[{"arxiv":1,"date_updated":"2026-06-16T10:47:41Z","PlanS_conform":"1","article_processing_charge":"No","day":"30","publication_status":"published","publication_identifier":{"eissn":["2565-6120"]},"year":"2026","_id":"21342","abstract":[{"lang":"eng","text":"JWST has revealed a stunning population of bright galaxies at surprisingly early epochs, z > 10,\r\nwhere few such sources were expected. Here we present the most distant example of this class yet – MoM-z14, a luminous (MUV = −20.2) source in the COSMOS legacy field at zspec = 14.44+0.02−0.02 that expands the observational frontier to a mere 280 million years after the Big Bang. The redshift is confirmed with NIRSpec/prism spectroscopy through a sharp Lyman-α break and ≈ 3σ detections of five rest-UV emission lines. The number density of bright zspec ≈ 14 − 15 sources implied by our “Mirage or Miracle” survey spanning ≈ 350 arcmin2 is > 100× larger (182+329 −105×) than pre-JWST consensus models. The high EWs of UV lines (≈15−35˚A) signal a rising star-formation history, with a ≈10× increase in the last 5 Myr (SFR5Myr/SFR50Myr = 9.9 +3.0 −5.8). The source is extremely compact (circularized re = 74+15\r\n−12 pc), and yet elongated (b/a = 0.25+0.11−0.06), suggesting an AGN is not the dominant source of UV light. The steep UV slope (β = −2.5 +0.2 −0.2) implies negligible dust attenuation\r\nand a young stellar population. The absence of a strong damping wing provides tentative evidence that the immediate surroundings of MoM-z14 may be partially ionized at a redshift where virtually every reionization model predicts a ≈ 100% neutral fraction. The nitrogen emission and highly supersolar [N/C]> 1 hint at an abundance pattern similar to local globular clusters that may have once hosted luminous supermassive stars. Since this abundance pattern is also common among the most ancient stars born in the Milky Way, we may be directly witnessing the formation of such stars in dense clusters, connecting galaxy evolution across the entire sweep of cosmic time. "}],"title":"A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST","author":[{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"last_name":"Weibel","full_name":"Weibel, Andrea","first_name":"Andrea"},{"full_name":"Li, Yijia","last_name":"Li","first_name":"Yijia"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Chisholm, John","last_name":"Chisholm","first_name":"John"},{"first_name":"Clara L.","full_name":"Pollock, Clara L.","last_name":"Pollock"},{"full_name":"Heintz, Kasper E.","last_name":"Heintz","first_name":"Kasper E."},{"last_name":"Johnson","full_name":"Johnson, Benjamin D.","first_name":"Benjamin D."},{"full_name":"Shen, Xuejian","last_name":"Shen","first_name":"Xuejian"},{"first_name":"Raphael E.","last_name":"Hviding","full_name":"Hviding, Raphael E."},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"first_name":"Arpita","last_name":"Ganguly","full_name":"Ganguly, Arpita"},{"last_name":"Witten","full_name":"Witten, Callum","first_name":"Callum"},{"full_name":"Atek, Hakim","last_name":"Atek","first_name":"Hakim"},{"first_name":"Sirio","last_name":"Belli","full_name":"Belli, Sirio"},{"first_name":"Sownak","full_name":"Bose, Sownak","last_name":"Bose"},{"last_name":"Bouwens","full_name":"Bouwens, Rychard","first_name":"Rychard"},{"last_name":"Dayal","full_name":"Dayal, Pratika","first_name":"Pratika"},{"last_name":"Decarli","full_name":"Decarli, Roberto","first_name":"Roberto"},{"last_name":"De Graaff","full_name":"De Graaff, Anna","first_name":"Anna"},{"full_name":"Fudamoto, Yoshinobu","last_name":"Fudamoto","first_name":"Yoshinobu"},{"first_name":"Emma","last_name":"Giovinazzo","full_name":"Giovinazzo, Emma"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"first_name":"Garth","full_name":"Illingworth, Garth","last_name":"Illingworth"},{"first_name":"Akio K.","full_name":"Inoue, Akio K.","last_name":"Inoue"},{"first_name":"Sarah G.","last_name":"Kane","full_name":"Kane, Sarah G."},{"last_name":"Labbe","full_name":"Labbe, Ivo","first_name":"Ivo"},{"last_name":"Leonova","full_name":"Leonova, Ecaterina","first_name":"Ecaterina"},{"last_name":"Marques-Chaves","full_name":"Marques-Chaves, Rui","first_name":"Rui"},{"full_name":"Meyer, Romain A.","last_name":"Meyer","first_name":"Romain A."},{"first_name":"Erica J.","last_name":"Nelson","full_name":"Nelson, Erica J."},{"full_name":"Roberts-Borsani, Guido","last_name":"Roberts-Borsani","first_name":"Guido"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Mauro","full_name":"Stefanon, Mauro","last_name":"Stefanon"},{"first_name":"Yuma","last_name":"Sugahara","full_name":"Sugahara, Yuma"},{"full_name":"Toft, Sune","last_name":"Toft","first_name":"Sune"},{"first_name":"Arjen","full_name":"Van Der Wel, Arjen","last_name":"Van Der Wel"},{"first_name":"Pieter","full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum"},{"last_name":"Walter","full_name":"Walter, Fabian","first_name":"Fabian"},{"last_name":"Watson","full_name":"Watson, Darach","first_name":"Darach"},{"last_name":"Weaver","full_name":"Weaver, John R.","first_name":"John R."},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."}],"publication":"The Open Journal of Astrophysics","article_type":"original","citation":{"ista":"Naidu RP, Oesch PA, Brammer G, Weibel A, Li Y, Matthee JJ, Chisholm J, Pollock CL, Heintz KE, Johnson BD, Shen X, Hviding RE, Leja J, Tacchella S, Ganguly A, Witten C, Atek H, Belli S, Bose S, Bouwens R, Dayal P, Decarli R, De Graaff A, Fudamoto Y, Giovinazzo E, Greene JE, Illingworth G, Inoue AK, Kane SG, Labbe I, Leonova E, Marques-Chaves R, Meyer RA, Nelson EJ, Roberts-Borsani G, Schaerer D, Simcoe RA, Stefanon M, Sugahara Y, Toft S, Van Der Wel A, Van Dokkum P, Walter F, Watson D, Weaver JR, Whitaker KE. 2026. A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. The Open Journal of Astrophysics. 9.","apa":"Naidu, R. P., Oesch, P. A., Brammer, G., Weibel, A., Li, Y., Matthee, J. J., … Whitaker, K. E. (2026). A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.156033\">https://doi.org/10.33232/001c.156033</a>","ama":"Naidu RP, Oesch PA, Brammer G, et al. A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.156033\">10.33232/001c.156033</a>","mla":"Naidu, Rohan P., et al. “A Cosmic Miracle: A Remarkably Luminous Galaxy at Zspec = 14.44 Confirmed with JWST.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.156033\">10.33232/001c.156033</a>.","ieee":"R. P. Naidu <i>et al.</i>, “A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026.","short":"R.P. Naidu, P.A. Oesch, G. Brammer, A. Weibel, Y. Li, J.J. Matthee, J. Chisholm, C.L. Pollock, K.E. Heintz, B.D. Johnson, X. Shen, R.E. Hviding, J. Leja, S. Tacchella, A. Ganguly, C. Witten, H. Atek, S. Belli, S. Bose, R. Bouwens, P. Dayal, R. Decarli, A. De Graaff, Y. Fudamoto, E. Giovinazzo, J.E. Greene, G. Illingworth, A.K. Inoue, S.G. Kane, I. Labbe, E. Leonova, R. Marques-Chaves, R.A. Meyer, E.J. Nelson, G. Roberts-Borsani, D. Schaerer, R.A. Simcoe, M. Stefanon, Y. Sugahara, S. Toft, A. Van Der Wel, P. Van Dokkum, F. Walter, D. Watson, J.R. Weaver, K.E. Whitaker, The Open Journal of Astrophysics 9 (2026).","chicago":"Naidu, Rohan P., Pascal A. Oesch, Gabriel Brammer, Andrea Weibel, Yijia Li, Jorryt J Matthee, John Chisholm, et al. “A Cosmic Miracle: A Remarkably Luminous Galaxy at Zspec = 14.44 Confirmed with JWST.