"Mathis, S.","last_name":"Mathis"},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Di Mauro","first_name":"M. P.","full_name":"Di Mauro, 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"}],"doi":"10.1051/0004-6361/202659309","file":[{"access_level":"open_access","checksum":"a7fd798bf450d67d4166fdf54ff2c70c","creator":"dernst","file_id":"21666","file_name":"2026_AstronomyAstrophysics_Breton.pdf","success":1,"content_type":"application/pdf","file_size":1535506,"date_updated":"2026-04-07T09:20:02Z","relation":"main_file","date_created":"2026-04-07T09:20:02Z"}],"article_number":"L16","status":"public","external_id":{"arxiv":["2603.01979"]},"year":"2026","publisher":"Wiley","citation":{"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>.","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>","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.","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>","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."},"PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","file_date_updated":"2026-04-07T09:20:02Z","date_updated":"2026-04-07T09:23:27Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"scopus_import":"1","article_type":"letter_editor","article_processing_charge":"No","title":"Core-envelope coupling of gravito-inertial waves in pre-main-sequence solar-type stars","intvolume":"       707","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","department":[{"_id":"LiBu"}],"day":"01","date_published":"2026-03-01T00:00:00Z","ddc":["520"],"abstract":[{"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.","lang":"eng"}],"date_created":"2026-04-05T22:01:32Z"},{"oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"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_status":"published","type":"journal_article","volume":706,"month":"02","DOAJ_listed":"1","author":[{"first_name":"Andrei-Alexandru","full_name":"Cristea, Andrei-Alexandru","last_name":"Cristea","id":"4d500bea-31f8-11ee-a48d-d4904fb363c7"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","last_name":"Caiazzo","first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria"},{"last_name":"Cunningham","full_name":"Cunningham, Tim","first_name":"Tim"},{"last_name":"Raymond","full_name":"Raymond, John C.","first_name":"John C."},{"first_name":"Stephane","full_name":"Vennes, Stephane","last_name":"Vennes"},{"last_name":"Kawka","full_name":"Kawka, Adela","first_name":"Adela"},{"last_name":"Desai","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","first_name":"Aayush A","full_name":"Desai, Aayush A"},{"full_name":"Miller, David R.","first_name":"David R.","last_name":"Miller"},{"full_name":"Hermes, J. J.","first_name":"J. J.","last_name":"Hermes"},{"full_name":"Fuller, Jim","first_name":"Jim","last_name":"Fuller"},{"last_name":"Heyl","full_name":"Heyl, Jeremy","first_name":"Jeremy"},{"last_name":"van Roestel","full_name":"van Roestel, Jan","first_name":"Jan"},{"first_name":"Kevin B.","full_name":"Burdge, Kevin B.","last_name":"Burdge"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"last_name":"Pelisoli","full_name":"Pelisoli, Ingrid","first_name":"Ingrid"},{"first_name":"Boris T.","full_name":"Gänsicke, Boris T.","last_name":"Gänsicke"},{"full_name":"Szkody, Paula","first_name":"Paula","last_name":"Szkody"},{"full_name":"Kenyon, Scott J.","first_name":"Scott J.","last_name":"Kenyon"},{"first_name":"Zach","full_name":"Vanderbosch, Zach","last_name":"Vanderbosch"},{"full_name":"Drake, Andrew","first_name":"Andrew","last_name":"Drake"},{"last_name":"Ferrario","full_name":"Ferrario, Lilia","first_name":"Lilia"},{"first_name":"Dayal","full_name":"Wickramasinghe, Dayal","last_name":"Wickramasinghe"},{"last_name":"Karambelkar","full_name":"Karambelkar, Viraj R.","first_name":"Viraj R."},{"last_name":"Justham","full_name":"Justham, Stephen","first_name":"Stephen"},{"last_name":"Pakmor","full_name":"Pakmor, Ruediger","first_name":"Ruediger"},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"last_name":"Prince","full_name":"Prince, Thomas","first_name":"Thomas"},{"last_name":"Kulkarni","full_name":"Kulkarni, S. R.","first_name":"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."},{"last_name":"Groom","full_name":"Groom, Steven L.","first_name":"Steven L."},{"last_name":"Purdum","full_name":"Purdum, Josiah","first_name":"Josiah"},{"last_name":"Dekany","full_name":"Dekany, Richard","first_name":"Richard"},{"last_name":"Bellm","first_name":"Eric C.","full_name":"Bellm, Eric C."}],"doi":"10.1051/0004-6361/202556432","article_number":"A188","file":[{"file_size":5352853,"content_type":"application/pdf","success":1,"file_name":"2026_AstronomyAstrophysics_Cristea.pdf","file_id":"21350","creator":"dernst","checksum":"229b688e6e78cab5bb8e2bac366d1575","access_level":"open_access","date_created":"2026-02-23T12:04:37Z","date_updated":"2026-02-23T12:04:37Z","relation":"main_file"}],"OA_type":"gold","quality_controlled":"1","_id":"21274","oa":1,"OA_place":"publisher","related_material":{"link":[{"description":"News on ISTA website","relation":"press_release","url":"https://ista.ac.at/en/news/twos-company-new-class-of-star-remnants/"}]},"intvolume":"       706","title":"A half ring of ionized circumstellar material trapped in the magnetosphere of a white dwarf merger remnant","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","department":[{"_id":"IlCa"},{"_id":"GradSch"}],"day":"10","date_published":"2026-02-10T00:00:00Z","ddc":["520"],"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>"}],"date_created":"2026-02-17T08:12:05Z","status":"public","corr_author":"1","year":"2026","publisher":"EDP Sciences","citation":{"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>.","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).","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>.","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.","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>","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.","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>"},"PlanS_conform":"1","has_accepted_license":"1","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","file_date_updated":"2026-02-23T12:04:37Z","date_updated":"2026-04-28T12:01:21Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_type":"original","article_processing_charge":"Yes"},{"year":"2025","status":"public","external_id":{"isi":["001490583400004"]},"citation":{"short":"A. de Graaff, G. Brammer, A. Weibel, Z. Lewis, M.V. Maseda, P.A. Oesch, R. Bezanson, L.A. Boogaard, N.J. Cleri, O.R. Cooper, R. Gottumukkala, J.E. Greene, M. Hirschmann, R.E. Hviding, H. Katz, I. Labbé, J. Leja, J.J. Matthee, I. McConachie, T.B. Miller, R.P. Naidu, S.H. Price, H.-W. Rix, D.J. Setton, K.A. Suess, B. Wang, K.E. Whitaker, C.C. Williams, Astronomy &#38; Astrophysics 697 (2025).","chicago":"Graaff, Anna de, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V. Maseda, Pascal A. Oesch, Rachel Bezanson, et al. “RUBIES: A Complete Census of the Bright and Red Distant Universe with JWST/NIRSpec.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452186\">https://doi.org/10.1051/0004-6361/202452186</a>.","mla":"de Graaff, Anna, et al. “RUBIES: A Complete Census of the Bright and Red Distant Universe with JWST/NIRSpec.” <i>Astronomy &#38; Astrophysics</i>, vol. 697, A189, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452186\">10.1051/0004-6361/202452186</a>.","ieee":"A. de Graaff <i>et al.</i>, “RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec,” <i>Astronomy &#38; Astrophysics</i>, vol. 697. EDP Sciences, 2025.","ama":"de Graaff A, Brammer G, Weibel A, et al. RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec. <i>Astronomy &#38; Astrophysics</i>. 2025;697. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452186\">10.1051/0004-6361/202452186</a>","apa":"de Graaff, A., Brammer, G., Weibel, A., Lewis, Z., Maseda, M. V., Oesch, P. A., … Williams, C. C. (2025). RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452186\">https://doi.org/10.1051/0004-6361/202452186</a>","ista":"de Graaff A, Brammer G, Weibel A, Lewis Z, Maseda MV, Oesch PA, Bezanson R, Boogaard LA, Cleri NJ, Cooper OR, Gottumukkala R, Greene JE, Hirschmann M, Hviding RE, Katz H, Labbé I, Leja J, Matthee JJ, McConachie I, Miller TB, Naidu RP, Price SH, Rix H-W, Setton DJ, Suess KA, Wang B, Whitaker KE, Williams CC. 2025. RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec. Astronomy &#38; Astrophysics. 697, A189."},"publisher":"EDP Sciences","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","has_accepted_license":"1","article_processing_charge":"Yes","scopus_import":"1","article_type":"original","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_updated":"2025-09-30T12:45:25Z","file_date_updated":"2025-06-03T09:25:49Z","title":"RUBIES: A complete census of the bright and red distant universe with JWST/NIRSpec","intvolume":"       697","language":[{"iso":"eng"}],"day":"19","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","date_created":"2025-06-03T08:59:52Z","abstract":[{"lang":"eng","text":"We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES) providing JWST/NIRSpec spectroscopy of red sources selected across ∼150 arcmin2 from public JWST/NIRCam imaging in the UDS and EGS fields. The novel observing strategy of RUBIES offers a well-quantified selection function. The survey has been optimised to reach high (>70%) spectroscopic completeness for bright and red (F150W−F444W>2) sources that are very rare. To place these rare sources in context, we simultaneously observed a reference sample of the 2<z<7 galaxy population, sampling sources at a rate that is inversely proportional to their number density in the 3D parameter space of F444W magnitude, F150W−F444W colour, and photometric redshift. In total, RUBIES observed ∼3000 targets across 1<zphot<10 with both the PRISM and G395M dispersers and ∼1500 targets at zphot>3 using only the G395M disperser. The RUBIES data reveal a highly diverse population of red sources that span a broad redshift range (zspec∼1−9), with photometric redshift scatter and an outlier fraction that are three times higher than for similarly bright sources that are less red. This diversity is not apparent from the photometric spectral energy distributions (SEDs). Only spectroscopy reveals that the SEDs encompass a mixture of galaxies with dust-obscured star formation, extreme line emission, a lack of star formation indicating early quenching, and luminous active galactic nuclei. As a first demonstration of our broader selection function we compared the stellar masses and rest-frame U−V colours of the red sources and our reference sample. We find that the red sources are typically more massive (M*∼1010−11.5 M⊙) across all redshifts. However, we also find that the most massive systems span a wide range in U−V colour. We describe our data reduction procedure and data quality, and we publicly release the reduced RUBIES data and vetted spectroscopic redshifts of the first half of the survey through the DAWN JWST Archive."