[{"has_accepted_license":"1","volume":1000,"OA_type":"gold","article_processing_charge":"Yes","citation":{"short":"E.T. Chickles, J. Chakraborty, K.B. Burdge, V.S. Dhillon, P. Draghis, K. El-Badry, M.J. Green, A. Householder, S. Hughes, C. Layden, S.P. Littlefair, J. Munday, I. Pelisoli, M.S. Redden, J. Tonry, J.C. van Roestel, F.E. Angile, A.J. Brown, N.C. Segura, J. Dinsmore, M. Dyer, G. Furesz, M. Gabutti, J. Garbutt, J. García-Mejía, D. Jarvis, M.R. Kennedy, P. Kerry, J. Mccormac, G. Mo, D. Osip, S. Parsons, E. Pike, J.J. Piotrowski, R.W. Romani, D. Sahman, R. Simcoe, The Astrophysical Journal 1000 (2026).","ama":"Chickles ET, Chakraborty J, Burdge KB, et al. An eclipsing 8.56 minutes orbital period mass-transferring binary. <i>The Astrophysical Journal</i>. 2026;1000(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae4871\">10.3847/1538-4357/ae4871</a>","ista":"Chickles ET, Chakraborty J, Burdge KB, Dhillon VS, Draghis P, El-Badry K, Green MJ, Householder A, Hughes S, Layden C, Littlefair SP, Munday J, Pelisoli I, Redden MS, Tonry J, van Roestel JC, Angile FE, Brown AJ, Segura NC, Dinsmore J, Dyer M, Furesz G, Gabutti M, Garbutt J, García-Mejía J, Jarvis D, Kennedy MR, Kerry P, Mccormac J, Mo G, Osip D, Parsons S, Pike E, Piotrowski JJ, Romani RW, Sahman D, Simcoe R. 2026. An eclipsing 8.56 minutes orbital period mass-transferring binary. The Astrophysical Journal. 1000(2), 237.","mla":"Chickles, Emma T., et al. “An Eclipsing 8.56 Minutes Orbital Period Mass-Transferring Binary.” <i>The Astrophysical Journal</i>, vol. 1000, no. 2, 237, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae4871\">10.3847/1538-4357/ae4871</a>.","chicago":"Chickles, Emma T., Joheen Chakraborty, Kevin B. Burdge, Vik S. Dhillon, Paul Draghis, Kareem El-Badry, Matthew J. Green, et al. “An Eclipsing 8.56 Minutes Orbital Period Mass-Transferring Binary.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae4871\">https://doi.org/10.3847/1538-4357/ae4871</a>.","ieee":"E. T. Chickles <i>et al.</i>, “An eclipsing 8.56 minutes orbital period mass-transferring binary,” <i>The Astrophysical Journal</i>, vol. 1000, no. 2. IOP Publishing, 2026.","apa":"Chickles, E. T., Chakraborty, J., Burdge, K. B., Dhillon, V. S., Draghis, P., El-Badry, K., … Simcoe, R. (2026). An eclipsing 8.56 minutes orbital period mass-transferring binary. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae4871\">https://doi.org/10.3847/1538-4357/ae4871</a>"},"ddc":["520"],"day":"01","publication_status":"published","date_published":"2026-04-01T00:00:00Z","intvolume":"      1000","quality_controlled":"1","date_updated":"2026-05-04T06:37:12Z","OA_place":"publisher","file":[{"relation":"main_file","creator":"dernst","success":1,"date_updated":"2026-05-04T06:36:00Z","content_type":"application/pdf","file_size":1225916,"access_level":"open_access","date_created":"2026-05-04T06:36:00Z","file_name":"2026_AstrophysicalJournal_Chickles.pdf","checksum":"c8f64a78f36224d8e0ea1f324e43e389","file_id":"21782"}],"oa":1,"author":[{"full_name":"Chickles, Emma T.","first_name":"Emma T.","last_name":"Chickles"},{"last_name":"Chakraborty","full_name":"Chakraborty, Joheen","first_name":"Joheen"},{"first_name":"Kevin B.","full_name":"Burdge, Kevin B.","last_name":"Burdge"},{"last_name":"Dhillon","first_name":"Vik S.","full_name":"Dhillon, Vik S."},{"last_name":"Draghis","first_name":"Paul","full_name":"Draghis, Paul"},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"first_name":"Matthew J.","full_name":"Green, Matthew J.","last_name":"Green"},{"full_name":"Householder, Aaron","first_name":"Aaron","last_name":"Householder"},{"last_name":"Hughes","full_name":"Hughes, Sarah","first_name":"Sarah"},{"last_name":"Layden","full_name":"Layden, Christopher","first_name":"Christopher"},{"last_name":"Littlefair","first_name":"Stuart P.","full_name":"Littlefair, Stuart P."},{"last_name":"Munday","first_name":"James","full_name":"Munday, James"},{"first_name":"Ingrid","full_name":"Pelisoli, Ingrid","last_name":"Pelisoli"},{"first_name":"Maya S.","full_name":"Redden, Maya S.","last_name":"Redden"},{"first_name":"John","full_name":"Tonry, John","last_name":"Tonry"},{"full_name":"van Roestel, Joannes C","first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","last_name":"van Roestel"},{"full_name":"Angile, Francesco Elio","first_name":"Francesco Elio","last_name":"Angile"},{"first_name":"Alex J.","full_name":"Brown, Alex J.","last_name":"Brown"},{"last_name":"Segura","first_name":"Noel Castro","full_name":"Segura, Noel Castro"},{"full_name":"Dinsmore, Jack","first_name":"Jack","last_name":"Dinsmore"},{"full_name":"Dyer, Martin","first_name":"Martin","last_name":"Dyer"},{"last_name":"Furesz","full_name":"Furesz, Gabor","first_name":"Gabor"},{"last_name":"Gabutti","first_name":"Michelle","full_name":"Gabutti, Michelle"},{"last_name":"Garbutt","full_name":"Garbutt, James","first_name":"James"},{"first_name":"Juliana","full_name":"García-Mejía, Juliana","last_name":"García-Mejía"},{"last_name":"Jarvis","full_name":"Jarvis, Daniel","first_name":"Daniel"},{"last_name":"Kennedy","first_name":"Mark R.","full_name":"Kennedy, Mark R."},{"full_name":"Kerry, Paul","first_name":"Paul","last_name":"Kerry"},{"last_name":"Mccormac","full_name":"Mccormac, James","first_name":"James"},{"last_name":"Mo","first_name":"Geoffrey","full_name":"Mo, Geoffrey"},{"last_name":"Osip","full_name":"Osip, Dave","first_name":"Dave"},{"last_name":"Parsons","full_name":"Parsons, Steven","first_name":"Steven"},{"first_name":"Eleanor","full_name":"Pike, Eleanor","last_name":"Pike"},{"first_name":"John J.","full_name":"Piotrowski, John J.","last_name":"Piotrowski"},{"full_name":"Romani, Roger W.","first_name":"Roger W.","last_name":"Romani"},{"full_name":"Sahman, David","first_name":"David","last_name":"Sahman"},{"first_name":"Rob","full_name":"Simcoe, Rob","last_name":"Simcoe"}],"status":"public","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"date_created":"2026-04-12T22:01:47Z","publisher":"IOP Publishing","article_type":"original","oa_version":"Published Version","arxiv":1,"article_number":"237","license":"https://creativecommons.org/licenses/by/4.0/","acknowledgement":"This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near-Earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889 and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and the Millennium Institute of Astrophysics (MAS), Chile. VSD and ULTRACAM are supported by STFC grant ST/Z000033/1. J.G.M. gratefully acknowledges support from the Heising-Simons Foundation and the Pappalardo family through the MIT Pappalardo Fellowship in Physics.","abstract":[{"text":"We report the discovery of ATLAS J101342.5−451656.8 (hereafter ATLAS J1013−4516), an 8.56 minute orbital-period mass-transferring AM Canum Venaticorum (AM CVn) binary with a mean Gaia magnitude of G = 19.51, identified via periodic variability in light curves from the Asteroid Terrestrial-impact Last Alert System (ATLAS) of Gaia white dwarf candidates. Follow-up with the Large Lenslet Array Magellan Spectrograph shows a helium-dominated accretion disk, and high-speed ULTRACAM photometry reveals pronounced primary and secondary eclipses. We construct a decade-long timing baseline leveraging light curves from the ATLAS and Gaia surveys, as well as the high-speed imagers ULTRACAM on the New Energy Telescope and proto-Lightspeed on the Magellan Clay telescope. From this timing baseline, we measure an orbital period derivative of P 1.60 0.07 10 = ± × 12 s s−1. Interpreted in the context of stable mass transfer, the magnitude and sign of P indicate that the orbital evolution is governed by the interplay between gravitationalwave-driven angular-momentum losses