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.156033\">https://doi.org/10.33232/001c.156033</a>."},"oa":1,"fulldoi":"https://doi.org/10.33232/001c.156033","acknowledgement":"We thank the two anonymous referees for their insightful comments that have strengthened this work. “Mirage or Miracle” is but the latest link in a long chain of surveys that have built COSMOS into a premier extragalactic legacy field. We are thankful to all the teams who have contributed to this legacy, particularly those mentioned in §3 for leading recent JWST programs whose imaging\r\nwe have incorporated in our analysis. We are grateful to Vasily Belokurov for help in compiling the Milky Way reference sample featured in Fig 8. We thank Danielle Berg for sharing a highly complete, highly decimalized NUV vacuum line list. We are grateful to our program’s NIRSpec reviewer, Dan Coe, and program coordinator, Allison Vick, for valuable input on our MSA design. We acknowledge illuminating conversations with Risa Wechsler and Chao-Lin Kuo about early reionization. RPN thanks Neil Pappalardo and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships in Physics, and for their enthusiasm and encouragement for seeking galaxies at the highest redshifts. RPN acknowledges funding from JWST program GO5224. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. 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. Funded by the European Union (ERC, AGENTS, 101076224 and HEAVYMETAL, 101071865). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of\r\nthe European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. This work has also been supported by JSPS KAKENHI Grant Number 23H00131. HA acknowledges support from CNES, focused on the JWST mission, and the Programme National Cosmology and Galaxies (PNCG)\r\nof CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. HA is supported by the French National Research Agency (ANR) under the project FIRSTGAL, grant number ANR-24-CE31-0838. SB is supported by the UK Research and Innovation (UKRI) Future Leaders Fellowship [grant number MR/V023381/1]. R.D. acknowledges support from the INAF GO 2022\r\ngrant “The birth of the giants: JWST sheds light on the build-up of quasars at cosmic dawn” and by the PRIN MUR “2022935STW”, RFF M4.C2.1.1, CUP J53D23001570006 and C53D23000950006. Computations supporting this paper were run on MIT’s Engaging cluster. This publication made use of the NASA Astrophysical Data System for bibliographic information. Some of the data products presented herein 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. Software used in developing this work includes: matplotlib (Hunter 2007), jupyter (Kluyver et al. 2016), IPython (P´erez & Granger 2007), numpy (Oliphant 2015), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy Collaboration et al. 2013).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\r\nTelescopes 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 # 5224.","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-02-22T23:01:35Z","publisher":"Maynooth Academic Publishing","doi":"10.33232/001c.156033","scopus_import":"1","status":"public","has_accepted_license":"1","department":[{"_id":"JoMa"}],"OA_place":"publisher","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2505.11263"]},"volume":9,"oa_version":"Published Version","type":"journal_article","date_published":"2026-01-30T00:00:00Z","intvolume":"         9","OA_type":"diamond","ddc":["520"],"main_file_link":[{"url":"https://doi.org/10.33232/001c.156033","open_access":"1"}],"quality_controlled":"1","month":"01"},{"volume":9,"external_id":{"arxiv":["2512.08490"]},"language":[{"iso":"eng"}],"oa_version":"Published Version","intvolume":"         9","type":"journal_article","date_published":"2026-04-09T00:00:00Z","ddc":["520"],"OA_type":"diamond","file":[{"date_updated":"2026-06-02T06:38:59Z","file_name":"2026_OpenJourAstrophysics_Castellano.pdf","content_type":"application/pdf","creator":"dernst","checksum":"ec33ca56b8836c61cb01e26893d43cbf","file_size":4855934,"relation":"main_file","access_level":"open_access","file_id":"21935","success":1,"date_created":"2026-06-02T06:38:59Z"}],"quality_controlled":"1","month":"04","doi":"10.33232/001c.160281","scopus_import":"1","status":"public","has_accepted_license":"1","OA_place":"publisher","department":[{"_id":"JoMa"}],"article_type":"original","citation":{"short":"M. Castellano, L. Napolitano, B. Moreschini, A. Calabrò, L. Christensen, M. Llerena, T.J.L.C. Bakx, F. Belfiore, D. Bevacqua, M. Dickinson, A. Fontana, G. Gandolfi, T. Gasparetto, A. Marconi, S. Mascia, E. Merlin, T. Morishita, T. Nanayakkara, D. Paris, L. Pentericci, B. Pérez-Díaz, G. Roberts-Borsani, S. Rojas-Ruiz, P. Santini, T. Treu, E. Vanzella, B. Vulcani, X. Wang, I. Yoon, J. Zavala, The Open Journal of Astrophysics 9 (2026).","chicago":"Castellano, M., L. Napolitano, B. Moreschini, A. Calabrò, L. Christensen, M. Llerena, T. J.L.C. Bakx, et al. “Investigating Ionising Sources and the Complex Interstellar Medium of GHZ2 at Z=12.3.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.160281\">https://doi.org/10.33232/001c.160281</a>.","ieee":"M. Castellano <i>et al.</i>, “Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026.","mla":"Castellano, M., et al. “Investigating Ionising Sources and the Complex Interstellar Medium of GHZ2 at Z=12.3.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.160281\">10.33232/001c.160281</a>.","ama":"Castellano M, Napolitano L, Moreschini B, et al. Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.160281\">10.33232/001c.160281</a>","apa":"Castellano, M., Napolitano, L., Moreschini, B., Calabrò, A., Christensen, L., Llerena, M., … Zavala, J. (2026). Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.160281\">https://doi.org/10.33232/001c.160281</a>","ista":"Castellano M, Napolitano L, Moreschini B, Calabrò A, Christensen L, Llerena M, Bakx TJLC, Belfiore F, Bevacqua D, Dickinson M, Fontana A, Gandolfi G, Gasparetto T, Marconi A, Mascia S, Merlin E, Morishita T, Nanayakkara T, Paris D, Pentericci L, Pérez-Díaz B, Roberts-Borsani G, Rojas-Ruiz S, Santini P, Treu T, Vanzella E, Vulcani B, Wang X, Yoon I, Zavala J. 2026. Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. The Open Journal of Astrophysics. 9."},"file_date_updated":"2026-06-02T06:38:59Z","oa":1,"acknowledgement":"We thank the referee for the constructive comments that\r\nhelped us improve the manuscript. We thank S. Finkelstein,\r\nY. Harikane, C. Mason, and D. Stark for the useful comments.