}],"ddc":["520"],"date_published":"2025-05-19T00:00:00Z","quality_controlled":"1","OA_type":"diamond","isi":1,"_id":"19784","oa":1,"OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"month":"05","volume":697,"type":"journal_article","publication_status":"published","acknowledgement":"We thank the CEERS and PRIMER teams for making their imaging data publicly available immediately. 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 #1345, #1837 #2234, #2279, #2514, #2750, #3990 and #4233. Support for program #4233 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. REH acknowledges support by the German Aerospace Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program 50OR2403 ‘RUBIES’. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #562. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant #140. 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. Support for this work for RPN 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. Open Access funding provided by Max Planck Society.","file":[{"date_created":"2025-06-03T09:25:49Z","date_updated":"2025-06-03T09:25:49Z","relation":"main_file","file_id":"19788","checksum":"cccf44629f28535dde91f2ebdf38c054","creator":"dernst","access_level":"open_access","file_size":6874721,"content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_deGraaff.pdf","success":1}],"article_number":"A189","doi":"10.1051/0004-6361/202452186","author":[{"full_name":"de Graaff, Anna","first_name":"Anna","last_name":"de Graaff"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"first_name":"Zach","full_name":"Lewis, Zach","last_name":"Lewis"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"full_name":"Cooper, Olivia R.","first_name":"Olivia R.","last_name":"Cooper"},{"full_name":"Gottumukkala, Rashmi","first_name":"Rashmi","last_name":"Gottumukkala"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"first_name":"Harley","full_name":"Katz, Harley","last_name":"Katz"},{"first_name":"Ivo","full_name":"Labbé, Ivo","last_name":"Labbé"},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"McConachie","full_name":"McConachie, Ian","first_name":"Ian"},{"last_name":"Miller","full_name":"Miller, Tim B.","first_name":"Tim B."},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Price","full_name":"Price, Sedona H.","first_name":"Sedona H."},{"full_name":"Rix, Hans-Walter","first_name":"Hans-Walter","last_name":"Rix"},{"last_name":"Setton","full_name":"Setton, David J.","first_name":"David J."},{"last_name":"Suess","full_name":"Suess, Katherine A.","first_name":"Katherine A."},{"last_name":"Wang","full_name":"Wang, Bingjie","first_name":"Bingjie"},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}]},{"author":[{"full_name":"Hovis-Afflerbach, B.","first_name":"B.","last_name":"Hovis-Afflerbach"},{"first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"full_name":"Schootemeijer, A.","first_name":"A.","last_name":"Schootemeijer"},{"last_name":"Klencki","first_name":"J.","full_name":"Klencki, J."},{"full_name":"Strom, A. L.","first_name":"A. L.","last_name":"Strom"},{"last_name":"Ludwig","first_name":"B. A.","full_name":"Ludwig, B. A."},{"first_name":"M. R.","full_name":"Drout, M. R.","last_name":"Drout"}],"article_number":"A239","file":[{"date_updated":"2025-06-10T07:00:38Z","relation":"main_file","date_created":"2025-06-10T07:00:38Z","success":1,"file_name":"2025_AstronomyAstrophysics_HovisAfflerbach.pdf","content_type":"application/pdf","file_size":6378030,"access_level":"open_access","file_id":"19799","checksum":"caa92beb22ab3146a75c5b03e926de1f","creator":"dernst"}],"doi":"10.1051/0004-6361/202453185","publication_status":"published","acknowledgement":"We thank the anonymous referee for providing a constructive report. We thank Tomer Shenar and Selma de Mink for the interesting discussions that helped us improve the content of Sect. 4. Thank you to Jorick Vink and Andreas Sander for helpful discussions about wind driving. BHA thanks the Caltech Summer Undergraduate Research Fellowship (SURF) program and Peter Adams for supporting this project in memory of Alain Porter and Arthur R. Adams. BHA thanks Gwen Rudie for organizing the Carnegie Astrophysics Summer Student Internship (CASSI) program and all the staff at Carnegie Observatories who help to support this program. BHA also thanks Laura Jaliff, Sal Wanying Fu, Ivanna Escala, Johanna Teske, Tony Piro, Brian Lorenz, and Peter Senchyna for their mentorship during this project. Computing resources used for this work were made possible by a grant from the Ahmanson Foundation. We thank the Observatories of the Carnegie Institution for Science for support, including Chris Burns for help with computations. This work used computing resources provided by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). This research was supported in part through the computational resources and staff contributions provided for the Quest high performance computing facility at Northwestern University which is jointly supported by the Office of the Provost, the Office for Research, and Northwestern University Information Technology. MRD acknowledges support from the NSERC through grant RGPIN-2019-06186, the Canada Research Chairs Program, and the Dunlap Institute at the University of Toronto. BHA is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-2234667.","month":"05","type":"journal_article","arxiv":1,"volume":697,"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","OA_place":"publisher","oa":1,"_id":"19797","isi":1,"OA_type":"diamond","quality_controlled":"1","ddc":["520"],"date_published":"2025-05-01T00:00:00Z","date_created":"2025-06-08T22:01:22Z","abstract":[{"lang":"eng","text":"Stars stripped of their hydrogen-rich envelopes through binary interaction are thought to be responsible for both hydrogen-poor supernovae and the hard ionizing radiation observed in low-Z galaxies. A population of these stars was recently observed for the first time, but their prevalence remains unknown. In preparation for such measurements, we estimate the mass distribution of hot, stripped stars using a population synthesis code that interpolates over detailed single and binary stellar evolution tracks. We predict that for a constant star formation rate of 1 M⊙/yr and regardless of metallicity, a scalable model population contains ∼30 000 stripped stars with mass Mstrip > 1 M⊙ and ∼4000 stripped stars that are sufficiently massive to explode (Mstrip > 2.6 M⊙). Below Mstrip = 5 M⊙, the distribution is metallicity-independent and can be described by a power law with the exponent α ∼ −2. At higher masses and lower metallicity (Z ≲ 0.002), the mass distribution exhibits a drop. This originates from the prediction, frequently seen in evolutionary models, that massive low-metallicity stars do not expand substantially until central helium burning or later and therefore cannot form long-lived stripped stars. With weaker line-driven winds at low metallicity, this suggests that neither binary interaction nor wind mass loss can efficiently strip massive stars at low metallicity. As a result, a “helium-star desert” emerges around Mstrip = 15 M⊙ at Z = 0.002, covering an increasingly large mass range with decreasing metallicity. We note that these high-mass stars are those that potentially boost a galaxy’s He+-ionizing radiation and that participate in the formation of merging black holes. This “helium-star desert” therefore merits further study."}],"day":"01","department":[{"_id":"YlGo"}],"publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"intvolume":"       697","title":"The mass distribution of stars stripped in binaries: The effect of metallicity","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2026-02-16T12:10:11Z","file_date_updated":"2025-06-10T07:00:38Z","article_processing_charge":"No","scopus_import":"1","article_type":"original","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","citation":{"apa":"Hovis-Afflerbach, B., Götberg, Y. L. L., Schootemeijer, A., Klencki, J., Strom, A. L., Ludwig, B. A., &#38; Drout, M. R. (2025). The mass distribution of stars stripped in binaries: The effect of metallicity. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202453185\">https://doi.org/10.1051/0004-6361/202453185</a>","ista":"Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, Klencki J, Strom AL, Ludwig BA, Drout MR. 2025. The mass distribution of stars stripped in binaries: The effect of metallicity. Astronomy &#38; Astrophysics. 697, A239.","ama":"Hovis-Afflerbach B, Götberg YLL, Schootemeijer A, et al. The mass distribution of stars stripped in binaries: The effect of metallicity. <i>Astronomy &#38; Astrophysics</i>. 2025;697. doi:<a href=\"https://doi.org/10.1051/0004-6361/202453185\">10.1051/0004-6361/202453185</a>","ieee":"B. Hovis-Afflerbach <i>et al.</i>, “The mass distribution of stars stripped in binaries: The effect of metallicity,” <i>Astronomy &#38; Astrophysics</i>, vol. 697. EDP Sciences, 2025.","mla":"Hovis-Afflerbach, B., et al. “The Mass Distribution of Stars Stripped in Binaries: The Effect of Metallicity.” <i>Astronomy &#38; Astrophysics</i>, vol. 697, A239, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202453185\">10.1051/0004-6361/202453185</a>.","short":"B. Hovis-Afflerbach, Y.L.L. Götberg, A. Schootemeijer, J. Klencki, A.L. Strom, B.A. Ludwig, M.R. Drout, Astronomy &#38; Astrophysics 697 (2025).","chicago":"Hovis-Afflerbach, B., Ylva Louise Linsdotter Götberg, A. Schootemeijer, J. Klencki, A. L. Strom, B. A. Ludwig, and M. R. Drout. “The Mass Distribution of Stars Stripped in Binaries: The Effect of Metallicity.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202453185\">https://doi.org/10.1051/0004-6361/202453185</a>."},"external_id":{"isi":["001494033100007"],"arxiv":["2412.05356"]},"status":"public","corr_author":"1","year":"2025"},{"date_created":"2025-06-15T22:01:29Z","abstract":[{"lang":"eng","text":"Context. The blue supergiant (BSG) domain contains a large variety of stars whose past and future evolutionary paths are still highly uncertain. Since binary interaction plays a crucial role in the fate of massive stars, investigating the multiplicity among BSGs helps shed light on the fate of such objects.\r\nAims. We aim to estimate the binary fraction of a large sample of BSGs in the Small Magellanic Cloud (SMC) within the Binarity at LOw Metallicity (BLOeM) survey. In total, we selected 262 targets with spectral types B0-B3 and luminosity classes I-II.\r\n\r\nMethods. This work is based on spectroscopic data collected by the FLAMES instrument, mounted on the Very Large Telescope, which gathered nine epochs over three months. Our spectroscopic analysis for each target includes the individual and peak-to-peak radial velocity measurements, an investigation of the line profile variability, and a periodogram analysis to search for possible short- and long-period binaries.