and mass transfer, directly probing the donor’s structural response to mass loss. We constrain the accretor and donor mass based on stable mass-transfer arguments assuming angularmomentum loss dominated by gravitational-wave emission, allowing us to infer the characteristic gravitational\r\nwave strain of the binary for future space-based GW observatories such as the Laser Interferometer Space Antenna (LISA). We predict a characteristic strain corresponding to a 4 yr LISA signal-to-noise ratio ≳10, establishing ATLAS J1013−4516 as a strong prospective LISA source that will probe long-term orbital evolution in the mass-transferring regime.","lang":"eng"}],"DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"An eclipsing 8.56 minutes orbital period mass-transferring binary","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2601.07925"]},"year":"2026","month":"04","type":"journal_article","_id":"21705","department":[{"_id":"IlCa"}],"file_date_updated":"2026-05-04T06:36:00Z","scopus_import":"1","issue":"2","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"doi":"10.3847/1538-4357/ae4871"},{"has_accepted_license":"1","article_processing_charge":"Yes","citation":{"apa":"Papovich, C., Cole, J. W., Hu, W., Finkelstein, S. L., Shen, L., Arrabal Haro, P., … Yung, L. Y. A. (2026). Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae3b25\">https://doi.org/10.3847/1538-4357/ae3b25</a>","ieee":"C. Papovich <i>et al.</i>, “Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions,” <i>The Astrophysical Journal</i>, vol. 1000, no. 1. IOP Publishing, 2026.","chicago":"Papovich, Casey, Justin W. Cole, Weida Hu, Steven L. Finkelstein, Lu Shen, Pablo Arrabal Haro, Ricardo O. Amorín, et al. “Galaxies in the Epoch of Reionization Are All Bark and No Bite-Plenty of Ionizing Photons, Low Escape Fractions.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae3b25\">https://doi.org/10.3847/1538-4357/ae3b25</a>.","short":"C. Papovich, J.W. Cole, W. Hu, S.L. Finkelstein, L. Shen, P. Arrabal Haro, R.O. Amorín, B.E. Backhaus, M.B. Bagley, R. Bhatawdekar, A. Calabrò, A.C. Carnall, N.J. Cleri, E. Daddi, M. Dickinson, N.A. Grogin, B.W. Holwerda, A.E. Jaskot, A.M. Koekemoer, M. Llerena, R.A. Lucas, S. Mascia, F. Pacucci, L. Pentericci, P.G. Pérez-González, N. Pirzkal, S. Raghunathan, L.M. Seillé, R.S. Somerville, L.Y.A. Yung, The Astrophysical Journal 1000 (2026).","mla":"Papovich, Casey, et al. “Galaxies in the Epoch of Reionization Are All Bark and No Bite-Plenty of Ionizing Photons, Low Escape Fractions.” <i>The Astrophysical Journal</i>, vol. 1000, no. 1, 111, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae3b25\">10.3847/1538-4357/ae3b25</a>.","ama":"Papovich C, Cole JW, Hu W, et al. Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions. <i>The Astrophysical Journal</i>. 2026;1000(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae3b25\">10.3847/1538-4357/ae3b25</a>","ista":"Papovich C, Cole JW, Hu W, Finkelstein SL, Shen L, Arrabal Haro P, Amorín RO, Backhaus BE, Bagley MB, Bhatawdekar R, Calabrò A, Carnall AC, Cleri NJ, Daddi E, Dickinson M, Grogin NA, Holwerda BW, Jaskot AE, Koekemoer AM, Llerena M, Lucas RA, Mascia S, Pacucci F, Pentericci L, Pérez-González PG, Pirzkal N, Raghunathan S, Seillé LM, Somerville RS, Yung LYA. 2026. Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions. The Astrophysical Journal. 1000(1), 111."},"publication_status":"published","ddc":["520"],"day":"20","volume":1000,"OA_type":"gold","date_published":"2026-03-20T00:00:00Z","date_updated":"2026-05-04T10:44:57Z","OA_place":"publisher","quality_controlled":"1","intvolume":"      1000","status":"public","file":[{"file_size":6670398,"content_type":"application/pdf","date_updated":"2026-05-04T10:40:07Z","success":1,"creator":"dernst","relation":"main_file","file_id":"21791","file_name":"2026_AstrophysicalJour_Papovich.pdf","checksum":"0031a6f197a3fa8c2845de10b6bdc696","date_created":"2026-05-04T10:40:07Z","access_level":"open_access"}],"oa":1,"author":[{"last_name":"Papovich","first_name":"Casey","full_name":"Papovich, Casey"},{"last_name":"Cole","first_name":"Justin W.","full_name":"Cole, Justin W."},{"last_name":"Hu","first_name":"Weida","full_name":"Hu, Weida"},{"first_name":"Steven L.","full_name":"Finkelstein, Steven L.","last_name":"Finkelstein"},{"last_name":"Shen","full_name":"Shen, Lu","first_name":"Lu"},{"last_name":"Arrabal Haro","first_name":"Pablo","full_name":"Arrabal Haro, Pablo"},{"last_name":"Amorín","first_name":"Ricardo O.","full_name":"Amorín, Ricardo O."},{"last_name":"Backhaus","full_name":"Backhaus, Bren E.","first_name":"Bren E."},{"full_name":"Bagley, Micaela B.","first_name":"Micaela B.","last_name":"Bagley"},{"full_name":"Bhatawdekar, Rachana","first_name":"Rachana","last_name":"Bhatawdekar"},{"full_name":"Calabrò, Antonello","first_name":"Antonello","last_name":"Calabrò"},{"last_name":"Carnall","full_name":"Carnall, Adam C.","first_name":"Adam C."},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"first_name":"Emanuele","full_name":"Daddi, Emanuele","last_name":"Daddi"},{"last_name":"Dickinson","full_name":"Dickinson, Mark","first_name":"Mark"},{"last_name":"Grogin","first_name":"Norman A.","full_name":"Grogin, Norman A."},{"full_name":"Holwerda, Benne W.","first_name":"Benne W.","last_name":"Holwerda"},{"full_name":"Jaskot, Anne E.","first_name":"Anne E.","last_name":"Jaskot"},{"full_name":"Koekemoer, Anton M.","first_name":"Anton M.","last_name":"Koekemoer"},{"last_name":"Llerena","first_name":"Mario","full_name":"Llerena, Mario"},{"first_name":"Ray A.","full_name":"Lucas, Ray A.","last_name":"Lucas"},{"last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"last_name":"Pacucci","full_name":"Pacucci, Fabio","first_name":"Fabio"},{"last_name":"Pentericci","full_name":"Pentericci, Laura","first_name":"Laura"},{"full_name":"Pérez-González, Pablo G.","first_name":"Pablo G.","last_name":"Pérez-González"},{"last_name":"Pirzkal","first_name":"Nor","full_name":"Pirzkal, Nor"},{"last_name":"Raghunathan","first_name":"Srinivasan","full_name":"Raghunathan, Srinivasan"},{"last_name":"Seillé","full_name":"Seillé, Lise Marie","first_name":"Lise Marie"},{"full_name":"Somerville, Rachel S.","first_name":"Rachel S.","last_name":"Somerville"},{"first_name":"L. Y.Aaron","full_name":"Yung, L. Y.Aaron","last_name":"Yung"}],"publisher":"IOP Publishing","date_created":"2026-04-12T22:01:49Z","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"oa_version":"Published Version","arxiv":1,"article_type":"original","acknowledgement":"We wish to thank our colleagues in the CEERS collaboration for their hard work and valuable contributions on this project. We extend our sincerest thanks to the anonymous referee whose critical and constructive report improved the quality of this manuscript. We also thank the JADES team for providing an excellent dataset for science. We with to thank colleagues for valuable discussions, feedback, and suggestions, including John Chisholm, Kevin Huffenberger, Jessica\r\nMeh, Julian Muñoz, Irene Shivaei, Justin Spilker, Aaron Smith, and Romain Teyssier.