\r\nWe thank Tony Roman (Program Coordinator) and Glenn\r\nWahlgren (NIRSpec reviewer) for the assistance in the\r\npreparation of GO-3073 observations. This work is based\r\non observations made with the NASA/ESA/CSA James\r\nWebb Space Telescope (JWST). The JWST data presented in this article were obtained from the Mikulski Archive for\r\nSpace Telescopes (MAST) at the Space Telescope Science\r\nInstitute. The specific observations analysed are associated with program JWST-GO-3073 and can be accessed\r\nvia https://doi.org/10.17909/4r6b-bx96 (first pointing) and\r\nhttps://doi:10.17909/zq4g-r525 (second pointing). We\r\nacknowledge financial support from NASA through grant\r\nJWST-ERS-1324 and JWST-GO-3073. Support was also\r\nprovided by the PRIN 2022 MUR project 2022CB3PJ3 –\r\nFirst Light And Galaxy aSsembly (FLAGS) funded by the\r\nEuropean Union – Next Generation EU, by INAF GO Grant\r\n2024 ”Revealing the nature of bright galaxies at cosmic\r\ndawn with deep JWST spectroscopy”, by INAF Mini-grant\r\n2022 “Reionization and Fundamental Cosmology with\r\nHigh-Redshift Galaxies”, and by INAF Large Grant 2022\r\n“Extragalactic Surveys with JWST”. L.N. acknowledges\r\nsupport from grant “Progetti per Avvio alla Ricerca - Tipo\r\n1, Unveiling Cosmic Dawn: Galaxy Evolution with CAPERS” (AR1241906F947685). EV acknowledges financial\r\nsupport through grants INAF GO Grant 2024 “Mapping Star\r\nCluster Feedback in a Galaxy 450 Myr after the Big Bang”\r\nand by the European Union – NextGenerationEU within\r\nPRIN 2022 project n.20229YBSAN - Globular clusters\r\nin cosmological simulations and lensed fields: from their\r\nbirth to the present epoch. AM acknowledges support\r\nfrom project PRIN-MUR project “PROMETEUS” financed\r\nby the European Union - Next Generation EU, Mission 4\r\nComponent 1 CUP B53D2300475000. AM acknowledges\r\nsupport from Ricerca Fondamentale INAF under Mini Grant\r\n2023 ”Quantitative Spectroscopy of Ionized Nebulae and\r\nGalaxies (QSING)” and under Data Analysis Grant 2024\r\n“Accurate measurements of metallicity in galaxies with a new\r\napproach to photoionization modelling”.","fulldoi":"https://doi.org/10.33232/001c.160281","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Maynooth Academic Publishing","DOAJ_listed":"1","date_created":"2026-05-31T22:02:14Z","arxiv":1,"date_updated":"2026-06-02T06:39:53Z","publication_status":"published","PlanS_conform":"1","day":"09","article_processing_charge":"No","publication_identifier":{"eissn":["2565-6120"]},"year":"2026","_id":"21934","abstract":[{"text":"An accurate characterisation of the physical properties of galaxies at cosmic dawn is key to understanding\r\nthe origin of the high abundance of UV-bright galaxies at z≳10. We exploit deep (9.1-hour exposure time)\r\nNIRSpec PRISM observations of GHZ2 to constrain the sources of ionising radiation and the properties of the\r\ninterstellar medium (ISM) in this bright, compact, and highly ionising galaxy at z=12.3. We measure with\r\nhigh significance the prominent N IV, C IV, He II, O III, C III, O II, and Ne III emission features previously\r\ndetected in shallower observations, and confirm the detection of the N III] λ1750 multiplet, yielding tight\r\nconstraints on the N/O ratio, which is found to be ≃2 times the solar value. We also detect the Mg II λ2800,\r\n[Fe IV] λ2833 and Si II λ1812 doublets, the H8+HeI λλ3889 blend, and the Si IV+O IV] λλ1400 absorption\r\ncomplex. The O III λ3133 fluorescence line is only detected in the first observing epoch, implying variability\r\non a rest-frame time span of 19 days, strongly suggesting the presence of an active nucleus. Combining the\r\nNIRSpec dataset with available optical and far-infrared constraints from MIRI and ALMA, we show that the\r\nemission spectrum of GHZ2 cannot be reproduced by single-density spectro-photometric models, even under\r\nextreme assumptions on the ionisation parameter and electron density. Multi-zone photoionisation modelling\r\nperformed with the HOMERUN code demonstrates that star formation must be occurring in a strongly stratified\r\nISM, where both low-/intermediate-density gas and high-density regions (log(ne/cm−3\r\n) ≳ 4) coexist. The\r\nGHZ2 emission landscape is consistent with either a composite star-formation plus AGN scenario, or with\r\nstar formation occurring in a combination of radiation- and matter-bounded regions. Purely radiation-bounded\r\nstellar models fail to reproduce the observed He II emission, making an additional hard ionising component\r\nunavoidable.","lang":"eng"}],"publication":"The Open Journal of Astrophysics","title":"Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3","author":[{"last_name":"Castellano","full_name":"Castellano, M.","first_name":"M."},{"first_name":"L.","last_name":"Napolitano","full_name":"Napolitano, L."},{"last_name":"Moreschini","full_name":"Moreschini, B.","first_name":"B."},{"last_name":"Calabrò","full_name":"Calabrò, A.","first_name":"A."},{"full_name":"Christensen, L.","last_name":"Christensen","first_name":"L."},{"first_name":"M.","last_name":"Llerena","full_name":"Llerena, M."},{"full_name":"Bakx, T. J.L.C.","last_name":"Bakx","first_name":"T. J.L.C."},{"last_name":"Belfiore","full_name":"Belfiore, F.","first_name":"F."},{"first_name":"D.","full_name":"Bevacqua, D.","last_name":"Bevacqua"},{"full_name":"Dickinson, M.","last_name":"Dickinson","first_name":"M."},{"last_name":"Fontana","full_name":"Fontana, A.","first_name":"A."},{"last_name":"Gandolfi","full_name":"Gandolfi, G.","first_name":"G."},{"first_name":"T.","full_name":"Gasparetto, T.","last_name":"Gasparetto"},{"first_name":"A.","full_name":"Marconi, A.","last_name":"Marconi"},{"first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia"},{"full_name":"Merlin, E.","last_name":"Merlin","first_name":"E."},{"full_name":"Morishita, T.","last_name":"Morishita","first_name":"T."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"last_name":"Paris","full_name":"Paris, D.","first_name":"D."},{"full_name":"Pentericci, L.","last_name":"Pentericci","first_name":"L."},{"first_name":"B.","full_name":"Pérez-Díaz, B.","last_name":"Pérez-Díaz"},{"last_name":"Roberts-Borsani","full_name":"Roberts-Borsani, G.","first_name":"G."},{"first_name":"S.","last_name":"Rojas-Ruiz","full_name":"Rojas-Ruiz, S."},{"last_name":"Santini","full_name":"Santini, P.","first_name":"P."},{"first_name":"T.","last_name":"Treu","full_name":"Treu, T."},{"first_name":"E.","last_name":"Vanzella","full_name":"Vanzella, E."},{"first_name":"B.","full_name":"Vulcani, B.","last_name":"Vulcani"},{"last_name":"Wang","full_name":"Wang, X.","first_name":"X."},{"first_name":"I.","full_name":"Yoon, I.","last_name":"Yoon"},{"full_name":"Zavala, J.","last_name":"Zavala","first_name":"J."