\r\n\r\nResults. By applying a 20 km s−1 threshold on the peak-to-peak radial velocities above which we would consider the star to be binary, the resulting observed spectroscopic binary fraction for our BSG sample is 23 ± 3%. An independent analysis of line profile variability reveals 11 (plus 5 candidates) double-lined spectroscopic binaries and 32 (plus 41 candidates) single-lined spectroscopic binaries. Based on these results, we estimated the overall observed binary fraction in this sample to be 34 ± 3%, which is close to the computed intrinsic binary fraction of 40 ± 4%. In addition, we derived reliable orbital periods for 41 spectroscopic binaries and potential binary candidates, among which there are 17 eclipsing binaries, including 20 SB1 and SB2 systems with periods of less than 10 days. We reported a significant drop in the binary fraction of BSGs with spectral types later than B2 and effective temperatures less than 18 kK, which could indicate the end of the main sequence phase in this temperature regime. We found no metallicity dependence in the binary fraction of BSGs, compared to existing spectroscopic surveys of the Galaxy and Large Magellanic Cloud."}],"ddc":["520"],"date_published":"2025-06-01T00:00:00Z","day":"01","publication":"Astronomy & Astrophysics","department":[{"_id":"YlGo"}],"language":[{"iso":"eng"}],"intvolume":"       698","title":"Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud","article_processing_charge":"Yes","scopus_import":"1","article_type":"original","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2026-02-16T12:09:34Z","file_date_updated":"2025-06-25T08:38:02Z","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"mla":"Britavskiy, N., et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity of Early B-Type Supergiants in the Small Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A40, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452963\">10.1051/0004-6361/202452963</a>.","chicago":"Britavskiy, N., L. Mahy, D. J. Lennon, L. R. Patrick, H. Sana, J. I. Villaseñor, T. Shenar, et al. “Binarity at LOw Metallicity (BLOeM): Multiplicity of Early B-Type Supergiants in the Small Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452963\">https://doi.org/10.1051/0004-6361/202452963</a>.","short":"N. Britavskiy, L. Mahy, D.J. Lennon, L.R. Patrick, H. Sana, J.I. Villaseñor, T. Shenar, J. Bodensteiner, M. Bernini-Peron, S.R. Berlanas, D.M. Bowman, P.A. Crowther, S.E. De Mink, C.J. Evans, Y.L.L. Götberg, G. Holgado, C. Johnston, Z. Keszthelyi, J. Klencki, N. Langer, I. Mandel, A. Menon, M. Moe, L.M. Oskinova, D. Pauli, M. Pawlak, V. Ramachandran, M. Renzo, A.A.C. Sander, F.R.N. Schneider, A. Schootemeijer, K. Sen, S. Simón-Díaz, J.T. Van Loon, J.S. Vink, Astronomy &#38; Astrophysics 698 (2025).","ista":"Britavskiy N, Mahy L, Lennon DJ, Patrick LR, Sana H, Villaseñor JI, Shenar T, Bodensteiner J, Bernini-Peron M, Berlanas SR, Bowman DM, Crowther PA, De Mink SE, Evans CJ, Götberg YLL, Holgado G, Johnston C, Keszthelyi Z, Klencki J, Langer N, Mandel I, Menon A, Moe M, Oskinova LM, Pauli D, Pawlak M, Ramachandran V, Renzo M, Sander AAC, Schneider FRN, Schootemeijer A, Sen K, Simón-Díaz S, Van Loon JT, Vink JS. 2025. Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud. Astronomy &#38; Astrophysics. 698, A40.","apa":"Britavskiy, N., Mahy, L., Lennon, D. J., Patrick, L. R., Sana, H., Villaseñor, J. I., … Vink, J. S. (2025). Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452963\">https://doi.org/10.1051/0004-6361/202452963</a>","ama":"Britavskiy N, Mahy L, Lennon DJ, et al. Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452963\">10.1051/0004-6361/202452963</a>","ieee":"N. Britavskiy <i>et al.</i>, “Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025."},"publisher":"EDP Sciences","year":"2025","external_id":{"isi":["001497903100019"],"arxiv":["2502.12239"]},"status":"public","file":[{"file_name":"2025_AstronomyAstrophysics_Britavskiy.pdf","content_type":"application/pdf","success":1,"file_size":7106568,"access_level":"open_access","creator":"dernst","checksum":"53a9f290cb1f468895e0d4446e0020f0","file_id":"19901","relation":"main_file","date_updated":"2025-06-25T08:38:02Z","date_created":"2025-06-25T08:38:02Z"}],"article_number":"A40","doi":"10.1051/0004-6361/202452963","author":[{"full_name":"Britavskiy, N.","first_name":"N.","last_name":"Britavskiy"},{"first_name":"L.","full_name":"Mahy, L.","last_name":"Mahy"},{"last_name":"Lennon","full_name":"Lennon, D. J.","first_name":"D. J."},{"full_name":"Patrick, L. R.","first_name":"L. R.","last_name":"Patrick"},{"full_name":"Sana, H.","first_name":"H.","last_name":"Sana"},{"full_name":"Villaseñor, J. I.","first_name":"J. I.","last_name":"Villaseñor"},{"first_name":"T.","full_name":"Shenar, T.","last_name":"Shenar"},{"last_name":"Bodensteiner","first_name":"J.","full_name":"Bodensteiner, J."},{"last_name":"Bernini-Peron","first_name":"M.","full_name":"Bernini-Peron, M."},{"full_name":"Berlanas, S. R.","first_name":"S. R.","last_name":"Berlanas"},{"full_name":"Bowman, D. M.","first_name":"D. M.","last_name":"Bowman"},{"last_name":"Crowther","full_name":"Crowther, P. A.","first_name":"P. A."},{"full_name":"De Mink, S. E.","first_name":"S. E.","last_name":"De Mink"},{"last_name":"Evans","first_name":"C. J.","full_name":"Evans, C. J."},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"last_name":"Holgado","first_name":"G.","full_name":"Holgado, G."},{"full_name":"Johnston, C.","first_name":"C.","last_name":"Johnston"},{"last_name":"Keszthelyi","full_name":"Keszthelyi, Z.","first_name":"Z."},{"last_name":"Klencki","first_name":"J.","full_name":"Klencki, J."},{"last_name":"Langer","full_name":"Langer, N.","first_name":"N."},{"last_name":"Mandel","full_name":"Mandel, I.","first_name":"I."},{"last_name":"Menon","first_name":"A.","full_name":"Menon, A."},{"first_name":"M.","full_name":"Moe, M.","last_name":"Moe"},{"first_name":"L. M.","full_name":"Oskinova, L. M.","last_name":"Oskinova"},{"last_name":"Pauli","first_name":"D.","full_name":"Pauli, D."},{"last_name":"Pawlak","full_name":"Pawlak, M.","first_name":"M."},{"first_name":"V.","full_name":"Ramachandran, V.","last_name":"Ramachandran"},{"first_name":"M.","full_name":"Renzo, M.","last_name":"Renzo"},{"first_name":"A. A.C.","full_name":"Sander, A. A.C.","last_name":"Sander"},{"last_name":"Schneider","first_name":"F. R.N.","full_name":"Schneider, F. R.N."},{"first_name":"A.","full_name":"Schootemeijer, A.","last_name":"Schootemeijer"},{"last_name":"Sen","first_name":"K.","full_name":"Sen, K."},{"last_name":"Simón-Díaz","first_name":"S.","full_name":"Simón-Díaz, S."},{"full_name":"Van Loon, J. T.","first_name":"J. T.","last_name":"Van Loon"},{"last_name":"Vink","first_name":"J. S.","full_name":"Vink, J. S."}],"month":"06","type":"journal_article","volume":698,"arxiv":1,"publication_status":"published","acknowledgement":"We thank the anonymous referee for helpful comments that have improved the manuscript. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement 101164755/METAL) and was supported by the Israel Science Foundation (ISF) under grant number 2434/24. NB acknowledges support from the Belgian federal government grant for Ukrainian postdoctoral researchers (contract UF/2022/10). TS acknowledges support by the Israel Science Foundation (ISF) under grant number 0603225041. DP acknowledges financial support from the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005 and the FWO junior postdoctoral fellowship No. 1256225N. DMB gratefully acknowledges UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; PI Bowman; grant number: EP/Y031059/1), and a Royal Society University Research Fellowship (PI Bowman; grant number: URF\\R1\\231631). KS is funded by the National Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. IM acknowledges support from the Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery (OzGav), through project number CE230100016. JIV acknowledges support from the European Research Council through ERC Advanced Grant No. 101054731. SS-D, and GH acknowledge support from the Spanish Ministry of Science and Innovation and Universities (MICIU) through the Spanish State Research Agency (AEI) through grants PID2021-122397NB-C21, and the Severo Ochoa Program 2020-2023 (CEX2019-000920-S).","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","OA_place":"publisher","oa":1,"_id":"19841","isi":1,"quality_controlled":"1","OA_type":"diamond"},{"OA_type":"diamond","quality_controlled":"1","isi":1,"_id":"19842","oa":1,"OA_place":"publisher","oa_version":"Published Version","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"acknowledgement":"We thank Sipra Hota for kindly sharing the SMC UVIT catalogue prior to publication. LRP, FN. and FT acknowledge support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41 funded by 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. TS acknowledges support by the Israel Science Foundation (ISF) under grant number 0603225041. The research leading to these results has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement numbers 772225: MULTIPLES). DMB gratefully acknowledges support from UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1), and a Royal Society University Research Fellowship (grant number: URF\\R1\\231631). GGT is supported by the German Deutsche Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1, PI Sander). AACS is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group – Project-ID 445674056 (SA4064/1-1, PI Sander). GGT and AACS further acknowledges support from the Federal Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments. This paper benefited from discussions at the International Space Science Institute (ISSI) in Bern through ISSI International Team project 512 (Multiwavelength View on Massive Stars in the Era of Multimessenger Astronomy). DP acknowledges financial support by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005. JIV acknowledges support from the European Research Council for the ERC Advanced Grant 101054731. PAC is supported by the Science and Technology Facilities Council research grant ST/V000853/1 (PI. V. Dhillon). JSV is supported by Science and Technology Facilities Council funding under grant number ST/V000233/1. DFR is thankful for the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). This work has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 945806) and is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES Excellence Cluster).","publication_status":"published","type":"journal_article","arxiv":1,"volume":698,"month":"06","author":[{"last_name":"Patrick","first_name":"L. R.","full_name":"Patrick, L. R."},{"full_name":"Lennon, D. J.","first_name":"D. J.","last_name":"Lennon"},{"full_name":"Najarro, F.","first_name":"F.","last_name":"Najarro"},{"last_name":"Shenar","full_name":"Shenar, T.","first_name":"T."},{"last_name":"Bodensteiner","first_name":"J.","full_name":"Bodensteiner, J."},{"full_name":"Sana, H.","first_name":"H.","last_name":"Sana"},{"last_name":"Crowther","first_name":"P. A.","full_name":"Crowther, P. A."