\r\nPortions of this research were conducted with the advanced computing resources provided by Texas A&M High Performance Research Computing (HPRC, http://hprc.tamu.edu). This work benefited from support from the George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University. CP thanks Marsha and Ralph Schilling for generous support of this research. This work was partially support by the Future Investigators in NASA Earth and Space Science and Technology (FINESST) program grant No. 80NSSC23K1487. R.A. acknowledges support of grant PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. A.C.C. acknowledges support from a UKRI Frontier Research Guarantee Grant (PI Carnall; grant reference EP/Y037065/1) This work acknowledges support from the NASA/ESA/CSA James Webb Space Telescope through the\r\nSpace Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-03127. Support for program JWST-ERS-01345.009-A, JWST-GO-02079.013-A, JWST-GO-06368.011-A, and JWST-GO-01837.030-A, 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. This work made use of v2.2 of the Binary Population\r\nand Spectral Synthesis (BPASS) models as described in E. R. Stanway & J. J. Eldridge (2018).","article_number":"111","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions","abstract":[{"lang":"eng","text":"Early results from JWST suggest that Epoch of Reionization (EoR) galaxies produce copious ionizing photons, which, if they escape efficiently, could cause reionization to occur too early. We study this problem using JWST imaging and prism spectroscopy for 412 galaxies at 4.5 < z < 9.0. We fit these data simultaneously with stellar population and nebular emission models that include a parameter for the fraction of ionizing photons that escape the galaxy, fesc. We find that the ionization production efficiency, ξion = Q(H0)/LUV, increases with redshift and decreasing UV luminosity, but shows significant scatter, (log ion z, MUV) 0.3 dex. The inferred escape fractions averaged over the population are low, ranging from〈fesc〉 ≃ 2.6% ± 1.4% at 6 < z < 9 to 6.5% ± 2.2% at 4.5 < z < 6, with weak or no indication of evolution with redshift. This implies that in our models most of the ionizing photons need to be absorbed to account for the nebular emission. We compute the impact of our results on reionization, including the distributions for ξion and fesc, and the evolution and uncertainty of the UV luminosity function. Considering galaxies brighter than MUV < −16 mag would produce an intergalactic medium hydrogen-ionized fraction of xe = 0.5 at 5.3 < z < 5.8, possibly too late compared to constraints from from quasistellar\r\nobject (QSO) sight lines. Including fainter galaxies, MUV < −14 mag, we obtain xe = 0.5 at 6.0 < z < 8.1, fully consistent with QSO and cosmic microwave background data. This implies that EoR galaxies produce plenty of ionizing photons, but that these do not efficiently escape. This may be a result of high gas column densities combined with burstier star formation histories, which limit the time massive stars are able to clear channels through the gas for ionizing photons to escape."}],"external_id":{"arxiv":["2505.08870"]},"year":"2026","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"month":"03","type":"journal_article","department":[{"_id":"JoMa"}],"_id":"21710","file_date_updated":"2026-05-04T10:40:07Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"issue":"1","doi":"10.3847/1538-4357/ae3b25","scopus_import":"1"},{"has_accepted_license":"1","citation":{"apa":"Lin, A., Charisi, M., &#38; Haiman, Z. (2026). Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae29a7\">https://doi.org/10.3847/1538-4357/ae29a7</a>","chicago":"Lin, Allison, Maria Charisi, and Zoltán Haiman. “Lomb-Scargle Periodogram Struggles with Non-Sinusoidal Supermassive Black Hole Binary Signatures in Quasar Lightcurves.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae29a7\">https://doi.org/10.3847/1538-4357/ae29a7</a>.","ieee":"A. Lin, M. Charisi, and Z. Haiman, “Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves,” <i>The Astrophysical Journal</i>, vol. 997, no. 2. IOP Publishing, 2026.","ama":"Lin A, Charisi M, Haiman Z. Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. <i>The Astrophysical Journal</i>. 2026;997(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae29a7\">10.3847/1538-4357/ae29a7</a>","ista":"Lin A, Charisi M, Haiman Z. 2026. Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves. The Astrophysical Journal. 997(2), 316.","mla":"Lin, Allison, et al. “Lomb-Scargle Periodogram Struggles with Non-Sinusoidal Supermassive Black Hole Binary Signatures in Quasar Lightcurves.” <i>The Astrophysical Journal</i>, vol. 997, no. 2, 316, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae29a7\">10.3847/1538-4357/ae29a7</a>.","short":"A. Lin, M. Charisi, Z. Haiman, The Astrophysical Journal 997 (2026)."},"article_processing_charge":"Yes","publication_status":"published","day":"01","ddc":["520"],"volume":997,"OA_type":"gold","date_published":"2026-02-01T00:00:00Z","date_updated":"2026-05-04T10:26:59Z","OA_place":"publisher","quality_controlled":"1","intvolume":"       997","status":"public","file":[{"file_name":"2026_AstrophysicalJour_Lin.pdf","checksum":"5162d1539ef7d10927ef73d8b4500017","file_id":"21789","access_level":"open_access","date_created":"2026-05-04T10:24:49Z","content_type":"application/pdf","file_size":2619679,"creator":"dernst","relation":"main_file","success":1,"date_updated":"2026-05-04T10:24:49Z"}],"oa":1,"author":[{"full_name":"Lin, Allison","first_name":"Allison","last_name":"Lin"},{"full_name":"Charisi, Maria","first_name":"Maria","last_name":"Charisi"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman","orcid":"0000-0003-3633-5403"}],"date_created":"2026-04-12T22:01:49Z","publisher":"IOP Publishing","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"oa_version":"Published Version","article_type":"original","acknowledgement":"M.C. acknowledges support by the European Union (ERC; MMMonsters, 101117624). This work was also supported in part by NASA grants 80NSSC24K0440 and 80NSSC22K0822. This research used the resources of the Center for Institutional Research Computing at Washington State University.","article_number":"316","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Lomb-scargle periodogram struggles with non-sinusoidal supermassive Black Hole binary signatures in quasar lightcurves","abstract":[{"lang":"eng","text":"Supermassive black hole binary (SMBHB) systems are expected to form as a consequence of galaxy mergers. At subparsec separations, SMBHBs can be identified as quasars with periodic variability, with previous periodicity searches uncovering significant candidates. However, these searches focused primarily on sinusoidal signals, while theoretical models and hydrodynamical simulations predict that binaries produce more complex non-sinusoidal pulse shapes. Here we examine the efficacy of the Lomb–Scargle periodogram (LSP; one of the most popular tools for periodicity searches in unevenly sampled lightcurves) to detect periodicities with a sawtooth shape mimicking results of hydrodynamical simulations. We simulate idealized well-sampled lightcurves, lightcurves that mimic the data in the Palomar Transient Factory (PTF) analyzed in M. Charisi et al. (2016), and lightcurves that resemble our expectations for single-band data in the upcoming Legacy Survey of Space and Time (LSST) of the Rubin Observatory. We approximate quasar variability with a damped random walk (DRW) model, inject sinusoidal and sawtooth pulse shapes, and assess their statistical significance. We find that in the presence of red noise, the LSP detects a relatively low fraction of the sinusoidal signals (∼45%, ∼24%, and ∼23%, in the PTF-like, idealized, and LSST-like lightcurves, respectively). The fraction is significantly reduced for sawtooth periodicity (with only ∼9% in PTF-like and ∼1% in idealized and LSST-like lightcurves). These low recovery rates imply that previous searches have missed the large majority of binaries. They also have significant implications for the detection of SMBHBs in upcoming LSST necessitating the development of advanced tools that go beyond the simple LSP."