}]},{"has_accepted_license":"1","status":"public","department":[{"_id":"JoMa"}],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"OA_place":"publisher","scopus_import":"1","doi":"10.33232/001c.162505","month":"05","file":[{"file_name":"2026_OpenJourAstrophysics_Sun.pdf","date_updated":"2026-06-08T08:23:37Z","creator":"dernst","checksum":"33c4a444f7c37b3f47ecbd53eb187c1b","content_type":"application/pdf","relation":"main_file","file_size":7591188,"date_created":"2026-06-08T08:23:37Z","access_level":"open_access","file_id":"21952","success":1}],"ddc":["520"],"OA_type":"diamond","quality_controlled":"1","oa_version":"Published Version","type":"journal_article","date_published":"2026-05-25T00:00:00Z","intvolume":"         9","language":[{"iso":"eng"}],"external_id":{"arxiv":["2601.20929"]},"volume":9,"abstract":[{"lang":"eng","text":"The central engines of Little Red Dots (LRDs) may be “black hole stars” (BH*s), early stages of\r\nblack hole growth characterized by dense gas envelopes. So far, the most direct evidence for BH*s\r\ncomes from a handful of sources where the host galaxy is completely outshone as suggested by their\r\nremarkably steep Balmer breaks. Here we present a novel scheme to disentangle BH*s from their\r\nhost galaxies assuming that the [O III]5008˚A line arises exclusively from the host. Using a sample\r\nof 98 LRDs (z ≈ 2 − 9) with high quality NIRSpec/PRISM spectra, we demonstrate that the hostsubtracted median stack displays a Balmer break > 2× stronger than massive quiescent galaxies,\r\nwith the rest-optical continuum resembling a blackbody-like SED (Teff ≈ 4050 K, log(Lbol) ≈ 43.9\r\nerg s−1\r\n, Reff ≈ 1300 au). We measure a steep Balmer decrement (Hα/Hβ > 10) and numerous\r\ndensity-sensitive features (e.g., Fe II, He I, O I). These are hallmark signatures of dense gas envelopes,\r\nproviding population-level evidence that BH*s indeed power LRDs. In the median LRD, BH*s account\r\nfor ∼ 20% of the UV emission, ∼ 50% at the Balmer break, and ∼ 90% at wavelengths longer\r\nthan Hα with the remainder arising from the host. BH*s preferentially reside in low-mass galaxies\r\n(M⋆ ≈ 108 M⊙) undergoing recent starbursts, as evidenced by extreme emission line EWs (e.g.,\r\n[O III]5008˚A≈ 1100˚A, C III]≈ 12˚A), thereby favoring BH* origins linked to star-formation. We show\r\nV-shaped LRD selections are biased to high BH*/host fractions (≳ 60% at 5500˚A) – less dominant\r\nBH*s may be powering JWST’s blue broad-line AGN. We find BH*s are so commonplace and transient\r\n(duty cycle ∼ 1%, lifetime ∼ 10 Myrs) that every massive black hole may have once shone as a BH*.\r\n"}],"publication":"The Open Journal of Astrophysics","title":"Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot","author":[{"full_name":"Sun, Wendy Q.","last_name":"Sun","first_name":"Wendy Q."},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"De Graaff, Anna","last_name":"De Graaff","first_name":"Anna"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa"},{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Simcoe, Robert A.","last_name":"Simcoe","first_name":"Robert A."},{"last_name":"Bose","full_name":"Bose, Sownak","first_name":"Sownak"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"full_name":"Dayal, Pratika","last_name":"Dayal","first_name":"Pratika"},{"first_name":"Anna Christina","full_name":"Eilers, Anna Christina","last_name":"Eilers"},{"full_name":"Fei, Qinyue","last_name":"Fei","first_name":"Qinyue"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"first_name":"Rashmi","full_name":"Gottumukkala, Rashmi","last_name":"Gottumukkala"},{"last_name":"Goulding","full_name":"Goulding, Andy","first_name":"Andy"},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"last_name":"Hirschmann","full_name":"Hirschmann, Michaela","first_name":"Michaela"},{"first_name":"Vasily","last_name":"Kokorev","full_name":"Kokorev, Vasily"},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"first_name":"Zhaoran","full_name":"Liu, Zhaoran","last_name":"Liu"},{"first_name":"Priyamvada","last_name":"Natarajan","full_name":"Natarajan, Priyamvada"},{"last_name":"Santarelli","full_name":"Santarelli, Andrew D.","first_name":"Andrew D."},{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"first_name":"Aaron","last_name":"Smith","full_name":"Smith, Aaron"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"last_name":"Volonteri","full_name":"Volonteri, Marta","first_name":"Marta"},{"first_name":"Fabian","full_name":"Walter, Fabian","last_name":"Walter"},{"first_name":"Andrea","full_name":"Weibel, Andrea","last_name":"Weibel"},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}],"publication_identifier":{"eissn":["2565-6120"]},"_id":"21951","year":"2026","article_processing_charge":"No","PlanS_conform":"1","day":"25","publication_status":"published","date_updated":"2026-06-08T08:25:40Z","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-06-07T22:01:36Z","publisher":"Maynooth Academic Publishing","DOAJ_listed":"1","acknowledgement":"We thank the two anonymous referees for their insightful comments that have strengthened this work.\r\nWQS and RPN acknowledge funding from JWST programs GO-3516, GO-5224, and the MIT Undergraduate\r\nResearch Opportunities Program (UROP). Support for\r\nthis work was provided by NASA through the NASA\r\nHubble Fellowship grant HST-HF2-51515.001-A awarded\r\nby the Space Telescope Science Institute, which is operated by the Association of Universities for Research in\r\nAstronomy, Incorporated, under NASA contract NAS5-\r\n26555. RPN thanks Neil Pappalardo and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships in Physics, and for their enthusiasm\r\nand encouragement for pursuing the earliest galaxies and\r\nblack holes. JM and AT acknowledge funding from the\r\nEuropean Union (ERC, AGENTS, 101076224). KEH\r\nacknowledges support from the Independent Research Fund Denmark (DFF) under grant 5251-00009B and cofunding by the European Union (ERC, HEAVYMETAL,\r\n101071865). Views and opinions expressed are, however,\r\nthose of the authors only and do not necessarily reflect\r\nthose of the European Union or the European Research\r\nCouncil. Neither the European Union nor the granting\r\nauthority can be held responsible for them. REH acknowledges support by the German Aerospace Center\r\n(DLR) and the Federal Ministry for Economic Affairs\r\nand Energy (BMWi) through program 50OR2403 ‘RUBIES’.\r\nThe data products presented herein were retrieved\r\nfrom the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is\r\nfunded by the Danish National Research Foundation under grant DNRF140. This work is based on observations\r\nmade with the NASA/ESA/CSA James Webb Space\r\nTelescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope\r\nScience Institute, which is operated by the Association\r\nof Universities for Research in Astronomy, Inc., under\r\nNASA contract NAS 5-03127 for JWST. Support for\r\nprograms #3516, #5224, #5664 was provided by NASA\r\nthrough grants from the Space Telescope Science Institute, which is operated by the Association of Universities\r\nfor Research in Astronomy, Inc., under NASA contract\r\nNAS 5-03127.