},{"last_name":"Britavskiy","first_name":"N.","full_name":"Britavskiy, N."},{"first_name":"N.","full_name":"Langer, N.","last_name":"Langer"},{"full_name":"Schootemeijer, A.","first_name":"A.","last_name":"Schootemeijer"},{"last_name":"Evans","first_name":"C. J.","full_name":"Evans, C. J."},{"full_name":"Mahy, L.","first_name":"L.","last_name":"Mahy"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"last_name":"De Mink","first_name":"S. E.","full_name":"De Mink, S. E."},{"first_name":"F. R.N.","full_name":"Schneider, F. R.N.","last_name":"Schneider"},{"full_name":"O’Grady, A. J.G.","first_name":"A. J.G.","last_name":"O’Grady"},{"last_name":"Villaseñor","full_name":"Villaseñor, J. I.","first_name":"J. I."},{"first_name":"M.","full_name":"Bernini-Peron, M.","last_name":"Bernini-Peron"},{"last_name":"Bowman","first_name":"D. M.","full_name":"Bowman, D. M."},{"full_name":"De Koter, A.","first_name":"A.","last_name":"De Koter"},{"last_name":"Deshmukh","full_name":"Deshmukh, K.","first_name":"K."},{"last_name":"Gilkis","full_name":"Gilkis, A.","first_name":"A."},{"full_name":"González-Torà, G.","first_name":"G.","last_name":"González-Torà"},{"last_name":"Kalari","first_name":"V. M.","full_name":"Kalari, V. M."},{"last_name":"K̃Eszthelyi","first_name":"Z.","full_name":"K̃Eszthelyi, Z."},{"last_name":"Mandel","full_name":"Mandel, I.","first_name":"I."},{"full_name":"Menon, A.","first_name":"A.","last_name":"Menon"},{"full_name":"Moe, M.","first_name":"M.","last_name":"Moe"},{"full_name":"Oskinova, L. M.","first_name":"L. M.","last_name":"Oskinova"},{"last_name":"Pauli","full_name":"Pauli, D.","first_name":"D."},{"last_name":"Renzo","first_name":"M.","full_name":"Renzo, M."},{"first_name":"A. A.C.","full_name":"Sander, A. A.C.","last_name":"Sander"},{"last_name":"Sen","full_name":"Sen, K.","first_name":"K."},{"first_name":"M.","full_name":"Stoop, M.","last_name":"Stoop"},{"last_name":"Van Loon","first_name":"J. T.","full_name":"Van Loon, J. T."},{"last_name":"Toonen","first_name":"S.","full_name":"Toonen, S."},{"last_name":"Tramper","full_name":"Tramper, F.","first_name":"F."},{"last_name":"Vink","first_name":"J. S.","full_name":"Vink, J. S."},{"last_name":"Wang","full_name":"Wang, C.","first_name":"C."}],"doi":"10.1051/0004-6361/202452949","file":[{"relation":"main_file","date_updated":"2025-06-23T07:09:38Z","date_created":"2025-06-23T07:09:38Z","file_name":"2025_AstronomyAstrophysics_Patrick.pdf","content_type":"application/pdf","success":1,"file_size":2130448,"access_level":"open_access","checksum":"93a907bf48da7e2ba7d75b53ea6011f5","creator":"dernst","file_id":"19863"}],"article_number":"A39","external_id":{"isi":["001497903100028"],"arxiv":["2502.02644"]},"status":"public","year":"2025","publisher":"EDP Sciences","citation":{"ista":"Patrick LR, Lennon DJ, Najarro F, Shenar T, Bodensteiner J, Sana H, Crowther PA, Britavskiy N, Langer N, Schootemeijer A, Evans CJ, Mahy L, Götberg YLL, De Mink SE, Schneider FRN, O’Grady AJG, Villaseñor JI, Bernini-Peron M, Bowman DM, De Koter A, Deshmukh K, Gilkis A, González-Torà G, Kalari VM, K̃Eszthelyi Z, Mandel I, Menon A, Moe M, Oskinova LM, Pauli D, Renzo M, Sander AAC, Sen K, Stoop M, Van Loon JT, Toonen S, Tramper F, Vink JS, Wang C. 2025. Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants. Astronomy &#38; Astrophysics. 698, A39.","apa":"Patrick, L. R., Lennon, D. J., Najarro, F., Shenar, T., Bodensteiner, J., Sana, H., … Wang, C. (2025). Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452949\">https://doi.org/10.1051/0004-6361/202452949</a>","ieee":"L. R. Patrick <i>et al.</i>, “Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025.","ama":"Patrick LR, Lennon DJ, Najarro F, et al. Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452949\">10.1051/0004-6361/202452949</a>","mla":"Patrick, L. R., et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity Properties and Evolution of BAF-Type Supergiants.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A39, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452949\">10.1051/0004-6361/202452949</a>.","chicago":"Patrick, L. R., D. J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner, H. Sana, P. A. Crowther, et al. “Binarity at LOw Metallicity (BLOeM): The Multiplicity Properties and Evolution of BAF-Type Supergiants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452949\">https://doi.org/10.1051/0004-6361/202452949</a>.","short":"L.R. Patrick, D.J. Lennon, F. Najarro, T. Shenar, J. Bodensteiner, H. Sana, P.A. Crowther, N. Britavskiy, N. Langer, A. Schootemeijer, C.J. Evans, L. Mahy, Y.L.L. Götberg, S.E. De Mink, F.R.N. Schneider, A.J.G. O’Grady, J.I. Villaseñor, M. Bernini-Peron, D.M. Bowman, A. De Koter, K. Deshmukh, A. Gilkis, G. González-Torà, V.M. Kalari, Z. K̃Eszthelyi, I. Mandel, A. Menon, M. Moe, L.M. Oskinova, D. Pauli, M. Renzo, A.A.C. Sander, K. Sen, M. Stoop, J.T. Van Loon, S. Toonen, F. Tramper, J.S. Vink, C. Wang, Astronomy &#38; Astrophysics 698 (2025)."},"has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2026-02-16T12:09:50Z","file_date_updated":"2025-06-23T07:09:38Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"scopus_import":"1","article_type":"original","article_processing_charge":"Yes","intvolume":"       698","title":"Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","department":[{"_id":"YlGo"}],"day":"01","date_published":"2025-06-01T00:00:00Z","ddc":["520"],"abstract":[{"text":"Given the uncertain evolutionary status of blue supergiant stars, their multiplicity properties hold vital clues to better understand their origin and evolution. As part of The Binarity at LOw Metallicity (BLOeM) campaign in the Small Magellanic Cloud, we present a multi-epoch spectroscopic survey of 128 supergiant stars of spectral type B5–F5, which roughly correspond to initial masses in the 6–30 M⊙ range. The observed binary fraction for the B5–9 supergiants is 25 ± 6% (10 ± 4%) and 5 ± 2% (0%) for the A–F stars, which were found using a radial-velocity (RV) variability threshold of 5 km s−1 (10 km s−1) as a criterion for binarity. Accounting for observational biases, we find an intrinsic multiplicity fraction of less than 18% for the B5–9 stars and 8−7+9% for the AF stars, for the orbital periods up to 103.5 days and mass ratios (q) in the 0.1 < q < 1 range. The large stellar radii of these supergiant stars prevent short orbital periods, but we demonstrate that this effect alone cannot explain our results. We assessed the spectra and RV time series of the detected binary systems and find that only a small fraction display convincing solutions. We conclude that the multiplicity fractions are compromised by intrinsic stellar variability, such that the true multiplicity fraction may be significantly smaller. Our main conclusions from comparing the multiplicity properties of the B5–9- and AF-type supergiants to that of their less evolved counterparts is that such stars cannot be explained by a direct evolution from the main sequence. Furthermore, by comparing their multiplicity properties to red supergiant stars, we conclude that the AF supergiant stars are neither progenitors nor descendants of red supergiants.","lang":"eng"}],"date_created":"2025-06-15T22:01:29Z"},{"OA_place":"publisher","oa":1,"_id":"19845","isi":1,"quality_controlled":"1","OA_type":"diamond","file":[{"date_updated":"2025-06-23T07:46:01Z","relation":"main_file","date_created":"2025-06-23T07:46:01Z","access_level":"open_access","checksum":"67600eba8bda24987a130ac334f10456","creator":"dernst","file_id":"19865","content_type":"application/pdf","success":1,"file_name":"2025_AstronomyAstrophysics_Oestlin.pdf","file_size":15858045}],"article_number":"A57","doi":"10.1051/0004-6361/202451723","author":[{"last_name":"Östlin","full_name":"Östlin, Göran","first_name":"Göran"},{"last_name":"Pérez-González","full_name":"Pérez-González, Pablo G.","first_name":"Pablo G."},{"full_name":"Melinder, Jens","first_name":"Jens","last_name":"Melinder"},{"first_name":"Steven","full_name":"Gillman, Steven","last_name":"Gillman"},{"first_name":"Edoardo","full_name":"Iani, Edoardo","orcid":"0000-0001-8386-3546","last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a"},{"last_name":"Costantin","first_name":"Luca","full_name":"Costantin, Luca"},{"last_name":"Boogaard","first_name":"Leindert A.","full_name":"Boogaard, Leindert A."},{"last_name":"Rinaldi","first_name":"Pierluigi","full_name":"Rinaldi, Pierluigi"},{"first_name":"Luis","full_name":"Colina, Luis","last_name":"Colina"},{"last_name":"Nørgaard-Nielsen","first_name":"Hans Ulrik","full_name":"Nørgaard-Nielsen, Hans Ulrik"},{"first_name":"Daniel","full_name":"Dicken, Daniel","last_name":"Dicken"},{"last_name":"Greve","full_name":"Greve, Thomas R.","first_name":"Thomas R."},{"last_name":"Wright","first_name":"Gillian","full_name":"Wright, Gillian"},{"full_name":"Alonso-Herrero, Almudena","first_name":"Almudena","last_name":"Alonso-Herrero"},{"first_name":"Javier","full_name":"Álvarez-Márquez, Javier","last_name":"Álvarez-Márquez"},{"first_name":"Marianna","full_name":"Annunziatella, Marianna","last_name":"Annunziatella"},{"first_name":"Arjan","full_name":"Bik, Arjan","last_name":"Bik"},{"last_name":"Bosman","full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I."},{"first_name":"Karina I.","full_name":"Caputi, Karina I.","last_name":"Caputi"},{"last_name":"Gomez","full_name":"Gomez, Alejandro Crespo","first_name":"Alejandro Crespo"},{"full_name":"Eckart, Andreas","first_name":"Andreas","last_name":"Eckart"},{"last_name":"Garcia-Marin","full_name":"Garcia-Marin, Macarena","first_name":"Macarena"},{"first_name":"Jens","full_name":"Hjorth, Jens","last_name":"Hjorth"},{"last_name":"Ilbert","first_name":"Olivier","full_name":"Ilbert, Olivier"},{"full_name":"Jermann, Iris","first_name":"Iris","last_name":"Jermann"},{"last_name":"Kendrew","full_name":"Kendrew, Sarah","first_name":"Sarah"},{"full_name":"Labiano, Alvaro","first_name":"Alvaro","last_name":"Labiano"},{"first_name":"Danial","full_name":"Langeroodi, Danial","last_name":"Langeroodi"},{"last_name":"Le Fevre","first_name":"Olivier","full_name":"Le Fevre, Olivier"},{"last_name":"Libralato","first_name":"Mattia","full_name":"Libralato, Mattia"},{"last_name":"Meyer","first_name":"Romain A.","full_name":"Meyer, Romain A."},{"last_name":"Moutard","first_name":"Thibaud","full_name":"Moutard, Thibaud"},{"last_name":"Peissker","first_name":"Florian","full_name":"Peissker, Florian"},{"first_name":"John P.","full_name":"Pye, John P.","last_name":"Pye"},{"first_name":"Tuomo V.","full_name":"Tikkanen, Tuomo V.","last_name":"Tikkanen"},{"last_name":"Topinka","full_name":"Topinka, Martin","first_name":"Martin"},{"first_name":"Fabian","full_name":"Walter, Fabian","last_name":"Walter"},{"first_name":"Martin","full_name":"Ward, Martin","last_name":"Ward"},{"last_name":"Van Der Werf","full_name":"Van Der Werf, Paul","first_name":"Paul"},{"last_name":"Van Dishoeck","first_name":"Ewine F.","full_name":"Van Dishoeck, Ewine F."