}],"DOAJ_listed":"1","year":"2026","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"month":"02","type":"journal_article","department":[{"_id":"ZoHa"}],"_id":"21712","file_date_updated":"2026-05-04T10:24:49Z","issue":"2","doi":"10.3847/1538-4357/ae29a7","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"scopus_import":"1"},{"has_accepted_license":"1","date_published":"2026-01-10T00:00:00Z","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"article_processing_charge":"Yes","citation":{"apa":"Greene, J. E., Setton, D. J., Furtak, L. J., Naidu, R. P., Volonteri, M., Dayal, P., … Zitrin, A. (2026). What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae1836\">https://doi.org/10.3847/1538-4357/ae1836</a>","ieee":"J. E. Greene <i>et al.</i>, “What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots,” <i>The Astrophysical Journal</i>, vol. 996, no. 2. IOP Publishing, 2026.","chicago":"Greene, Jenny E., David J. Setton, Lukas J. Furtak, Rohan P. Naidu, Marta Volonteri, Pratika Dayal, Ivo Labbe, et al. “What You See Is What You Get: Empirically Measured Bolometric Luminosities of Little Red Dots.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae1836\">https://doi.org/10.3847/1538-4357/ae1836</a>.","short":"J.E. Greene, D.J. Setton, L.J. Furtak, R.P. Naidu, M. Volonteri, P. Dayal, I. Labbe, P. Van Dokkum, R. Bezanson, G. Brammer, S.E. Cutler, K. Glazebrook, A. De Graaff, M. Hirschmann, R.E. Hviding, V. Kokorev, J. Leja, H. Liu, Y. Ma, J.J. Matthee, T. Nanayakkara, P.A. Oesch, R. Pan, S.H. Price, J.S. Spilker, B. Wang, J.R. Weaver, K.E. Whitaker, C.C. Williams, A. Zitrin, The Astrophysical Journal 996 (2026).","ista":"Greene JE, Setton DJ, Furtak LJ, Naidu RP, Volonteri M, Dayal P, Labbe I, Van Dokkum P, Bezanson R, Brammer G, Cutler SE, Glazebrook K, De Graaff A, Hirschmann M, Hviding RE, Kokorev V, Leja J, Liu H, Ma Y, Matthee JJ, Nanayakkara T, Oesch PA, Pan R, Price SH, Spilker JS, Wang B, Weaver JR, Whitaker KE, Williams CC, Zitrin A. 2026. What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. The Astrophysical Journal. 996(2), 129.","ama":"Greene JE, Setton DJ, Furtak LJ, et al. What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. <i>The Astrophysical Journal</i>. 2026;996(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1836\">10.3847/1538-4357/ae1836</a>","mla":"Greene, Jenny E., et al. “What You See Is What You Get: Empirically Measured Bolometric Luminosities of Little Red Dots.” <i>The Astrophysical Journal</i>, vol. 996, no. 2, 129, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1836\">10.3847/1538-4357/ae1836</a>."},"day":"10","ddc":["520"],"publication_status":"published","volume":996,"OA_type":"gold","status":"public","file":[{"access_level":"open_access","date_created":"2026-05-04T11:19:48Z","checksum":"7b3cb025d4bcaa35c6e52bd0c8fb6cf4","file_name":"2026_AstrophysicalJour_Greene.pdf","file_id":"21792","relation":"main_file","creator":"dernst","date_updated":"2026-05-04T11:19:48Z","success":1,"content_type":"application/pdf","file_size":684400}],"oa":1,"author":[{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"first_name":"David J.","full_name":"Setton, David J.","last_name":"Setton"},{"first_name":"Lukas J.","full_name":"Furtak, Lukas J.","last_name":"Furtak"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"last_name":"Volonteri","first_name":"Marta","full_name":"Volonteri, Marta"},{"last_name":"Dayal","full_name":"Dayal, Pratika","first_name":"Pratika"},{"full_name":"Labbe, Ivo","first_name":"Ivo","last_name":"Labbe"},{"full_name":"Van Dokkum, Pieter","first_name":"Pieter","last_name":"Van Dokkum"},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"first_name":"Sam E.","full_name":"Cutler, Sam E.","last_name":"Cutler"},{"full_name":"Glazebrook, Karl","first_name":"Karl","last_name":"Glazebrook"},{"first_name":"Anna","full_name":"De Graaff, Anna","last_name":"De Graaff"},{"first_name":"Michaela","full_name":"Hirschmann, Michaela","last_name":"Hirschmann"},{"last_name":"Hviding","first_name":"Raphael E.","full_name":"Hviding, Raphael E."},{"full_name":"Kokorev, Vasily","first_name":"Vasily","last_name":"Kokorev"},{"last_name":"Leja","full_name":"Leja, Joel","first_name":"Joel"},{"first_name":"Hanpu","full_name":"Liu, Hanpu","last_name":"Liu"},{"first_name":"Yilun","full_name":"Ma, Yilun","last_name":"Ma"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"last_name":"Pan","full_name":"Pan, Richard","first_name":"Richard"},{"full_name":"Price, Sedona H.","first_name":"Sedona H.","last_name":"Price"},{"full_name":"Spilker, Justin S.","first_name":"Justin S.","last_name":"Spilker"},{"first_name":"Bingjie","full_name":"Wang, Bingjie","last_name":"Wang"},{"first_name":"John R.","full_name":"Weaver, John R.","last_name":"Weaver"},{"first_name":"Katherine E.","full_name":"Whitaker, Katherine E.","last_name":"Whitaker"},{"last_name":"Williams","full_name":"Williams, Christina C.","first_name":"Christina C."},{"first_name":"Adi","full_name":"Zitrin, Adi","last_name":"Zitrin"}],"date_updated":"2026-05-04T11:20:42Z","OA_place":"publisher","quality_controlled":"1","intvolume":"       996","oa_version":"Published Version","arxiv":1,"PlanS_conform":"1","article_type":"original","publisher":"IOP Publishing","date_created":"2026-04-12T22:01:50Z","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots","DOAJ_listed":"1","abstract":[{"text":"New populations of red active galactic nuclei (known as “little red dots”) discovered by JWST exhibit remarkable spectral energy distributions. Leveraging X-ray through far-infrared observations of two of the most luminous known little red dots, we directly measure their bolometric luminosities. We find evidence that more than half of the bolometric luminosity likely emerges in the rest-frame optical, with Lbol/L5100 = 5, roughly half the value for “standard” active galactic nuclei. Meanwhile, the X-ray emitting corona, UV-emitting blackbody, and reprocessed mid to far-infrared emission are all considerably subdominant, assuming that the far-infrared luminosity is well below current measured limits. We present new bolometric corrections that dramatically lower inferred bolometric luminosities by a factor of 10 compared to published values in the literature. These bolometric corrections are in accord with expectations from models in which gas absorption and reprocessing are responsible for the red rest-frame optical colors of little red dots. We discuss how this lowered luminosity scale suggests a lower mass scale for the population by at least an order of magnitude (e.g., ∼105–107 M⊙ black holes, and ∼108 M⊙ galaxies), alleviating tensions with clustering, overmassive black holes, and the integrated black hole mass density in the Universe.","lang":"eng"}],"acknowledgement":"We benefit from the following JWST programs: UNCOVER (JWST/GO #2561; Labbé & Bezanson); ALT (JWST-GO #3516; Naidu & Matthee); MegaScience (JWST-GO #4111; Suess); RUBIES (JWST-GO #4233; de Graaff & Brammer); PRIMER (JWST/GO #1837; Dunlop).\r\n\r\nWe acknowledge funding from NSF/AAG #2306950, JWST-GO-02561, JWST-GO-03516, and JWST-GO-04111, provided through a grant from the STScI under NASA contract NAS5-03127. I.L. acknowledges support from Australian Research Council Future Fellowship FT220100798. K.G. and T.N. acknowledge support from Australian Research Council Laureate Fellowship FL180100060. A.Z. 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); by the Ministry of Science & Technology, Israel; and by the Israel Science Foundation grant No. 864/23. J.M. and I.K. are 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. Y.F. acknowledges support from JSPS KAKENHI grant No. JSPS KAKENHI grant Nos. JP22K21349 and JP23K13149. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. 