\r\nThe spectra used in this paper are associated with programs 1180 (D’Eugenio et al. 2025d), 1181 (PI: D. Eisenstein), 1208 (Willott et al. 2022), 1210 (PI: N. Luetzgendorf), 1211 (Maseda et al. 2024), 1212 - 1215 (PI: N.\r\nLuetzgendorf), 1228 (Luhman et al. 2024b), 1229 (Luhman et al. 2024a), 1286 (PI: N. Luetzgendorf), 1287 (PI:\r\nK. Isaak), 1345 (Finkelstein et al. 2023), 1433 (Hsiao\r\net al. 2024), 1747 (PI: G. Roberts-Borsani), 2028 (Wang\r\net al. 2024c), 2073 (PI: J. Hennawi), 2198 (Barrufet\r\net al. 2025), 2282 (Bradley et al. 2023), 2561 (Bezanson\r\net al. 2024), 2565 (Nanayakkara et al. 2025), 2640 (PI:\r\nW. Best), 2750 (Arrabal Haro et al. 2023), 2756 (Mascia et al. 2024), 2767 (Williams et al. 2023b), 2770 (PI:\r\nM. McCaughrean), 3073 (Castellano et al. 2024), 3215\r\n(Eisenstein et al. 2025), 4106 (PI: E. Nelson), 4233 (de\r\nGraaff et al. 2025c), 4446 (Frye et al. 2024), 4557 (PI: H.\r\nYan), 5105 (Shen et al. 2024), 5224 (PIs: P.A. Oesch &\r\nR.P. Naidu), 6368 (PI: M. Dickinson), 6541 (DeCoursey\r\net al. 2025), 6585 (PI: D. Coulter), 6642 (PI: J. Muzerolle\r\nPage), and FRESCO IFU (Matthee et al. 2024; Torralba\r\net al. 2025b).\r\nSoftware used in developing this work includes:\r\nmatplotlib (Hunter 2007), jupyter (Kluyver et al.\r\n2016), IPython (P´erez & Granger 2007), numpy\r\n(Oliphant 2015), scipy (Virtanen et al. 2020), TOPCAT\r\n(Taylor 2005), Astropy (Astropy Collaboration et al.\r\n2013), msaexp (Brammer 2023).","fulldoi":"https://doi.org/10.33232/001c.162505","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file_date_updated":"2026-06-08T08:23:37Z","citation":{"chicago":"Sun, Wendy Q., Rohan P. Naidu, Jorryt J Matthee, Anna De Graaff, John Chisholm, Jenny E. Greene, Pascal A. Oesch, et al. “Little Red Dot - Host Galaxy = Black Hole Star: A Gas-Enshrouded Heart at the Center of Every Little Red Dot.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.162505\">https://doi.org/10.33232/001c.162505</a>.","short":"W.Q. Sun, R.P. Naidu, J.J. Matthee, A. De Graaff, J. Chisholm, J.E. Greene, P.A. Oesch, A. Torralba Torregrosa, R.E. Hviding, G. Brammer, R.A. Simcoe, S. Bose, R. Bouwens, P. Dayal, A.C. Eilers, Q. Fei, L.J. Furtak, R. Gottumukkala, A. Goulding, K.E. Heintz, M. Hirschmann, V. Kokorev, J. Leja, Z. Liu, P. Natarajan, A.D. Santarelli, D.J. Setton, A. Smith, S. Tacchella, M. Volonteri, F. Walter, A. Weibel, C.C. Williams, The Open Journal of Astrophysics 9 (2026).","apa":"Sun, W. Q., Naidu, R. P., Matthee, J. J., De Graaff, A., Chisholm, J., Greene, J. E., … Williams, C. C. (2026). Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.162505\">https://doi.org/10.33232/001c.162505</a>","ama":"Sun WQ, Naidu RP, Matthee JJ, et al. Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.162505\">10.33232/001c.162505</a>","mla":"Sun, Wendy Q., et al. “Little Red Dot - Host Galaxy = Black Hole Star: A Gas-Enshrouded Heart at the Center of Every Little Red Dot.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.162505\">10.33232/001c.162505</a>.","ista":"Sun WQ, Naidu RP, Matthee JJ, De Graaff A, Chisholm J, Greene JE, Oesch PA, Torralba Torregrosa A, Hviding RE, Brammer G, Simcoe RA, Bose S, Bouwens R, Dayal P, Eilers AC, Fei Q, Furtak LJ, Gottumukkala R, Goulding A, Heintz KE, Hirschmann M, Kokorev V, Leja J, Liu Z, Natarajan P, Santarelli AD, Setton DJ, Smith A, Tacchella S, Volonteri M, Walter F, Weibel A, Williams CC. 2026. Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. The Open Journal of Astrophysics. 9.","ieee":"W. Q. Sun <i>et al.</i>, “Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026."},"oa":1,"article_type":"original"},{"date_updated":"2026-07-13T09:09:34Z","arxiv":1,"PlanS_conform":"1","article_processing_charge":"No","day":"30","publication_status":"published","publication_identifier":{"eissn":["2565-6120"]},"_id":"22270","year":"2026","abstract":[{"lang":"eng","text":"The explosion of a white dwarf (WD) in a close binary can launch a surviving runaway star at\r\nvelocities of ≳ 1000 km s−1\r\n. Such runaways provide a direct probe of thermonuclear supernovae (SNe)\r\nin double-degenerate binaries. Several candidate runaways are known, but their evolutionary states\r\nand the demographics of the broader population are uncertain. To enable robust population inference,\r\nwe carry out a systematic survey for hypervelocity runaways with a simple selection function, selecting\r\ncandidates based on large Gaia-inferred tangential velocities and blue colors. We classify 100% of the\r\nresulting 92 candidates using a combination of spectroscopic follow-up and archival data. The search\r\nyields ten suspected D6\r\nstars and three LP 40-365 stars. Three D6\r\nstars are new discoveries, including\r\ntwo hot (Teff ≳ 50,000 K) objects and one cool (Teff ≈ 7,000 K) object. We forward-model our survey\r\nunder several proposed D6\r\nstar evolutionary models, coupling each to a Galactic model and the survey\r\nselection function. No single model reproduces the observed diversity of D6\r\nstars, which likely reflects\r\na range of remnant masses, ages, and heating mechanisms. Models in which runaway companions\r\nare heated by SN shocks alone are too faint and short-lived to explain most of the observed sample,\r\nwhile fully reheated models are too luminous and long-lived. Models with intermediate heating,\r\nas occurs in some simulations of violent mergers and partially disrupted remnants, best match the\r\nobserved magnitude, distance, and kinematic-age distributions. The inferred D6\r\nstar birth rate is\r\nmodel dependent, but the models that best match the observed population require rates of only a\r\nfew percent of the Galactic SN Ia rate, perhaps implying that most SNe Ia result from WD binaries\r\nin which both components explode. If most SNe Ia do produce surviving runaways, these must be\r\nfainter or shorter-lived than the currently known runaways."}],"publication":"The Open Journal of Astrophysics","author":[{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Werner","full_name":"Werner, Klaus","first_name":"Klaus"},{"last_name":"Shen","full_name":"Shen, Ken J.","first_name":"Ken J."},{"first_name":"Jay","full_name":"Strader, Jay","last_name":"Strader"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"first_name":"Jiwon Jesse","last_name":"Han","full_name":"Han, Jiwon Jesse"},{"first_name":"Vedant","last_name":"Chandra","full_name":"Chandra, Vedant"},{"full_name":"Chomiuk, Laura","last_name":"Chomiuk","first_name":"Laura"},{"full_name":"Vanderbosch, Zachary P.","last_name":"Vanderbosch","first_name":"Zachary P."},{"first_name":"Lisa","full_name":"Blomberg, Lisa","last_name":"Blomberg"},{"last_name":"Yamaguchi","full_name":"Yamaguchi, Natsuko","first_name":"Natsuko"},{"last_name":"Nagarajan","full_name":"Nagarajan, Pranav","first_name":"Pranav"},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"full_name":"van Roestel, Joannes C","last_name":"van Roestel","first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333"},{"last_name":"Glanz","full_name":"Glanz, Hila","first_name":"Hila"},{"first_name":"Tin Long Sunny","full_name":"Wong, Tin Long Sunny","last_name":"Wong"},{"full_name":"Bhat, Aakash","last_name":"Bhat","first_name":"Aakash"},{"full_name":"Hollands, Mark A.","last_name":"Hollands","first_name":"Mark A."