},{"last_name":"Güdel","full_name":"Güdel, Manuel","first_name":"Manuel"},{"first_name":"Thomas","full_name":"Henning, Thomas","last_name":"Henning"},{"last_name":"Lagage","first_name":"Pierre Olivier","full_name":"Lagage, Pierre Olivier"},{"last_name":"Ray","full_name":"Ray, Tom P.","first_name":"Tom P."},{"full_name":"Vandenbussche, Bart","first_name":"Bart","last_name":"Vandenbussche"}],"month":"04","volume":696,"type":"journal_article","arxiv":1,"publication_status":"published","acknowledgement":"We dedicate this paper to the memory of our deceased and much valued MIRI-EC team members Hans Ulrik Nørgaard-Nielsen and Olivier Le Fèvre, both of whom played a central role in defining the MIDIS project. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The work presented is the effort of the entire MIRI team and the enthusiasm within the MIRI partnership is a significant factor in its success. The following National and International Funding Agencies funded and supported the MIRI development: NASA; ESA; Belgian Science Policy Office (BELSPO); Centre Nationale d’Etudes Spatiales (CNES); Danish National Space Centre; Deutsches Zentrum fur Luftund Raumfahrt (DLR); Enterprise Ireland; Ministerio De Economia y Competividad; Netherlands Research School for Astronomy (NOVA); Netherlands Organisation for Scientific Research (NWO); Science and Technology Facilities Council; Swiss Space Office; Swedish National Space Agency (SNSA); and UK Space Agency. MIRI drew on the scientific and technical expertise of the following organizations: Ames Research Center, USA; Airbus Defence and Space, UK; CEAIrfu, Saclay, France; Centre Spatial de Liège, Belgium; Consejo Superior de Investigaciones Cientficas, Spain; Carl Zeiss Optronics, Germany; Chalmers University of Technology, Sweden; Danish Space Research Institute, Denmark; Dublin Institute for Advanced Studies, Ireland; European Space Agency, Netherlands; ETCA, Belgium; ETH Zurich, Switzerland; Goddard Space Flight Center, USA; Institute d’Astrophysique Spatiale, France; Instituto Nacional de Técnica Aeroespacial,Spain; Institute for Astronomy, Edinburgh, UK; Jet Propulsion Laboratory, USA; Laboratoire d’Astrophysique de Marseille (LAM), France; Leiden University, Netherlands; Lockheed Advanced Technology Center (USA); NOVA Opt-IR group at Dwingeloo, Netherlands; Northrop Grumman, USA; Max Planck Institut f ür Astronomie (MPIA), Heidelberg, Germany; Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique (LESIA), France; Paul Scherrer Institut, Switzerland; Raytheon Vision Systems, USA; RUAG Aerospace, Switzerland; Rutherford Appleton Laboratory (RAL Space), UK; Space Telescope Science Institute, USA; Stockholm University, Sweden; Toegepast- Natuurwetenschappelijk Onderzoek (TNOTPD), Netherlands; UK Astronomy Technology Centre, UK; University College London, UK; University of Amsterdam, Netherlands; University of Arizona, USA; University of Cardiff, UK; University of Cologne, Germany; University of Ghent; University of Groningen, Netherlands; University of Leicester, UK; University of Leuven, Belgium; Utah State University, USA. Additional acknowledgements related to specific grants: G.Ö., J.M. and A.B. acknowledges funding from the Swedish National Space Administration (SNSA). P.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. This work was supported by research grants (VIL16599,VIL54489) from VILLUM FONDEN. L.C. and J.A.-M. acknowledge support by grant PIB2021-127718NB-100 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. M.A. acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2020-T2/TIC-19971. J.P.P. and T.V.T. acknowledge financial support from the UK Science and Technology Facilities Council, and the UK Space Agency. A.A.-H. acknowledges financial support from grant PID2021-124665NB-I00 funded by MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”. E.I. and K.I.C. acknowledge funding from the Netherlands Research School for Astronomy (NOVA). K.I.C. acknowledges funding from the Dutch Research Council (NWO) through the award of the Vici Grant VI.C.212.036. RAM acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The paper uses JWST data from programme #1283, obtained from the Barbara Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (STScI). For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) licence to the Author Accepted Manuscript version arising from this submission.","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","article_processing_charge":"Yes","scopus_import":"1","article_type":"original","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2026-02-16T12:10:36Z","file_date_updated":"2025-06-23T07:46:01Z","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"mla":"Östlin, Göran, et al. “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey Description and Early Results for the Galaxy Population Detected at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>, vol. 696, A57, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451723\">10.1051/0004-6361/202451723</a>.","chicago":"Östlin, Göran, Pablo G. Pérez-González, Jens Melinder, Steven Gillman, Edoardo Iani, Luca Costantin, Leindert A. Boogaard, et al. “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey Description and Early Results for the Galaxy Population Detected at 5.6 Μm.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202451723\">https://doi.org/10.1051/0004-6361/202451723</a>.","short":"G. Östlin, P.G. Pérez-González, J. Melinder, S. Gillman, E. Iani, L. Costantin, L.A. Boogaard, P. Rinaldi, L. Colina, H.U. Nørgaard-Nielsen, D. Dicken, T.R. Greve, G. Wright, A. Alonso-Herrero, J. Álvarez-Márquez, M. Annunziatella, A. Bik, S.E.I. Bosman, K.I. Caputi, A.C. Gomez, A. Eckart, M. Garcia-Marin, J. Hjorth, O. Ilbert, I. Jermann, S. Kendrew, A. Labiano, D. Langeroodi, O. Le Fevre, M. Libralato, R.A. Meyer, T. Moutard, F. Peissker, J.P. Pye, T.V. Tikkanen, M. Topinka, F. Walter, M. Ward, P. Van Der Werf, E.F. Van Dishoeck, M. Güdel, T. Henning, P.O. Lagage, T.P. Ray, B. Vandenbussche, Astronomy &#38; Astrophysics 696 (2025).","ista":"Östlin G, Pérez-González PG, Melinder J, Gillman S, Iani E, Costantin L, Boogaard LA, Rinaldi P, Colina L, Nørgaard-Nielsen HU, Dicken D, Greve TR, Wright G, Alonso-Herrero A, Álvarez-Márquez J, Annunziatella M, Bik A, Bosman SEI, Caputi KI, Gomez AC, Eckart A, Garcia-Marin M, Hjorth J, Ilbert O, Jermann I, Kendrew S, Labiano A, Langeroodi D, Le Fevre O, Libralato M, Meyer RA, Moutard T, Peissker F, Pye JP, Tikkanen TV, Topinka M, Walter F, Ward M, Van Der Werf P, Van Dishoeck EF, Güdel M, Henning T, Lagage PO, Ray TP, Vandenbussche B. 2025. MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. Astronomy &#38; Astrophysics. 696, A57.","apa":"Östlin, G., Pérez-González, P. G., Melinder, J., Gillman, S., Iani, E., Costantin, L., … Vandenbussche, B. (2025). MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451723\">https://doi.org/10.1051/0004-6361/202451723</a>","ama":"Östlin G, Pérez-González PG, Melinder J, et al. MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm. <i>Astronomy &#38; Astrophysics</i>. 2025;696. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451723\">10.1051/0004-6361/202451723</a>","ieee":"G. Östlin <i>et al.</i>, “MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm,” <i>Astronomy &#38; Astrophysics</i>, vol. 696. EDP Sciences, 2025."},"publisher":"EDP Sciences","year":"2025","external_id":{"isi":["001459780300005"],"arxiv":["2411.19686 "]},"status":"public","date_created":"2025-06-15T22:01:30Z","abstract":[{"text":"Context. The recently launched James Webb Space Telescope (JWST) is opening new observing windows on the distant Universe. Among JWST’s instruments, the Mid Infrared Instrument (MIRI) offers the unique capability of imaging observations at wavelengths of λ > 5 μm. This enables unique access to the rest frame near-infrared (NIR, λ ≥ 1 μm) emission from galaxies at redshifts of z > 4 and the visual (λ ≳ 5000 Å) rest frame for z > 9. We report here on the guaranteed time observations (GTO), from the MIRI European Consortium, of the Hubble Ultra Deep Field (HUDF), forming the MIRI Deep Imaging Survey (MIDIS), consisting of an on source integration time of ∼41 hours in the MIRI/F560W (5.6 μm) filter. The F560W filter was selected since it would produce the deepest data in terms of AB magnitudes in a given time. To our knowledge, this constitutes the longest single filter exposure obtained with JWST of an extragalactic field as of yet.\r\nAims. The HUDF is one of the most observed extragalactic fields, with extensive multi-wavelength coverage, where (before JWST) galaxies up to z ∼ 7 have been confirmed, and at z > 10 suggested, from HST photometry. We aim to characterise the galaxy population in HUDF at 5.6 μm, enabling studies such as: the rest frame NIR morphologies for galaxies at z ≲ 4.6, probing mature stellar populations and emission lines in z > 6 sources, intrinsically red and dusty galaxies, and active galactic nuclei (AGNs) and their host galaxies at intermediate redshifts.\r\n\r\nMethods. We reduced the MIRI data using the official JWST pipeline, augmented by in-house custom scripts. We measured the noise characteristics of the resulting image. Galaxy photometry was obtained, and photometric redshifts were estimated for sources with available multi-wavelength photometry (and compared to spectroscopic redshifts when available).\r\n\r\nResults. Over the deepest part of our image, the 5σ point source limit is 28.65 mag AB (12.6 nJy), ∼0.35 mag better than predicted by the JWST exposure time calculator. We find ∼2500 sources, the overwhelming majority of which are distant galaxies, but we note that spurious sources likely remain at faint magnitudes due to imperfect cosmic ray rejection in the JWST pipeline. More than 500 galaxies with available spectroscopic redshifts, up to z ≈ 11, have been identified, the majority of which are at z < 6. More than 1000 galaxies have reliable photometric redshift estimates, of which ∼25 are at 6 < z < 12. The point spread function in the F560W filter has a full width at half maximum (FWHM) of ≈0.2″ (corresponding to 1.4 kpc at z = 4), allowing the NIR rest frame morphologies and stellar mass distributions to be resolved for z < 4.5. Moreover, > 100 objects with very red NIRCam vs MIRI (3.6–5.6 μm > 1 mag) colours have been found, suggestive of dusty or old stellar populations at high redshifts.\r\n\r\nConclusions. We conclude that MIDIS surpasses preflight expectations and that deep MIRI imaging has great potential to characterise the galaxy population from cosmic noon to dawn.","lang":"eng"}],"ddc":["520"],"date_published":"2025-04-01T00:00:00Z","day":"01","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"title":"MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm","intvolume":"       696"},{"isi":1,"OA_type":"diamond","quality_controlled":"1","OA_place":"publisher","oa":1,"_id":"19929","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","author":[{"first_name":"Siddhartha","full_name":"Gurung-López, Siddhartha","last_name":"Gurung-López"},{"full_name":"Byrohl, Chris","first_name":"Chris","last_name":"Byrohl"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"last_name":"Spinoso","full_name":"Spinoso, Daniele","first_name":"Daniele"},{"first_name":"Alberto","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa"},{"full_name":"Fernández-Soto, Alberto","first_name":"Alberto","last_name":"Fernández-Soto"},{"last_name":"Arnalte-Mur","first_name":"Pablo","full_name":"Arnalte-Mur, Pablo"},{"last_name":"Martínez","first_name":"Vicent J.","full_name":"Martínez, Vicent J."