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. The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. J.M. acknowledges funding by the European Union (ERC, AGENTS, 101076224). R.E.H. acknowledges support by the German Aerospace Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.”","article_number":"129","month":"01","type":"journal_article","external_id":{"arxiv":["2509.05434"]},"year":"2026","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"JoMa"}],"_id":"21715","issue":"2","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae1836","scopus_import":"1","file_date_updated":"2026-05-04T11:19:48Z"},{"type":"journal_article","month":"01","year":"2026","external_id":{"arxiv":["2510.24877"]},"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"title":"The White Dwarf initial–final mass relation from open clusters in Gaia DR3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"The initial–final mass relation (IFMR) links a star’s birth mass to the mass of its white dwarf (WD) remnant, providing key constraints on stellar evolution. Open clusters offer the most straightforward way to empirically determine the IFMR, as their well-defined ages allow for direct progenitor lifetime estimates. We construct the most comprehensive open cluster WD IFMR to date by combining new spectroscopy of 22 WDs with an extensive literature review of WDs with strong cluster associations. To minimize systematics, we restrict our analysis to spectroscopically confirmed hydrogen-atmosphere (DA) WDs consistent with single-stellar origins. We separately analyze a subset with reliable Gaia-based astrometric membership assessments, as well as a full sample that adds WDs with strong cluster associations whose membership cannot be reliably assessed with Gaia. The Gaia-based sample includes 69 spectroscopically confirmed DA WDs, more than doubling the sample size of previous Gaia-based open cluster IFMRs. The full sample, which includes 53 additional literature WDs,\r\nincreases the total number of cluster WDs by over 50% relative to earlier works. We provide functional forms for both the Gaia-based and full-sample IFMRs. The Gaia-based result useful for Mi � 2.67 M⊙ is Mf = [0.179 0.100H (Mi 3.84 M )] × (Mi 3.84 M ) + 0.628 M , where H(x) is the Heaviside step function. Comparing our IFMR to recent literature, we identify significant deviations from best-fit IFMRs derived from both Gaia-based volume-limited samples of field WDs and double WD binaries, with the largest discrepancy occurring for initial masses of about 5 M⊙.","lang":"eng"}],"DOAJ_listed":"1","acknowledgement":"The authors would like to thank the anonymous referee for their constructive feedback, which helped improve the clarify of the manuscript. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada Discovery grants Nos. DG-RGPIN-2022-03051 and DG-RGPIN-2023-04486. This research received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program number 101002408 (MOS100PC). This work includes results based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.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. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Gemini spectra were processed using the DRAGONS package (K. Labrie et al. 2023). LRIS spectra were reduced using the Lpipe pipeline (D. A. Perley 2019).\r\n\r\nFacilities: Gaia - (DR2 & DR3), Gemini:Gillett - Gillett Gemini North Telescope (GMOS-N), Gemini:South - Gemini South Telescope (GMOS-S), Keck:I - KECK I Telescope (LRIS).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013,2018, 2022), emcee (D. Foreman-Mackey et al. 2013).","article_number":"69","doi":"10.3847/1538-4357/ae18c8","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"scopus_import":"1","file_date_updated":"2026-04-13T08:36:50Z","keyword":["White dwarf stars","Open star clusters","Compact objects","Stellar evolution"],"department":[{"_id":"IlCa"}],"_id":"21725","date_published":"2026-01-01T00:00:00Z","day":"01","ddc":["520"],"publication_status":"published","article_processing_charge":"Yes","citation":{"ieee":"D. R. Miller <i>et al.</i>, “The White Dwarf initial–final mass relation from open clusters in Gaia DR3,” <i>The Astrophysical Journal</i>, vol. 996, no. 1. IOP Publishing, 2026.","apa":"Miller, D. R., Caiazzo, I., Heyl, J., Richer, H. B., Hollands, M. A., Tremblay, P. E., … Vanderbosch, Z. P. (2026). The White Dwarf initial–final mass relation from open clusters in Gaia DR3. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">https://doi.org/10.3847/1538-4357/ae18c8</a>","chicago":"Miller, David R., Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Mark A. Hollands, Pier Emmanuel Tremblay, Kareem El-Badry, Antonio C. Rodriguez, and Zachary P. Vanderbosch. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">https://doi.org/10.3847/1538-4357/ae18c8</a>.","short":"D.R. Miller, I. Caiazzo, J. Heyl, H.B. Richer, M.A. Hollands, P.E. Tremblay, K. El-Badry, A.C. Rodriguez, Z.P. Vanderbosch, The Astrophysical Journal 996 (2026).","mla":"Miller, David R., et al. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” <i>The Astrophysical Journal</i>, vol. 996, no. 1, 69, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">10.3847/1538-4357/ae18c8</a>.","ama":"Miller DR, Caiazzo I, Heyl J, et al. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. <i>The Astrophysical Journal</i>. 2026;996(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">10.3847/1538-4357/ae18c8</a>","ista":"Miller DR, Caiazzo I, Heyl J, Richer HB, Hollands MA, Tremblay PE, El-Badry K, Rodriguez AC, Vanderbosch ZP. 2026. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. The Astrophysical Journal. 996(1), 69."},"OA_type":"gold","volume":996,"has_accepted_license":"1","arxiv":1,"oa_version":"Published Version","article_type":"original","PlanS_conform":"1","date_created":"2026-04-12T22:01:52Z","publisher":"IOP Publishing","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","status":"public","author":[{"last_name":"Miller","full_name":"Miller, David R.","first_name":"David R."},{"last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria"},{"last_name":"Heyl","first_name":"Jeremy","full_name":"Heyl, Jeremy"},{"last_name":"Richer","full_name":"Richer, Harvey B.","first_name":"Harvey B."},{"last_name":"Hollands","first_name":"Mark A.","full_name":"Hollands, Mark A."},{"last_name":"Tremblay","full_name":"Tremblay, Pier Emmanuel","first_name":"Pier Emmanuel"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"last_name":"Vanderbosch","first_name":"Zachary P.","full_name":"Vanderbosch, Zachary P."}],"oa":1,"file":[{"relation":"main_file","creator":"dernst","success":1,"date_updated":"2026-04-13T08:36:50Z","file_size":19310053,"content_type":"application/pdf","access_level":"open_access","date_created":"2026-04-13T08:36:50Z","checksum":"65a8237a519188af83b6dc4d47ad85fa","file_name":"2026_AstrophysicalJournal_Miller.pdf","file_id":"21733"}],"OA_place":"publisher","date_updated":"2026-04-13T08:39:39Z","quality_controlled":"1","intvolume":"       996"},{"acknowledgement":"We thank the anonymous referee for a careful reading of the manuscript and for constructive comments that improved the paper. X.P.C. and S.T. thank J.L. Gragera-Más and Ylva Götberg for their valuable feedback and comments. X.P.C. acknowledges financial support from the Spanish National Programme for the Promotion of Talent and its Employability grant PRE2022-104959 cofunded by the European Social Fund. S.T. acknowledges the funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 101034413. E.V. acknowledges support from the DISCOBOLO project funded by the Spanish Ministerio de Ciencia, Innovación y Universidades under grant PID2021-127289NB-I00. A.J.M. acknowledges support