}],"title":"A systematic survey for hypervelocity runaways from thermonuclear supernovae","article_type":"original","das_tickbox":"1","file_date_updated":"2026-07-13T09:05:36Z","supplementarymaterial":"no","citation":{"chicago":"El-Badry, Kareem, Klaus Werner, Ken J. Shen, Jay Strader, Antonio C. Rodriguez, Jiwon Jesse Han, Vedant Chandra, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.164326\">https://doi.org/10.33232/001c.164326</a>.","short":"K. El-Badry, K. Werner, K.J. Shen, J. Strader, A.C. Rodriguez, J.J. Han, V. Chandra, L. Chomiuk, Z.P. Vanderbosch, L. Blomberg, N. Yamaguchi, P. Nagarajan, I. Caiazzo, J.C. van Roestel, H. Glanz, T.L.S. Wong, A. Bhat, M.A. Hollands, The Open Journal of Astrophysics 9 (2026).","ista":"El-Badry K, Werner K, Shen KJ, Strader J, Rodriguez AC, Han JJ, Chandra V, Chomiuk L, Vanderbosch ZP, Blomberg L, Yamaguchi N, Nagarajan P, Caiazzo I, van Roestel JC, Glanz H, Wong TLS, Bhat A, Hollands MA. 2026. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 9.","apa":"El-Badry, K., Werner, K., Shen, K. J., Strader, J., Rodriguez, A. C., Han, J. J., … Hollands, M. A. (2026). A systematic survey for hypervelocity runaways from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.164326\">https://doi.org/10.33232/001c.164326</a>","mla":"El-Badry, Kareem, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.164326\">10.33232/001c.164326</a>.","ama":"El-Badry K, Werner K, Shen KJ, et al. A systematic survey for hypervelocity runaways from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.164326\">10.33232/001c.164326</a>","ieee":"K. El-Badry <i>et al.</i>, “A systematic survey for hypervelocity runaways from thermonuclear supernovae,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026."},"researchdata_availability":"no","oa":1,"fulldoi":"https://doi.org/10.33232/001c.164326","acknowledgement":"We thank Lars Bildsten, Evan Bauer, Ruediger Pakmor, Jim Fuller, Logan Proust, Abinaya Rajamuthukumar, and Stephan Geier for useful discussion related to\r\nthis work.\r\nThis work was supported by NSF grants AST-2508988\r\nand AST-2205631, NASA/ESA Hubble Space Telescope\r\nprogram No. 17441, and Scialog grant #SA-LSST-2024-\r\n114c from the Research Corporation for Science Advancement. The Kavli Institute for Theoretical Physics\r\n(KITP) hosted the program, “White Dwarfs as Probes of\r\nthe Evolution of Planets, Stars, the Milky Way, and the\r\nExpanding Universe,” during which this project was initiated. This research was supported in part by the U.S.\r\nNational Science Foundation (NSF) under grants PHY1748958. This research benefited from discussions that\r\nwere funded by the Gordon and Betty Moore Foundation\r\nthrough Grant GBMF5076.\r\nWe thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the observatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-07-12T22:02:19Z","DOAJ_listed":"1","publisher":"Maynooth Academic Publishing","doi":"10.33232/001c.164326","scopus_import":"1","status":"public","has_accepted_license":"1","department":[{"_id":"IlCa"}],"OA_place":"publisher","keyword":["white dwarfs","binaries: close","stars: chemically peculiar"],"language":[{"iso":"eng"}],"external_id":{"arxiv":["2606.11293"]},"volume":9,"oa_version":"Published Version","type":"journal_article","date_published":"2026-06-30T00:00:00Z","intvolume":"         9","file":[{"date_created":"2026-07-13T09:05:36Z","success":1,"file_id":"22282","access_level":"open_access","relation":"main_file","file_size":1994596,"checksum":"6320fd19e5ea3399f332be5aab022736","creator":"dernst","content_type":"application/pdf","file_name":"2026_OpenJourAstrophysics_ElBadry.pdf","date_updated":"2026-07-13T09:05:36Z"}],"OA_type":"gold","ddc":["520"],"quality_controlled":"1","dataavailabilitystatement":"We thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the\r\nobservatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","month":"06"},{"date_updated":"2026-09-17T08:31:24Z","arxiv":1,"publication_status":"published","article_processing_charge":"No","day":"21","publication_identifier":{"eissn":["2565-6120"]},"_id":"22928","year":"2026","abstract":[{"text":"We present deep ALMA Band 7 observations of the [O iii] 88 µm line and underlying dust continuum\r\nemission in four UV-bright, gravitationally lensed (magnification µ = 1.4 − 3.8), JWST-selected\r\ngalaxies at z = 8.5 − 10.3, with observed magnitudes −22.5 ≲ MUV ≲ −20.5. [O iii] 88 µm is\r\nconfidently detected in UNCOVER-10646 at z = 8.5080 ± 0.0011 (15σ) and DHZ1 at z = 9.3113 ±\r\n0.0006 (6σ), with both being intrinsically luminous systems [L[O iii] = (1.1− 1.6) ×109 L⊙] that follow\r\nthe local [O iii]-SFR relation. [O iii] 88 µm remains undetected in the two z > 10 targets, including in\r\nthe z = 10.07 X-ray AGN UHZ1, where we obtain a deep limit of L[O iii] < 6 × 107 L⊙. Dust emission\r\nis not detected in any individual source nor in a stack (< 3σ). The high S/N [O iii] 88 µm detection\r\nin UNCOVER-10646 uniquely reveals an additional broad component (FWHM = 1366+473\r\n−329 km/s;\r\n∆BIC ≈ 20) indicative of an ionized outflow. We infer a high outflow rate of M˙\r\nout = 128+80\r\n−46 M⊙ yr−1\r\n,\r\ncorresponding to a mass loading factor η = M˙\r\nout/SFR = 2.9\r\n+1.8\r\n−1.0\r\nthat matches or exceeds theoretical\r\npredictions and JWST-based studies of ionized outflows at high redshift. While high-resolution ALMA\r\nfollow-up is required to confirm and spatially resolve the outflow, this first systematic study at z > 8\r\nhighlights the unique diagnostic power of [O iii] 88 µm in characterizing galaxies in the early Universe.","lang":"eng"}],"author":[{"last_name":"Algera","full_name":"Algera, Hiddo S.B.","first_name":"Hiddo S.B."},{"last_name":"Weaver","full_name":"Weaver, John R.","first_name":"John R."},{"last_name":"Bakx","full_name":"Bakx, Tom J.L.C.","first_name":"Tom J.L.C."