}],"article_number":"A139","file":[{"relation":"main_file","date_updated":"2025-06-30T08:28:40Z","date_created":"2025-06-30T08:28:40Z","access_level":"open_access","file_id":"19933","creator":"dernst","checksum":"a50a817b72f03534c6a867035b51e433","content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_GurungLopez.pdf","success":1,"file_size":5758102}],"doi":"10.1051/0004-6361/202453547","publication_status":"published","acknowledgement":"The authors acknowledge the financial support from the MICIU with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022) Project (VAL-JPAS), reference ASFAE/2022/025. This work is part of the research Project PID2023-149420NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU. This work is also supported by the project of excellence PROMETEO CIPROM/2023/21 of the Conselleria de Educación, Universidades y Empleo (Generalitat Valenciana). MG thanks the Max Planck Society for support through the Max Planck Research Group. DS acknowledges the support by the Tsinghua Shui Mu Scholarship, funding of the National Key R&D Program of China (grant no. 2023YFA1605600), the science research grants from the China Manned Space Project with no. CMS-CSST2021-A05, and the Tsinghua University Initiative Scientific Research Program (no. 20223080023). This research made use of matplotlib, a Python library for publication quality graphics (Hunter 2007), NumPy (Harris et al. 2020) and SciPy (Virtanen et al. 2020).","month":"06","volume":698,"arxiv":1,"type":"journal_article","publisher":"EDP Sciences","citation":{"ieee":"S. Gurung-López <i>et al.</i>, “zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural networks,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025.","ama":"Gurung-López S, Byrohl C, Gronke M, et al. zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural networks. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202453547\">10.1051/0004-6361/202453547</a>","ista":"Gurung-López S, Byrohl C, Gronke M, Spinoso D, Torralba Torregrosa A, Fernández-Soto A, Arnalte-Mur P, Martínez VJ. 2025. zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural networks. Astronomy &#38; Astrophysics. 698, A139.","apa":"Gurung-López, S., Byrohl, C., Gronke, M., Spinoso, D., Torralba Torregrosa, A., Fernández-Soto, A., … Martínez, V. J. (2025). zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural networks. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202453547\">https://doi.org/10.1051/0004-6361/202453547</a>","short":"S. Gurung-López, C. Byrohl, M. Gronke, D. Spinoso, A. Torralba Torregrosa, A. Fernández-Soto, P. Arnalte-Mur, V.J. Martínez, Astronomy &#38; Astrophysics 698 (2025).","chicago":"Gurung-López, Siddhartha, Chris Byrohl, Max Gronke, Daniele Spinoso, Alberto Torralba Torregrosa, Alberto Fernández-Soto, Pablo Arnalte-Mur, and Vicent J. Martínez. “ZELDA II: Reconstruction of Galactic Lyman-Alpha Spectra Attenuated by the Intergalactic Medium Using Neural Networks.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202453547\">https://doi.org/10.1051/0004-6361/202453547</a>.","mla":"Gurung-López, Siddhartha, et al. “ZELDA II: Reconstruction of Galactic Lyman-Alpha Spectra Attenuated by the Intergalactic Medium Using Neural Networks.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A139, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202453547\">10.1051/0004-6361/202453547</a>."},"status":"public","external_id":{"arxiv":["2501.04077"],"isi":["001507317300003"]},"year":"2025","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"file_date_updated":"2025-06-30T08:28:40Z","date_updated":"2026-02-16T12:11:56Z","article_processing_charge":"No","article_type":"original","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","language":[{"iso":"eng"}],"title":"zELDA II: Reconstruction of galactic Lyman-alpha spectra attenuated by the intergalactic medium using neural networks","intvolume":"       698","ddc":["520"],"date_published":"2025-06-01T00:00:00Z","date_created":"2025-06-29T22:01:15Z","abstract":[{"lang":"eng","text":"Context. The observed Lyman-alpha (Lyα) line profile is a convolution of the complex Lyα radiative transfer taking place in the interstellar, circumgalactic, and intergalactic media (ISM, CGM, and IGM, respectively). Discerning the different components of the Lyα line is crucial in order to use it as a probe of galaxy formation or the evolution of the IGM.\r\n\r\nAims. We aim to present the second version of zELDA (redshift Estimator for Line profiles of Distant Lyman-Alpha emitters), an open-source Python module focused on modelling and fitting observed Lyα line profiles. This new version of zELDA focuses on disentangling the galactic from the IGM effects.\r\n\r\nMethods. We built realistic Lyα line profiles that include the ISM and IGM contributions by combining the Monte Carlo radiative-transfer simulations for the so-called shell model (ISM) and IGM transmission curves generated from TNG100. We used these mock line profiles to train different artificial neural networks. These use the observed spectrum as input and the outflow parameters of the best fitting ‘shell model’ as output along with the redshift and Lyα emission IGM escape fraction of the source.\r\n\r\nResults. We measured the accuracy of zELDA on mock Lyα line profiles. We find that zELDA is capable of reconstructing the ISM emerging Lyα line profile with high levels of accuracy (Kolmogórov-Smirnov<0.1) for 95% of the cases for HST/COS-like observations and 80% for MUSE-WIDE-like observations. zELDA is able to measure the IGM transmission with typical uncertainties below 10% for HST/COS and MUSE-WIDE data.\r\n\r\nConclusions. This work represents a step forward in the high-precision reconstruction of IGM-attenuated Lyα line profiles. zELDA allows the disentanglement of the galactic and IGM contribution shaping the Lyα line shape and thus allows us to use Lyα as a tool to study galaxy and ISM evolution."}],"day":"01","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics"},{"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","author":[{"last_name":"Dottorini","first_name":"D.","full_name":"Dottorini, D."},{"full_name":"Calabrò, A.","first_name":"A.","last_name":"Calabrò"},{"first_name":"L.","full_name":"Pentericci, L.","last_name":"Pentericci"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara"},{"last_name":"Llerena","full_name":"Llerena, M.","first_name":"M."},{"last_name":"Napolitano","full_name":"Napolitano, L.","first_name":"L."},{"last_name":"Santini","first_name":"P.","full_name":"Santini, P."},{"full_name":"Roberts-Borsani, G.","first_name":"G.","last_name":"Roberts-Borsani"},{"last_name":"Castellano","first_name":"M.","full_name":"Castellano, M."},{"first_name":"R.","full_name":"Amorin, R.","last_name":"Amorin"},{"first_name":"M.","full_name":"Dickinson, M.","last_name":"Dickinson"},{"last_name":"Fontana","full_name":"Fontana, A.","first_name":"A."},{"last_name":"Hathi","full_name":"Hathi, N.","first_name":"N."},{"first_name":"M.","full_name":"Hirschmann, M.","last_name":"Hirschmann"},{"first_name":"A. M.","full_name":"Koekemoer, A. M.","last_name":"Koekemoer"},{"full_name":"Lucas, R. A.","first_name":"R. A.","last_name":"Lucas"},{"last_name":"Merlin","first_name":"E.","full_name":"Merlin, E."},{"full_name":"Morales, A.","first_name":"A.","last_name":"Morales"},{"last_name":"Pacucci","first_name":"F.","full_name":"Pacucci, F."},{"full_name":"Wilkins, S.","first_name":"S.","last_name":"Wilkins"},{"last_name":"Arrabal Haro","full_name":"Arrabal Haro, P.","first_name":"P."},{"last_name":"Bagley","first_name":"M.","full_name":"Bagley, M."},{"last_name":"Finkelstein","full_name":"Finkelstein, S. L.","first_name":"S. L."},{"last_name":"Kartaltepe","full_name":"Kartaltepe, J.","first_name":"J."},{"full_name":"Papovich, C.","first_name":"C.","last_name":"Papovich"},{"last_name":"Pirzkal","full_name":"Pirzkal, N.","first_name":"N."}],"doi":"10.1051/0004-6361/202453267","file":[{"content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_Dottorini.pdf","success":1,"file_size":2442076,"access_level":"open_access","file_id":"19932","checksum":"100f897d468de9d0113277c870035b62","creator":"dernst","relation":"main_file","date_updated":"2025-06-30T08:22:08Z","date_created":"2025-06-30T08:22:08Z"}],"article_number":"A234","acknowledgement":"We acknowledges support from the INAF Large Grant for Extragalactic Surveys with JWST and from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. PS acknowledges INAF Mini Grant 2022 “The evolution of passive galaxies through cosmic time”. Part of the research activities described in this paper were carried out with the contribution of the Next Generation EU funds within the National Recovery and Resilience Plan (PNRR), Mission 4 – Education and Research, Component 2 – From Research to Business (M4C2), Investment Line 3.1 – Strengthening and creation of Research Infrastructures, Project IR0000034 – “STILES – Strengthening the Italian Leadership in ELT and SKA”. RA acknowledges support of Grant project 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.","publication_status":"published","arxiv":1,"volume":698,"type":"journal_article","month":"06","isi":1,"OA_type":"diamond","quality_controlled":"1","OA_place":"publisher","_id":"19930","oa":1,"language":[{"iso":"eng"}],"title":"Evolution of the UV slope of galaxies at cosmic morning (z > 4): The properties of extremely blue galaxies","intvolume":"       698","date_published":"2025-06-01T00:00:00Z","ddc":["520"],"abstract":[{"lang":"eng","text":"We present an analysis of the UV continuum slope, β, using a sample of 726 galaxies with z > 4, selected from a mixture of JWST ERS, GTO, and GO observational programs. We considered only spectroscopic data obtained with the low-resolution (R ∼ 30 − 300) PRISM/CLEAR NIRSpec configuration. Studying the correlation between β and MUV, we find an overall decreasing trend, described by β = ( − 0.055 ± 0.017)MUV + ( − 2.98 ± 0.34). This is consistent with previous studies, where brighter galaxies show redder β values. However, when analyzing the trend in separate redshift bins, we find that at high redshift the relation becomes much flatter and is consistent with a flat slope within 1σ. Furthermore, we find that β tends to decrease with redshift, following β = ( − 0.075 ± 0.010)z + ( − 1.496 ± 0.056). This is consistent with most recent results showing a steepening of the spectra at higher z. We selected a sample of galaxies with extremely blue slopes (i.e., β < −2.6). Such slopes are steeper than predicted by stellar evolution models – even for dust-free, young, metal-poor populations – when the contribution of nebular emission is included. We selected 44 extremely blue galaxies (XBGs) and investigated the possible physical origin of their steep slopes by comparing them to a subsample of redder galaxies (matched in Δz = ±0.5 and ΔMUV = ±0.2). We find that XBGs have younger stellar populations, stronger ionization fields, lower dust attenuation, and lower but not pristine metallicity (∼10% Z⊙) compared to red galaxies. However, these properties alone cannot explain the extreme β values. Using indirect inference of Lyman continuum escape with the most recent models, we estimated the escape fraction fesc > 10% in at least 25% of the XBGs, whereas all the red sources exhibit much lower fesc values. A reduced nebular continuum contribution – resulting from either a high escape fraction or a bursty star formation history – is likely the origin of the extremely blue slopes."