from the Swedish National Space Agency (Career grant 2023-00146). X.P.C. and M.M. acknowledge support from the Spanish Ministerio de Ciencia, Innovaciòn y Universidades under grants PID2021122842OB-C22 and PID2024-157964OB-C22; from the Xunta de Galicia and the European Union (FEDER Galicia 2021-2027 Program) Ref. ED431B 2024/21, ED431B 2024/02, and CITIC ED431G 2023/01. This work has made use of data from the European Space Agency (ESA) Gaia mission and processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, particularly the institutions participating in the Gaia Multilateral Agreement.","article_number":"146","title":"3I/ATLAS: In search of the witnesses to its voyage","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"lang":"eng","text":"3I/ATLAS is the third interstellar object discovered to date, following 1I/‘Oumuamua and 2I/Borisov. Its unusually high excess velocity and active cometary nature make it a key probe of the Galactic population of icy planetesimals. Understanding its origin requires its past trajectory through the Galaxy to be traced and the possible role of stellar encounters to be assessed, both as a potential origin and a perturber to its orbit. We integrated the orbit of 3I/ATLAS backward in time for 10 Myr, together with a sample of Gaia DR3 stars with high-quality astrometry and radial velocities, to identify close passages within 2 pc. We identify 93 nominal encounters, 62 of which are significant at the 2σ level. However, none of these encounters produced any meaningful perturbation. The strongest perturber Gaia DR3 6863591389529611264 at 0.30 pc and with a relative velocity of 35 km s−1, imparted only a velocity change of ∣Δv∣  ≃  5  ×  10−4 km s−1 to the orbit of 3I/ATLAS. Our results indicate that no stellar flybys within the past 10 Myr and 500 pc contained in Gaia DR3 can account for the present trajectory of 3I/ATLAS or be associated with its origin. We further show that 3I/ATLAS is kinematically consistent with a thin-disk population, despite its large peculiar velocity."}],"DOAJ_listed":"1","year":"2026","external_id":{"arxiv":["2509.07678"]},"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","month":"04","department":[{"_id":"LiBu"}],"_id":"21760","file_date_updated":"2026-04-28T13:06:00Z","ec_funded":1,"issue":"2","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae56ff","scopus_import":"1","has_accepted_license":"1","day":"20","ddc":["520"],"publication_status":"published","article_processing_charge":"Yes","citation":{"short":"X. Pérez-Couto, S. Torres Rodriguez, E. Villaver, A.J. Mustill, M. Manteiga, The Astrophysical Journal 1001 (2026).","ista":"Pérez-Couto X, Torres Rodriguez S, Villaver E, Mustill AJ, Manteiga M. 2026. 3I/ATLAS: In search of the witnesses to its voyage. The Astrophysical Journal. 1001(2), 146.","ama":"Pérez-Couto X, Torres Rodriguez S, Villaver E, Mustill AJ, Manteiga M. 3I/ATLAS: In search of the witnesses to its voyage. <i>The Astrophysical Journal</i>. 2026;1001(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae56ff\">10.3847/1538-4357/ae56ff</a>","mla":"Pérez-Couto, X., et al. “3I/ATLAS: In Search of the Witnesses to Its Voyage.” <i>The Astrophysical Journal</i>, vol. 1001, no. 2, 146, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae56ff\">10.3847/1538-4357/ae56ff</a>.","chicago":"Pérez-Couto, X., Santiago Torres Rodriguez, E. Villaver, A. J. Mustill, and M. Manteiga. “3I/ATLAS: In Search of the Witnesses to Its Voyage.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae56ff\">https://doi.org/10.3847/1538-4357/ae56ff</a>.","apa":"Pérez-Couto, X., Torres Rodriguez, S., Villaver, E., Mustill, A. J., &#38; Manteiga, M. (2026). 3I/ATLAS: In search of the witnesses to its voyage. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae56ff\">https://doi.org/10.3847/1538-4357/ae56ff</a>","ieee":"X. Pérez-Couto, S. Torres Rodriguez, E. Villaver, A. J. Mustill, and M. Manteiga, “3I/ATLAS: In search of the witnesses to its voyage,” <i>The Astrophysical Journal</i>, vol. 1001, no. 2. IOP Publishing, 2026."},"OA_type":"gold","volume":1001,"project":[{"_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413","call_identifier":"H2020"}],"date_published":"2026-04-20T00:00:00Z","OA_place":"publisher","date_updated":"2026-04-28T13:08:39Z","intvolume":"      1001","quality_controlled":"1","status":"public","author":[{"last_name":"Pérez-Couto","first_name":"X.","full_name":"Pérez-Couto, X."},{"id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","full_name":"Torres Rodriguez, Santiago","first_name":"Santiago","last_name":"Torres Rodriguez","orcid":"0000-0002-3150-8988"},{"full_name":"Villaver, E.","first_name":"E.","last_name":"Villaver"},{"first_name":"A. J.","full_name":"Mustill, A. J.","last_name":"Mustill"},{"first_name":"M.","full_name":"Manteiga, M.","last_name":"Manteiga"}],"oa":1,"file":[{"file_id":"21773","checksum":"c3daf49261a9933c079854c38eec316f","file_name":"2026_AstrophysicalJournal_PerezCouto.pdf","date_created":"2026-04-28T13:06:00Z","access_level":"open_access","file_size":2905627,"content_type":"application/pdf","date_updated":"2026-04-28T13:06:00Z","success":1,"relation":"main_file","creator":"dernst"}],"publisher":"IOP Publishing","date_created":"2026-04-26T22:01:46Z","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","arxiv":1,"oa_version":"Published Version","article_type":"original","PlanS_conform":"1"},{"has_accepted_license":"1","date_published":"2026-05-01T00:00:00Z","volume":1002,"OA_type":"gold","citation":{"ieee":"K. Inayoshi, J. Shangguan, X. Chen, L. C. Ho, and Z. Haiman, “The emergence of Little Red Dots from binary massive black holes,” <i>The Astrophysical Journal</i>, vol. 1002, no. 1. IOP Publishing, 2026.","apa":"Inayoshi, K., Shangguan, J., Chen, X., Ho, L. C., &#38; Haiman, Z. (2026). The emergence of Little Red Dots from binary massive black holes. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae548d\">https://doi.org/10.3847/1538-4357/ae548d</a>","chicago":"Inayoshi, Kohei, Jinyi Shangguan, Xian Chen, Luis C. Ho, and Zoltán Haiman. “The Emergence of Little Red Dots from Binary Massive Black Holes.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae548d\">https://doi.org/10.3847/1538-4357/ae548d</a>.","short":"K. Inayoshi, J. Shangguan, X. Chen, L.C. Ho, Z. Haiman, The Astrophysical Journal 1002 (2026).","mla":"Inayoshi, Kohei, et al. “The Emergence of Little Red Dots from Binary Massive Black Holes.” <i>The Astrophysical Journal</i>, vol. 1002, no. 1, 25, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae548d\">10.3847/1538-4357/ae548d</a>.","ista":"Inayoshi K, Shangguan J, Chen X, Ho LC, Haiman Z. 2026. The emergence of Little Red Dots from binary massive black holes. The Astrophysical Journal. 1002(1), 25.","ama":"Inayoshi K, Shangguan J, Chen X, Ho LC, Haiman Z. The emergence of Little Red Dots from binary massive black holes. <i>The Astrophysical Journal</i>. 2026;1002(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae548d\">10.3847/1538-4357/ae548d</a>"},"article_processing_charge":"Yes","publication_status":"published","day":"01","ddc":["520"],"file":[{"date_created":"2026-05-11T07:07:22Z","access_level":"open_access","file_id":"21853","checksum":"b4506dfef3dd6da335775071d8f2a0a6","file_name":"2026_AstrophysicalJour_Inayoshi.pdf","success":1,"date_updated":"2026-05-11T07:07:22Z","relation":"main_file","creator":"dernst","file_size":3041897,"content_type":"application/pdf"}],"author":[{"first_name":"Kohei","full_name":"Inayoshi, Kohei","last_name":"Inayoshi"},{"last_name":"Shangguan","first_name":"Jinyi","full_name":"Shangguan, Jinyi"},{"last_name":"Chen","full_name":"Chen, Xian","first_name":"Xian"},{"last_name":"Ho","first_name":"Luis C.","full_name":"Ho, Luis C."