},{"first_name":"Manuel","full_name":"Aravena, Manuel","last_name":"Aravena"},{"first_name":"Rychard J.","full_name":"Bouwens, Rychard J.","last_name":"Bouwens"},{"full_name":"Cescon, Karin","last_name":"Cescon","first_name":"Karin"},{"first_name":"Chian Chou","full_name":"Chen, Chian Chou","last_name":"Chen"},{"last_name":"Da Cunha","full_name":"Da Cunha, Elisabete","first_name":"Elisabete"},{"first_name":"Pratika","last_name":"Dayal","full_name":"Dayal, Pratika"},{"first_name":"Andreas","full_name":"Faisst, Andreas","last_name":"Faisst"},{"first_name":"Andrea","full_name":"Ferrara, Andrea","last_name":"Ferrara"},{"first_name":"Seiji","full_name":"Fujimoto, Seiji","last_name":"Fujimoto"},{"first_name":"Takuya","full_name":"Hashimoto, Takuya","last_name":"Hashimoto"},{"full_name":"Heintz, Kasper","last_name":"Heintz","first_name":"Kasper"},{"last_name":"Herrera-Camus","full_name":"Herrera-Camus, Rodrigo","first_name":"Rodrigo"},{"first_name":"Jacqueline","last_name":"Hodge","full_name":"Hodge, Jacqueline"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"first_name":"Akio K.","full_name":"Inoue, Akio K.","last_name":"Inoue"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Meyer, Romain","last_name":"Meyer","first_name":"Romain"},{"full_name":"Mizukoshi, Shoichiro","last_name":"Mizukoshi","first_name":"Shoichiro"},{"first_name":"Chayan","last_name":"Mondal","full_name":"Mondal, Chayan"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"first_name":"Andrea","full_name":"Pallottini, Andrea","last_name":"Pallottini"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"full_name":"Rowland, Lucie E.","last_name":"Rowland","first_name":"Lucie E."},{"full_name":"Schouws, Sander","last_name":"Schouws","first_name":"Sander"},{"first_name":"Renske","last_name":"Smit","full_name":"Smit, Renske"},{"first_name":"Laura","last_name":"Sommovigo","full_name":"Sommovigo, Laura"},{"full_name":"Stark, Daniel P.","last_name":"Stark","first_name":"Daniel P."},{"last_name":"Sugahara","full_name":"Sugahara, Yuma","first_name":"Yuma"},{"first_name":"Livia","full_name":"Vallini, Livia","last_name":"Vallini"},{"first_name":"Bovornpratch","last_name":"Vijarnwannaluk","full_name":"Vijarnwannaluk, Bovornpratch"},{"first_name":"Paul","last_name":"Van Der Werf","full_name":"Van Der Werf, Paul"},{"full_name":"Werner, Norbert","last_name":"Werner","first_name":"Norbert"},{"full_name":"Witstok, Joris","last_name":"Witstok","first_name":"Joris"},{"first_name":"Mengyuan","full_name":"Xiao, Mengyuan","last_name":"Xiao"}],"publication":"The Open Journal of Astrophysics","title":"A first systematic study of [OIII] 88μm at z>8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years","article_type":"original","citation":{"chicago":"Algera, Hiddo S.B., John R. Weaver, Tom J.L.C. Bakx, Manuel Aravena, Rychard J. Bouwens, Karin Cescon, Chian Chou Chen, et al. “A First Systematic Study of [OIII] 88μm at Z&#62;8: Two Luminous Oxygen Lines and a Powerful Ionized Outflow in the First 600 Million Years.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.165333\">https://doi.org/10.33232/001c.165333</a>.","short":"H.S.B. Algera, J.R. Weaver, T.J.L.C. Bakx, M. Aravena, R.J. Bouwens, K. Cescon, C.C. Chen, E. Da Cunha, P. Dayal, A. Faisst, A. Ferrara, S. Fujimoto, T. Hashimoto, K. Heintz, R. Herrera-Camus, J. Hodge, H. Inami, A.K. Inoue, J.J. Matthee, R. Meyer, S. Mizukoshi, C. Mondal, T. Nanayakkara, P.A. Oesch, A. Pallottini, H. Röttgering, L.E. Rowland, S. Schouws, R. Smit, L. Sommovigo, D.P. Stark, Y. Sugahara, L. Vallini, B. Vijarnwannaluk, P. Van Der Werf, N. Werner, J. Witstok, M. Xiao, The Open Journal of Astrophysics 9 (2026).","ama":"Algera HSB, Weaver JR, Bakx TJLC, et al. A first systematic study of [OIII] 88μm at z&#62;8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.165333\">10.33232/001c.165333</a>","mla":"Algera, Hiddo S. B., et al. “A First Systematic Study of [OIII] 88μm at Z&#62;8: Two Luminous Oxygen Lines and a Powerful Ionized Outflow in the First 600 Million Years.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.165333\">10.33232/001c.165333</a>.","apa":"Algera, H. S. B., Weaver, J. R., Bakx, T. J. L. C., Aravena, M., Bouwens, R. J., Cescon, K., … Xiao, M. (2026). A first systematic study of [OIII] 88μm at z&#62;8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.165333\">https://doi.org/10.33232/001c.165333</a>","ista":"Algera HSB, Weaver JR, Bakx TJLC, Aravena M, Bouwens RJ, Cescon K, Chen CC, Da Cunha E, Dayal P, Faisst A, Ferrara A, Fujimoto S, Hashimoto T, Heintz K, Herrera-Camus R, Hodge J, Inami H, Inoue AK, Matthee JJ, Meyer R, Mizukoshi S, Mondal C, Nanayakkara T, Oesch PA, Pallottini A, Röttgering H, Rowland LE, Schouws S, Smit R, Sommovigo L, Stark DP, Sugahara Y, Vallini L, Vijarnwannaluk B, Van Der Werf P, Werner N, Witstok J, Xiao M. 2026. A first systematic study of [OIII] 88μm at z&#62;8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years. The Open Journal of Astrophysics. 9.","ieee":"H. S. B. Algera <i>et al.</i>, “A first systematic study of [OIII] 88μm at z&#62;8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026."},"supplementarymaterial":"yes","researchdata_availability":"no","oa":1,"fulldoi":"https://doi.org/10.33232/001c.165333","acknowledgement":"We thank the referee for their valuable and constructive comments that improved this work. We also thank Javier Alvarez-M´arquez for useful discussions ´\r\nabout the MIRI observations of UHZ1 and UNCOVER37126. HSBA gratefully acknowledges support from\r\nAcademia Sinica through grant AS-PD-1141-M01-2. MA\r\nis supported by FONDECYT grant number 1252054,\r\nand gratefully acknowledges support from ANID Basal\r\nProject FB210003 and ANID MILENIO NCN2024 112.\r\nAKI acknowledges support from KAKENHI Grant No.\r\n23H00131. NW was supported by the GACR EXPRO\r\ngrant No. 21-13491X.\r\nThis paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2024.1.00440.S,\r\nADS/JAO.ALMA#2024.1.01197.S\r\nALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with\r\nNRC (Canada), MOST and ASIAA (Taiwan), and KASI\r\n(Republic of Korea), in cooperation with the Republic\r\nof Chile. The Joint ALMA Observatory is operated by\r\nESO, AUI/NRAO and NAOJ.","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Maynooth Academic Publishing","date_created":"2026-09-13T22:01:57Z","doi":"10.33232/001c.165333","scopus_import":"1","status":"public","has_accepted_license":"1","OA_place":"publisher","department":[{"_id":"JoMa"}],"volume":9,"external_id":{"arxiv":["2512.14486"]},"language":[{"iso":"eng"}],"oa_version":"Published Version","intvolume":"         9","type":"journal_article","date_published":"2026-07-21T00:00:00Z","OA_type":"diamond","ddc":["520"],"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2512.14486"}],"month":"07","dataavailabilitystatement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2024.1.00440.S,\r\nADS/JAO.ALMA#2024.1.01197.S\r\nALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with\r\nNRC (Canada), MOST and ASIAA (Taiwan), and KASI\r\n(Republic of Korea), in cooperation with the Republic\r\nof Chile. The Joint ALMA Observatory is operated by\r\nESO, AUI/NRAO and NAOJ."},{"file_date_updated":"2025-09-30T14:28:25Z","citation":{"short":"H. Katz, A.J. Cameron, A. Saxena, L. Barrufet, N. Choustikov, N.J. Cleri, A. De Graaff, R.S. Ellis, R.A.E. Fosbury, K.E. Heintz, M. Maseda, J.J. Matthee, I. Mcconachie, P.A. Oesch, The Open Journal of Astrophysics 8 (2025).","chicago":"Katz, Harley, Alex J. Cameron, Aayush Saxena, Laia Barrufet, Nicholas Choustikov, Nikko J. Cleri, Anna De Graaff, et al. “21 Balmer Jump Street: The Nebular Continuum at High Redshift and Implications for the Bright Galaxy Problem, UV Continuum Slopes, and Early Stellar Populations.