}],"date_created":"2025-06-29T22:01:15Z","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","day":"01","publisher":"EDP Sciences","citation":{"ieee":"D. Dottorini <i>et al.</i>, “Evolution of the UV slope of galaxies at cosmic morning (z &#62; 4): The properties of extremely blue galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025.","ama":"Dottorini D, Calabrò A, Pentericci L, et al. Evolution of the UV slope of galaxies at cosmic morning (z &#62; 4): The properties of extremely blue galaxies. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202453267\">10.1051/0004-6361/202453267</a>","apa":"Dottorini, D., Calabrò, A., Pentericci, L., Mascia, S., Llerena, M., Napolitano, L., … Pirzkal, N. (2025). Evolution of the UV slope of galaxies at cosmic morning (z &#62; 4): The properties of extremely blue galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202453267\">https://doi.org/10.1051/0004-6361/202453267</a>","ista":"Dottorini D, Calabrò A, Pentericci L, Mascia S, Llerena M, Napolitano L, Santini P, Roberts-Borsani G, Castellano M, Amorin R, Dickinson M, Fontana A, Hathi N, Hirschmann M, Koekemoer AM, Lucas RA, Merlin E, Morales A, Pacucci F, Wilkins S, Arrabal Haro P, Bagley M, Finkelstein SL, Kartaltepe J, Papovich C, Pirzkal N. 2025. Evolution of the UV slope of galaxies at cosmic morning (z &#62; 4): The properties of extremely blue galaxies. Astronomy &#38; Astrophysics. 698, A234.","chicago":"Dottorini, D., A. Calabrò, L. Pentericci, Sara Mascia, M. Llerena, L. Napolitano, P. Santini, et al. “Evolution of the UV Slope of Galaxies at Cosmic Morning (z &#62; 4): The Properties of Extremely Blue Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202453267\">https://doi.org/10.1051/0004-6361/202453267</a>.","short":"D. Dottorini, A. Calabrò, L. Pentericci, S. Mascia, M. Llerena, L. Napolitano, P. Santini, G. Roberts-Borsani, M. Castellano, R. Amorin, M. Dickinson, A. Fontana, N. Hathi, M. Hirschmann, A.M. Koekemoer, R.A. Lucas, E. Merlin, A. Morales, F. Pacucci, S. Wilkins, P. Arrabal Haro, M. Bagley, S.L. Finkelstein, J. Kartaltepe, C. Papovich, N. Pirzkal, Astronomy &#38; Astrophysics 698 (2025).","mla":"Dottorini, D., et al. “Evolution of the UV Slope of Galaxies at Cosmic Morning (z &#62; 4): The Properties of Extremely Blue Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A234, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202453267\">10.1051/0004-6361/202453267</a>."},"external_id":{"arxiv":["2412.01623"],"isi":["001510826300019"]},"status":"public","year":"2025","date_updated":"2026-02-16T12:11:39Z","file_date_updated":"2025-06-30T08:22:08Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"scopus_import":"1","article_type":"original","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1"},{"isi":1,"OA_type":"diamond","quality_controlled":"1","OA_place":"publisher","_id":"19931","oa":1,"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","author":[{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"last_name":"Secunda","first_name":"Amy R.","full_name":"Secunda, Amy R."},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"last_name":"Zitrin","first_name":"Adi","full_name":"Zitrin, Adi"},{"last_name":"Labbé","first_name":"Ivo","full_name":"Labbé, Ivo"},{"last_name":"Golubchik","first_name":"Miriam","full_name":"Golubchik, Miriam"},{"first_name":"Rachel","full_name":"Bezanson, Rachel","last_name":"Bezanson"},{"last_name":"Kokorev","full_name":"Kokorev, Vasily","first_name":"Vasily"},{"first_name":"Hakim","full_name":"Atek, Hakim","last_name":"Atek"},{"last_name":"Brammer","full_name":"Brammer, Gabriel B.","first_name":"Gabriel B."},{"first_name":"Iryna","full_name":"Chemerynska, Iryna","last_name":"Chemerynska"},{"full_name":"Cutler, Sam E.","first_name":"Sam E.","last_name":"Cutler"},{"last_name":"Dayal","first_name":"Pratika","full_name":"Dayal, Pratika"},{"full_name":"Feldmann, Robert","first_name":"Robert","last_name":"Feldmann"},{"last_name":"Fujimoto","full_name":"Fujimoto, Seiji","first_name":"Seiji"},{"full_name":"Glazebrook, Karl","first_name":"Karl","last_name":"Glazebrook"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"full_name":"Ma, Yilun","first_name":"Yilun","last_name":"Ma"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Nelson","full_name":"Nelson, Erica J.","first_name":"Erica J."},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"full_name":"Pan, Richard","first_name":"Richard","last_name":"Pan"},{"full_name":"Price, Sedona H.","first_name":"Sedona H.","last_name":"Price"},{"last_name":"Suess","first_name":"Katherine A.","full_name":"Suess, Katherine A."},{"full_name":"Wang, Bingjie","first_name":"Bingjie","last_name":"Wang"},{"first_name":"John R.","full_name":"Weaver, John R.","last_name":"Weaver"},{"full_name":"Whitaker, Katherine E.","first_name":"Katherine E.","last_name":"Whitaker"}],"file":[{"file_name":"2025_AstronomyAstrophysics_Furtak.pdf","content_type":"application/pdf","success":1,"file_size":1835865,"access_level":"open_access","file_id":"19934","creator":"dernst","checksum":"567fa02a9791d489355ec75d02bb1cb9","date_updated":"2025-06-30T08:44:24Z","relation":"main_file","date_created":"2025-06-30T08:44:24Z"}],"article_number":"A227","doi":"10.1051/0004-6361/202554110","publication_status":"published","acknowledgement":"We would like to thank Xihan Ji, Hannah Übler, and Roberto Maiolino, for cordial and useful discussions. The BGU lensing group acknowledges support by grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF), and by the Israel Science Foundation Grant No. 864/23. P.D. warmly thanks the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. This work is based on observations obtained with the NASA/ESA/CSA JWST, namely programs GO-2756, -2561, -2883, -3538, -4111, and -3516, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The spectroscopy products presented herein, from JWST program GO-2561, were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140. The data used in this work may be retrieved from the MAST archive at: http://dx.doi.org/10.17909/p7t7-te67. This work also makes use of the Center for Computational Astrophysics at the Flatiron Institute which is supported by the Simons Foundation. Support for JWST programs GO-2561, -4111, and -3516 was provided by NASA through grants from STScI. This research made use of Astropy, (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018) and Photutils, an Astropy package for detection and photometry of astronomical sources (Bradley et al. 2024), as well as the packages NumPy (van der Walt et al. 2011), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), and the MAAT Astronomy and Astrophysics tools for MATLAB (Ofek 2014).","month":"06","volume":698,"arxiv":1,"type":"journal_article","publisher":"EDP Sciences","citation":{"chicago":"Furtak, Lukas J., Amy R. Secunda, Jenny E. Greene, Adi Zitrin, Ivo Labbé, Miriam Golubchik, Rachel Bezanson, et al. “Investigating Photometric and Spectroscopic Variability in the Multiply Imaged Little Red Dot A2744-QSO1.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202554110\">https://doi.org/10.1051/0004-6361/202554110</a>.","short":"L.J. Furtak, A.R. Secunda, J.E. Greene, A. Zitrin, I. Labbé, M. Golubchik, R. Bezanson, V. Kokorev, H. Atek, G.B. Brammer, I. Chemerynska, S.E. Cutler, P. Dayal, R. Feldmann, S. Fujimoto, K. Glazebrook, J. Leja, Y. Ma, J.J. Matthee, R.P. Naidu, E.J. Nelson, P.A. Oesch, R. Pan, S.H. Price, K.A. Suess, B. Wang, J.R. Weaver, K.E. Whitaker, Astronomy &#38; Astrophysics 698 (2025).","mla":"Furtak, Lukas J., et al. “Investigating Photometric and Spectroscopic Variability in the Multiply Imaged Little Red Dot A2744-QSO1.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A227, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202554110\">10.1051/0004-6361/202554110</a>.","ieee":"L. J. Furtak <i>et al.</i>, “Investigating photometric and spectroscopic variability in the multiply imaged little red dot A2744-QSO1,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025.","ama":"Furtak LJ, Secunda AR, Greene JE, et al. Investigating photometric and spectroscopic variability in the multiply imaged little red dot A2744-QSO1. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202554110\">10.1051/0004-6361/202554110</a>","apa":"Furtak, L. J., Secunda, A. R., Greene, J. E., Zitrin, A., Labbé, I., Golubchik, M., … Whitaker, K. E. (2025). Investigating photometric and spectroscopic variability in the multiply imaged little red dot A2744-QSO1. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202554110\">https://doi.org/10.1051/0004-6361/202554110</a>","ista":"Furtak LJ, Secunda AR, Greene JE, Zitrin A, Labbé I, Golubchik M, Bezanson R, Kokorev V, Atek H, Brammer GB, Chemerynska I, Cutler SE, Dayal P, Feldmann R, Fujimoto S, Glazebrook K, Leja J, Ma Y, Matthee JJ, Naidu RP, Nelson EJ, Oesch PA, Pan R, Price SH, Suess KA, Wang B, Weaver JR, Whitaker KE. 2025. Investigating photometric and spectroscopic variability in the multiply imaged little red dot A2744-QSO1. Astronomy &#38; Astrophysics. 698, A227."