},{"orcid":"0000-0003-3633-5403","last_name":"Haiman","first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"oa":1,"status":"public","quality_controlled":"1","intvolume":"      1002","date_updated":"2026-05-11T07:09:12Z","OA_place":"publisher","PlanS_conform":"1","article_type":"original","oa_version":"Published Version","arxiv":1,"publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"date_created":"2026-05-10T22:02:14Z","publisher":"IOP Publishing","abstract":[{"lang":"eng","text":"Little red dots (LRDs) are a newly identified class of broad-line active galactic nuclei (AGNs) with a distinctive V-shaped spectrum characterized by red optical and blue UV continuum emission. Their high abundance at redshifts of z ∼ 6–8 and decline at lower redshifts suggest a transient origin. We propose that the spectral shape of LRDs originates from compact binary black hole systems, in which each black hole is surrounded by a mini-disk and embedded within a larger circumbinary disk. With a binary separation of ≲103 Schwarzschild radii, the Wien tail of a T ≃ 5000 K blackbody spectrum at the inner edge of the circumbinary disk produces the red optical emission, while the mini-disks power the UV continuum. Binary torques carve out a gap between the circumbinary disk and the mini-disks, setting the turnover wavelength of the V-shaped spectrum around the Balmer limit. This scenario naturally reproduces LRD spectra requiring only modest dust attenuation (AV ≲ 1 mag), resolving overestimated luminosities for LRDs in previous studies and alleviating a tension with the so-called Sołtan argument. This model predicts distinct spectral evolution as the binary orbit decays through binary disk interactions and gravitational-wave (GW) emission, linking early-stage “proto-LRD” binaries to the broader AGN population and late-stage “LRD descendants” to coalescing binaries detectable in GW experiments."}],"DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"The emergence of Little Red Dots from binary massive black holes","article_number":"25","acknowledgement":"We greatly thank Kenta Hotokezaka and Hanpu Liu for constructive discussions. K.I., J.S., X.C., and L.C.H. acknowledge support from National Natural Science Foundation of China (grant Nos. 12573015, 1251101148, 12233001, and 12473037), the Beijing Natural Science Foundation (grant No. IS25003), and the China Manned Space Program (grant No. CMS-CSST-2025-A09). J.S. is also supported by “The Fundamental Research Funds for the Central Universities, Peking University” (grant No. 7100604896). Z.H. acknowledges support by US NSF grant AST-2006176 and by NASA grant Nos. 80NSSC24K0440 and 80NSSC22K0822.","month":"05","type":"journal_article","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2505.05322"]},"year":"2026","_id":"21844","department":[{"_id":"ZoHa"}],"scopus_import":"1","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae548d","file_date_updated":"2026-05-11T07:07:22Z"},{"language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","publisher":"IOP Publishing","date_created":"2026-05-17T22:02:10Z","article_type":"original","PlanS_conform":"1","arxiv":1,"oa_version":"Published Version","intvolume":"      1003","quality_controlled":"1","OA_place":"publisher","date_updated":"2026-05-18T08:18:39Z","author":[{"full_name":"Wang, Bingjie","first_name":"Bingjie","last_name":"Wang"},{"full_name":"Leja, Joel","first_name":"Joel","last_name":"Leja"},{"full_name":"Katz, Harley","first_name":"Harley","last_name":"Katz"},{"last_name":"Inayoshi","first_name":"Kohei","full_name":"Inayoshi, Kohei"},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter","first_name":"Pieter"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"Labbé","full_name":"Labbé, Ivo","first_name":"Ivo"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"last_name":"Nelson","full_name":"Nelson, Erica J.","first_name":"Erica J."}],"oa":1,"file":[{"file_id":"21891","file_name":"2026_AstrophysicalJourn_Wang.pdf","checksum":"ee9ebc8ae2304fec04f24b82ebaac8bc","date_created":"2026-05-18T08:17:26Z","access_level":"open_access","content_type":"application/pdf","file_size":2584417,"success":1,"date_updated":"2026-05-18T08:17:26Z","relation":"main_file","creator":"dernst"}],"status":"public","OA_type":"gold","volume":1003,"ddc":["520"],"day":"01","publication_status":"published","article_processing_charge":"Yes","citation":{"ieee":"B. Wang <i>et al.</i>, “The missing hard photons of Little Red Dots: Their incident ionizing spectra resemble massive stars,” <i>The Astrophysical Journal</i>, vol. 1003, no. 1. IOP Publishing, 2026.","chicago":"Wang, Bingjie, Joel Leja, Harley Katz, Kohei Inayoshi, Nikko J. Cleri, Anna De Graaff, Raphael E. Hviding, et al. “The Missing Hard Photons of Little Red Dots: Their Incident Ionizing Spectra Resemble Massive Stars.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae5bab\">https://doi.org/10.3847/1538-4357/ae5bab</a>.","apa":"Wang, B., Leja, J., Katz, H., Inayoshi, K., Cleri, N. J., De Graaff, A., … Nelson, E. J. (2026). The missing hard photons of Little Red Dots: Their incident ionizing spectra resemble massive stars. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae5bab\">https://doi.org/10.3847/1538-4357/ae5bab</a>","ista":"Wang B, Leja J, Katz H, Inayoshi K, Cleri NJ, De Graaff A, Hviding RE, Van Dokkum P, Greene JE, Labbé I, Matthee JJ, Mcconachie I, Naidu RP, Nelson EJ. 2026. The missing hard photons of Little Red Dots: Their incident ionizing spectra resemble massive stars. The Astrophysical Journal. 1003(1), 10.","ama":"Wang B, Leja J, Katz H, et al. The missing hard photons of Little Red Dots: Their incident ionizing spectra resemble massive stars. <i>The Astrophysical Journal</i>. 2026;1003(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae5bab\">10.3847/1538-4357/ae5bab</a>","mla":"Wang, Bingjie, et al. “The Missing Hard Photons of Little Red Dots: Their Incident Ionizing Spectra Resemble Massive Stars.” <i>The Astrophysical Journal</i>, vol. 1003, no. 1, 10, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae5bab\">10.3847/1538-4357/ae5bab</a>.","short":"B. Wang, J. Leja, H. Katz, K. Inayoshi, N.J. Cleri, A. De Graaff, R.E. Hviding, P. Van Dokkum, J.E. Greene, I. Labbé, J.J. Matthee, I. Mcconachie, R.P. Naidu, E.J. Nelson, The Astrophysical Journal 1003 (2026)."},"date_published":"2026-05-01T00:00:00Z","has_accepted_license":"1","file_date_updated":"2026-05-18T08:17:26Z","scopus_import":"1","doi":"10.3847/1538-4357/ae5bab","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"_id":"21882","department":[{"_id":"JoMa"}],"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"year":"2026","external_id":{"arxiv":["2508.18358"]},"type":"journal_article","month":"05","article_number":"10","acknowledgement":"B.W. thanks Michael Eracleous for valuable discussions. B.W. and J.L. acknowledge support from JWST-GO-04233.009. B.W. also acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51592.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under the contract NAS 5-26555. K.I. acknowledges support from the National Natural Science Foundation of China (12573015, W2532003), the Beijing Natural Science Foundation (IS25003), and the China Manned Space Program (CMS-CSST-2025-A09). R.E.H. acknowledges support by the German Aerospace Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.”