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2025. <a href=\"https://doi.org/10.33232/001c.142570\">https://doi.org/10.33232/001c.142570</a>.","ama":"Katz H, Cameron AJ, Saxena A, et al. 21 Balmer Jump Street: The nebular continuum at high redshift and implications for the bright galaxy problem, UV continuum slopes, and early stellar populations. <i>The Open Journal of Astrophysics</i>. 2025;8. doi:<a href=\"https://doi.org/10.33232/001c.142570\">10.33232/001c.142570</a>","apa":"Katz, H., Cameron, A. J., Saxena, A., Barrufet, L., Choustikov, N., Cleri, N. J., … Oesch, P. A. (2025). 21 Balmer Jump Street: The nebular continuum at high redshift and implications for the bright galaxy problem, UV continuum slopes, and early stellar populations. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.142570\">https://doi.org/10.33232/001c.142570</a>","mla":"Katz, Harley, et al. “21 Balmer Jump Street: The Nebular Continuum at High Redshift and Implications for the Bright Galaxy Problem, UV Continuum Slopes, and Early Stellar Populations.” <i>The Open Journal of Astrophysics</i>, vol. 8, Maynooth Academic Publishing, 2025, doi:<a href=\"https://doi.org/10.33232/001c.142570\">10.33232/001c.142570</a>.","ista":"Katz H, Cameron AJ, Saxena A, Barrufet L, Choustikov N, Cleri NJ, De Graaff A, Ellis RS, Fosbury RAE, Heintz KE, Maseda M, Matthee JJ, Mcconachie I, Oesch PA. 2025. 21 Balmer Jump Street: The nebular continuum at high redshift and implications for the bright galaxy problem, UV continuum slopes, and early stellar populations. The Open Journal of Astrophysics. 8.","ieee":"H. Katz <i>et al.</i>, “21 Balmer Jump Street: The nebular continuum at high redshift and implications for the bright galaxy problem, UV continuum slopes, and early stellar populations,” <i>The Open Journal of Astrophysics</i>, vol. 8. Maynooth Academic Publishing, 2025."},"oa":1,"article_type":"original","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2025-08-17T22:01:37Z","publisher":"Maynooth Academic Publishing","acknowledgement":"HK thanks Andrey Kravtsov for insightful comments and thoughtful discussions. We sincerely thank the PIs and Co-Is of the JWST programs where spectral data was made publicly available on the DJA. We refer interested readers to the following papers for survey descriptions regarding the spectral data: Bunker et al. (2023a); D’Eugenio et al. (2024); Bezanson et al. (2022); Barrufet et al. (2024); de Graaff et al. (2024); Finkelstein et al. (2024); Glazebrook et al. (2024); Pierel et al. (2024); Siebert et al. (2024); Maseda et al. (2024). 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 programs listed in Table 1. AJC and AS acknowledge funding from the “FirstGalaxies” Advanced Grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 789056). ","fulldoi":"https://doi.org/10.33232/001c.142570","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"PlanS_conform":"1","day":"25","article_processing_charge":"No","publication_status":"published","arxiv":1,"date_updated":"2025-09-30T14:29:33Z","abstract":[{"text":"We study the physical origin and spectroscopic impact of extreme nebular emission in high-redshift galaxies. The nebular continuum, which can appear during an extreme starburst, is of particular importance as it tends to redden UV slopes and has a significant contribution to the UV luminosities of galaxies. Furthermore, its shape can be used to infer the gas density and temperature of the interstellar medium. First, we provide a theoretical background, showing how different stellar populations (SPS models, initial mass functions (IMFs), and stellar temperatures) and nebular conditions impact observed galaxy spectra. We demonstrate that, for systems with strong nebular continuum emission, 1) UV fluxes can increase by up to 0.7~mag (or more in the case of hot/massive stars) above the stellar continuum, which may help reconcile the surprising abundance of bright high-redshift galaxies and the elevated UV luminosity density at z>10, 2) at high gas densities, UV slopes can redden from \\beta<-2.5 to \\beta\\sim-1, 3) observational measurements of \\xi_{\\rm ion} are gross underestimates, and 4) UV downturns from two-photon emission can masquerade as damped Ly\\alpha systems. Second, we present a dataset of 58 galaxies observed with NIRSpec on JWST at 2.5<z<9.0 that are selected to have strong nebular continuum emission via the detection of the Balmer jump. Five of the 58 spectra are consistent with being dominated by nebular emission, exhibiting both a Balmer jump and a UV downturn consistent with two-photon emission. For some galaxies, this may imply the presence of hot massive stars and a top-heavy IMF. We conclude by exploring the properties of spectroscopically confirmed z>10 galaxies, finding that UV slopes and UV downturns are in some cases redder or steeper than expected from SPS models, which may hint at more exotic (e.g. hotter/more massive stars or AGN) ionizing sources.","lang":"eng"}],"publication":"The Open Journal of Astrophysics","title":"21 Balmer Jump Street: The nebular continuum at high redshift and implications for the bright galaxy problem, UV continuum slopes, and early stellar populations","author":[{"first_name":"Harley","full_name":"Katz, Harley","last_name":"Katz"},{"first_name":"Alex J.","last_name":"Cameron","full_name":"Cameron, Alex J."},{"first_name":"Aayush","last_name":"Saxena","full_name":"Saxena, Aayush"},{"full_name":"Barrufet, Laia","last_name":"Barrufet","first_name":"Laia"},{"full_name":"Choustikov, Nicholas","last_name":"Choustikov","first_name":"Nicholas"},{"first_name":"Nikko J.","full_name":"Cleri, Nikko J.","last_name":"Cleri"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"Richard S.","last_name":"Ellis","full_name":"Ellis, Richard S."},{"first_name":"Robert A.E.","full_name":"Fosbury, Robert A.E.","last_name":"Fosbury"},{"first_name":"Kasper E.","full_name":"Heintz, Kasper E.","last_name":"Heintz"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Mcconachie","full_name":"Mcconachie, Ian","first_name":"Ian"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."}],"publication_identifier":{"eissn":["2565-6120"]},"year":"2025","_id":"20192","oa_version":"Published Version","date_published":"2025-07-25T00:00:00Z","type":"journal_article","intvolume":"         8","language":[{"iso":"eng"}],"volume":8,"external_id":{"arxiv":["2408.03189"]},"month":"07","file":[{"creator":"dernst","checksum":"ba469d132907147f9e86d87f9124dd14","content_type":"application/pdf","file_name":"2025_OpenJourAstrophysics_Katz.pdf","date_updated":"2025-09-30T14:28:25Z","date_created":"2025-09-30T14:28:25Z","access_level":"open_access","file_id":"20412","success":1,"relation":"main_file","file_size":1836432}],"OA_type":"diamond","ddc":["520"],"quality_controlled":"1","scopus_import":"1","doi":"10.33232/001c.142570","has_accepted_license":"1","status":"public","department":[{"_id":"JoMa"}],"OA_place":"publisher"}]