},"external_id":{"arxiv":["2502.07875"],"isi":["001510826300017"]},"status":"public","year":"2025","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"file_date_updated":"2025-06-30T08:44:24Z","date_updated":"2026-02-16T12:11:22Z","article_processing_charge":"No","article_type":"original","scopus_import":"1","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"intvolume":"       698","title":"Investigating photometric and spectroscopic variability in the multiply imaged little red dot A2744-QSO1","ddc":["520"],"date_published":"2025-06-01T00:00:00Z","date_created":"2025-06-29T22:01:16Z","abstract":[{"text":"JWST observations have uncovered a new population of red, compact objects at high redshifts dubbed “little red dots” (LRDs), which typically show broad emission lines and are thought to be dusty active galactic nuclei (AGNs). Some of their other features, however, challenge the AGN explanation, such as prominent Balmer breaks and extremely faint or even missing metal high-ionization lines, X-ray, or radio emission, including in deep stacks. Time variability is another robust test of AGN activity. Here, we exploit the z = 7.045 multiply imaged LRD A2744-QSO1, which offers a particularly unique test of variability due to lensing-induced time delays between the three images spanning 22 yr (2.7 yr in the rest-frame), to investigate its photometric and spectroscopic variability. We find the equivalent widths (EWs) of the broad Hα and Hβ lines, which are independent of magnification and other systematics, to exhibit significant variations, of up to 18 ± 3% for Hα and up to 22 ± 8% in Hβ, on a timescale of 875 d (2.4 yr) in the rest-frame. This suggests that A2744-QSO1 is indeed an AGN. We find no significant photometric variability beyond the limiting systematic uncertainties, so it currently cannot be determined whether the EW variations are due to line-flux or continuum variability. These results are consistent with a typical damped random walk variability model for an AGN such as A2744-QSO1 (MBH = 4 × 107 M⊙) given the sparse sampling of the light curve with the available data. Our results therefore support the AGN interpretation of this LRD, and highlight the need for further photometric and spectroscopic monitoring in order to build a detailed and reliable light curve.","lang":"eng"}],"day":"01","publication":"Astronomy & Astrophysics","department":[{"_id":"JoMa"}]},{"publisher":"EDP Sciences","citation":{"ista":"Llerena M, Pentericci L, Napolitano L, Mascia S, Amorín R, Calabrò A, Castellano M, Cleri NJ, Giavalisco M, Grogin NA, Hathi NP, Hirschmann M, Koekemoer AM, Nanayakkara T, Pacucci F, Shen L, Wilkins SM, Yoon I, Yung LYA, Bhatawdekar R, Lucas RA, Wang X, Arrabal Haro P, Bagley MB, Finkelstein SL, Kartaltepe JS, Merlin E, Papovich C, Pirzkal N, Santini P. 2025. The ionizing photon production efficiency of star-forming galaxies at z ∼ 4–10. Astronomy &#38; Astrophysics. 698, A302.","apa":"Llerena, M., Pentericci, L., Napolitano, L., Mascia, S., Amorín, R., Calabrò, A., … Santini, P. (2025). The ionizing photon production efficiency of star-forming galaxies at z ∼ 4–10. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202453251\">https://doi.org/10.1051/0004-6361/202453251</a>","ama":"Llerena M, Pentericci L, Napolitano L, et al. The ionizing photon production efficiency of star-forming galaxies at z ∼ 4–10. <i>Astronomy &#38; Astrophysics</i>. 2025;698. doi:<a href=\"https://doi.org/10.1051/0004-6361/202453251\">10.1051/0004-6361/202453251</a>","ieee":"M. Llerena <i>et al.</i>, “The ionizing photon production efficiency of star-forming galaxies at z ∼ 4–10,” <i>Astronomy &#38; Astrophysics</i>, vol. 698. EDP Sciences, 2025.","mla":"Llerena, M., et al. “The Ionizing Photon Production Efficiency of Star-Forming Galaxies at z ∼ 4–10.” <i>Astronomy &#38; Astrophysics</i>, vol. 698, A302, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202453251\">10.1051/0004-6361/202453251</a>.","chicago":"Llerena, M., L. Pentericci, L. Napolitano, Sara Mascia, R. Amorín, A. Calabrò, M. Castellano, et al. “The Ionizing Photon Production Efficiency of Star-Forming Galaxies at z ∼ 4–10.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202453251\">https://doi.org/10.1051/0004-6361/202453251</a>.","short":"M. Llerena, L. Pentericci, L. Napolitano, S. Mascia, R. Amorín, A. Calabrò, M. Castellano, N.J. Cleri, M. Giavalisco, N.A. Grogin, N.P. Hathi, M. Hirschmann, A.M. Koekemoer, T. Nanayakkara, F. Pacucci, L. Shen, S.M. Wilkins, I. Yoon, L.Y.A. Yung, R. Bhatawdekar, R.A. Lucas, X. Wang, P. Arrabal Haro, M.B. Bagley, S.L. Finkelstein, J.S. Kartaltepe, E. Merlin, C. Papovich, N. Pirzkal, P. Santini, Astronomy &#38; Astrophysics 698 (2025)."},"external_id":{"arxiv":["2412.01358"],"isi":["001512479700026"]},"status":"public","year":"2025","file_date_updated":"2025-07-08T06:17:02Z","date_updated":"2026-02-16T12:12:15Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_type":"original","scopus_import":"1","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","language":[{"iso":"eng"}],"intvolume":"       698","title":"The ionizing photon production efficiency of star-forming galaxies at z ∼ 4–10","date_published":"2025-06-20T00:00:00Z","ddc":["520"],"abstract":[{"lang":"eng","text":"Context. Investigating the ionizing emission of star-forming galaxies and the escape fraction of ionizing photons is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends on not only the abundance of galaxies but also their efficiency in producing ionizing photons (ξion). This quantity is thus fundamental to quantify the role of faint versus bright sources in driving this process, as we must assess their relative contribution to the total ionizing emissivity.\r\n\r\nAims. Our goal is to estimate the ξion using Balmer lines (Hα or Hβ) in a sample of 761 galaxies at 4 ≤ z ≤ 10 selected from different JWST spectroscopic surveys. We aim to determine the redshift evolution of ξion and the relation of ξion with the physical properties of the galaxies.\r\n\r\nMethods. We used the available HST and JWST photometry to perform a spectral energy distribution (SED) fitting in the sample to determine their physical properties and relate them with ξion. We used the BAGPIPES code for the SED fitting and assumed a delayed exponential model for the star formation history. We used the NIRSpec spectra from prism or grating configurations to estimate Balmer luminosities, and then constrained ξion values after dust correction.\r\n\r\nResults. We find a mean value of 1025.22 Hz erg−1 for ξion in the sample with an observed scatter of 0.42 dex. We find an increase in the median values of ξion with redshift from 1025.09 Hz erg−1 at z ∼ 4.18 to 1025.28 Hz erg−1 at z ∼ 7.14, confirming the redshift evolution of ξion found in other studies. Regarding the relation between ξion and physical properties, we find a decrease in ξion with increasing stellar mass, indicating that low-mass galaxies are efficient producers of ionizing photons. We also find an increase in ξion with increasing specific star formation rate (sSFR) and increasing UV absolute magnitude. This indicates that faint galaxies and galaxies with high sSFR are also efficient producers. We also investigated the relation of ξion with the rest-frame equivalent width (EW) of [OIII]λ5007 and find that galaxies with the higher EW([OIII]λ5007) are more efficient producers of ionizing photons, with the best fit leading to the relation log(ξion)  =  0.43 × log(EW[OIII])+23.99. Similarly, we find that galaxies with higher O32 = [OIII]λ5007/[OII]λλ3727,3729 and lower gas-phase metallicities (based on the R23 = ([OIII]λλ4959,5007+[OII]λλ3727,3729)/Hβ calibration) show higher ξion values."}],"date_created":"2025-07-06T22:01:23Z","department":[{"_id":"JoMa"}],"publication":"Astronomy & Astrophysics","day":"20","isi":1,"OA_type":"diamond","quality_controlled":"1","OA_place":"publisher","oa":1,"_id":"19967","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa_version":"Published Version","author":[{"full_name":"Llerena, M.","first_name":"M.","last_name":"Llerena"},{"first_name":"L.","full_name":"Pentericci, L.","last_name":"Pentericci"},{"first_name":"L.","full_name":"Napolitano, L.","last_name":"Napolitano"},{"full_name":"Mascia, Sara","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia"},{"last_name":"Amorín","full_name":"Amorín, R.","first_name":"R."},{"last_name":"Calabrò","full_name":"Calabrò, A.","first_name":"A."},{"full_name":"Castellano, M.","first_name":"M.","last_name":"Castellano"},{"last_name":"Cleri","full_name":"Cleri, N. J.","first_name":"N. J."},{"full_name":"Giavalisco, M.","first_name":"M.","last_name":"Giavalisco"},{"last_name":"Grogin","first_name":"N. A.","full_name":"Grogin, N. A."},{"last_name":"Hathi","full_name":"Hathi, N. P.","first_name":"N. P."},{"full_name":"Hirschmann, M.","first_name":"M.","last_name":"Hirschmann"},{"first_name":"A. M.","full_name":"Koekemoer, A. M.","last_name":"Koekemoer"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, T.","first_name":"T."},{"last_name":"Pacucci","first_name":"F.","full_name":"Pacucci, F."},{"last_name":"Shen","full_name":"Shen, L.","first_name":"L."},{"first_name":"S. M.","full_name":"Wilkins, S. M.","last_name":"Wilkins"},{"last_name":"Yoon","first_name":"I.","full_name":"Yoon, I."},{"last_name":"Yung","full_name":"Yung, L. Y.A.","first_name":"L. Y.A."},{"full_name":"Bhatawdekar, R.","first_name":"R.","last_name":"Bhatawdekar"},{"full_name":"Lucas, R. A.","first_name":"R. A.","last_name":"Lucas"},{"last_name":"Wang","full_name":"Wang, X.","first_name":"X."},{"last_name":"Arrabal Haro","full_name":"Arrabal Haro, P.","first_name":"P."},{"last_name":"Bagley","first_name":"M. B.","full_name":"Bagley, M. B."},{"last_name":"Finkelstein","first_name":"S. L.","full_name":"Finkelstein, S. L."},{"last_name":"Kartaltepe","full_name":"Kartaltepe, J. S.","first_name":"J. S."},{"last_name":"Merlin","full_name":"Merlin, E.","first_name":"E."},{"last_name":"Papovich","first_name":"C.","full_name":"Papovich, C."},{"last_name":"Pirzkal","first_name":"N.","full_name":"Pirzkal, N."},{"last_name":"Santini","first_name":"P.","full_name":"Santini, P."}],"doi":"10.1051/0004-6361/202453251","article_number":"A302","file":[{"relation":"main_file","date_updated":"2025-07-08T06:17:02Z","date_created":"2025-07-08T06:17:02Z","access_level":"open_access","checksum":"92745034d9448d38b6b0394407ae39a0","creator":"dernst","file_id":"19974","file_name":"2025_AstronomyAstrophysics_Llerena.pdf","content_type":"application/pdf","success":1,"file_size":7557993}],"acknowledgement":"We thank the anonymous referee for the detailed review and useful suggestions that helped to improve this paper. We wish to thank all our colleagues in the CEERS collaboration for their hard work and valuable contributions to this project. We thank Pietro Bergamini for providing us with the magnification factors for the lensed sources. MLl acknowledges support from the INAF Large Grant 2022 “Extragalactic Surveys with JWST” (PI L. Pentericci), the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and INAF Mini-grant “Galaxies in the epoch of Reionization and their analogs at lower redshift” (PI M. Llerena). 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 This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope (JWST). The JWST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed are associated with program JWST-GO-3073 and can be accessed via DOI. We acknowledge support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift Galaxies”. This work has made extensive use of Python packages astropy (Astropy Collaboration 2018), numpy (Harris et al. 2020), Matplotlib (Hunter 2007) and LiMe (Fernández et al. 2024).","publication_status":"published","volume":698,"type":"journal_article","arxiv":1,"month":"06"}]