\r\n\r\nThis 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 # 1433, 2561, 4106, 4233, 5224, 6585. The specific observations analyzed can be accessed via DOI: 10.17909/9hpc-nc45. Computations for this research were performed on the Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar supercomputer; and on computational resources managed and supported by Princeton Research Computing, a consortium of groups including the Princeton Institute for Computational Science and Engineering (PICSciE) and Research Computing at Princeton University. Some of the stellar spectra are retrieved from the POLLUX database (pollux.oreme.org) operated at LUPM (Université de Montpellier—CNRS, France) with the support of the PNPS and INSU. This publication made use of the NASA Astrophysical Data System for bibliographic information.","DOAJ_listed":"1","abstract":[{"lang":"eng","text":"The nature of little red dots (LRDs) has largely been investigated through their continuum emission, with lines assumed to arise from a broad-line region. In this paper, we instead use recombination lines to infer the intrinsic properties of the central engine. Our analysis first reveals a tension between the ionizing properties implied from Hα and He ii λ4686. The high Hα EWs require copious H-ionizing photons, more than the bluest active galactic nucleus (AGN) ionizing spectra can provide. In contrast, He ii emission is marginally detected, and its low EW is, at most, consistent with the softest AGN spectra. The low He ii/Hβ (∼10−2, <20×  local AGN median) further points to an unusually soft ionizing spectrum. We extend our analysis to dense gas envelopes (quasi-star/black-hole star) and find that hydrogen recombination lines become optically thick and lose diagnostic power, but He ii remains optically thin and a robust tracer. Photoionization modeling with Cloudy rules out standard AGN accretion disk spectra. Alternative explanations include exotic AGN with red rest-optical emission, high average optical depth (>10) from gas/dust, and soft ionizing spectra with abundant H-ionizing photons, consistent with, e.g., a cold accretion disk or a composite of AGN and stars. The latter is an intriguing scenario since high hydrogen densities are highly conducive for star formation, and nuclear star clusters are found in the vicinity of local massive black holes. While previous studies have mostly focused on features dominated by the absorbing hydrogen cloud, the He ii-based diagnostic proposed here represents a crucial step toward understanding the central engine of LRDs."}],"title":"The missing hard photons of Little Red Dots: Their incident ionizing spectra resemble massive stars","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"department":[{"_id":"JoMa"}],"_id":"21930","file_date_updated":"2026-06-02T08:46:08Z","doi":"10.3847/1538-4357/ae5e4c","issue":"2","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"scopus_import":"1","acknowledgement":"\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy\r\nDanielle A. Berg, Rohan P. Naidu, John Chisholm, Hakim Atek, Seiji Fujimoto, Vasily Kokorev, Lukas J. Furtak, Chiaki Kobayashi, Daniel Schaerer, Angela Adamo, Qinyue Fei, Damien Korber, Jorryt Matthee, Rui Marques-Chaves, Zorayda Martinez, Kristen. B. W. McQuinn, Julian B. Muñoz, Pascal A. Oesch, Alberto Saldana-Lopez, Daniel P. Stark, Mabel G. Stephenson, and Tiger Yu-Yang HsiaoHide full author list\r\n\r\nPublished 2026 May 20 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal, Volume 1003, Number 2\r\nCitation Danielle A. Berg et al 2026 ApJ 1003 112\r\nDOI 10.3847/1538-4357/ae5e4c\r\n\r\nDownloadArticle PDFDownloadArticle ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nDownload PDFDownload ePub\r\nArticle metrics\r\n173 Total downloads\r\n\r\nShare this article\r\nArticle information\r\nAbstract\r\nWe present the discovery of extreme nitrogen enrichment by Wolf Rayet nitrogen (WN) stars in the metal-poor (∼10%Z⊙), lensed, compact (Reff ∼ 20 pc) galaxy RXCJ2248 at z = 6.1, revealed by unprecedentedly deep JWST/NIRSpec medium-resolution spectroscopy from the GLIMPSE-D Survey. The exquisite signal-to-noise ratio reveals multiple high-ionization nebular lines and broad Balmer and [O iii] components (FWHM ∼700–3000 km s−1). We detect broadened He ii λ1640 and λ4687 (FWHM ∼ 530 km s−1) and strong N iii λ4642 emission consistent with a population of WN stars, making RXCJ2248 the most distant galaxy with confirmed Wolf Rayet (WR) features to date. We measure the multiphase nebular density across five ions, the direct-method metallicity (\r\n), and a nonuniform elemental enrichment pattern of extreme N/O enhancement (\r\n from N+, N+2, and N+3) but suppressed C/O relative to empirical C/N trends. We show that this abundance pattern can be explained by enrichment from a dual-burst with a low WR carbon/WN ratio, as expected at low metallicities. Crucially, these signatures can only arise during a brief, rare evolutionary window shortly after a burst (∼3–6 Myr), when WN stars dominate chemical feedback but before dilution by later yields (e.g., supernovae). The observed frequency of strong N emitters at high−z implies a ∼50 Myr burst duty cycle, suggesting that N/O outliers may represent a brief but ubiquitous phase in the evolution of highly star-forming early galaxies. The WN detection in RXCJ2248, therefore, provides the first direct evidence of WR-driven nitrogen enrichment in the first billion years of the Universe and a novel timing argument for the bursty star formation cycles that shaped galaxies at cosmic dawn.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nA key tracer of galaxy evolution is the change in their chemical composition over time. The metallicity of a galaxy is a sensitive observational diagnostic of its past star formation history and present-day evolutionary state given that metallicity increases with each successive generation of massive star yields (e.g., M. Tosi 1988; J.-R. Roy & D. Kunth 1995; D. A. Berg et al. 2019; R. Maiolino & F. Mannucci 2019). Oxygen is an important tracer of metallicity because it is the most abundant element in the Universe after H and He and is convenient to observe, with ubiquitous emission lines from H ii regions in the rest-frame optical regime. While O emission in dwarf and spiral galaxies has been widely observed in the rest-frame optical and UV (e.g., R. C. Kennicutt 1992; Y. I. Izotov & T. X. Thuan 1999; L. van Zee & M. Haynes2006; D. A. Berg et al. 2012, 2016, 2019; P. Senchyna et al. 2017; N. S. J. Rogers et al. 2022), the N emission in these same galaxies has been predominantly traced only in the optical through the low-ionization [N ii] λλ6550,6585 emission lines. In general, there is a surprising dearth of detections of the high-ionization N emission counterparts in local galaxies, totaling less than 10 galaxies with significant detections of either N iv] λλ1483,1486 or N iii] λ1750 (e.g., M. Mingozzi et al. 2022; Z. Martinez et al. 2025). However, with the advent of JWST, there is a growing prevalence of z ≳ 5 galaxies with extreme properties, including intense UV N emission (e.g., A. J. Bunker et al. 2023; Y. Isobe et al. 2023; M. Castellano et al. 2024; T. Y.-Y. Hsiao et al. 2024; X. Ji et al. 2024; R. Marques-Chaves et al. 2024; D. Schaerer et al. 2024; M. Curti et al. 2025a; Y. Harikane et al. 2025a; R. P. Naidu et al. 2026; M. W. Topping et al. 2025b).\r\n\r\nThe first noted, and one of the most distant, examples of extreme rest-frame UV N emission comes from the spectroscopically confirmed z = 10.6 galaxy, GN-z11. JWST spectra of GN-z11 revealed surprisingly strong N iv] λλ1483,1486 and N iii] λ1750 emission (e.g., A. J. Bunker et al. 2023) that corresponds to supersolar nitrogen-to-oxygen (N/O) enrichment (\r\n; e.g., A. J. Cameron et al. 2023). Subsequently, enhanced N/O has been reported in a number of high−z galaxies, including GDS 3073 (z = 5.55; X. Ji et al. 2024), RXCJ2248-ID (z = 6.10; M. W. Topping et al. 2024), A1703-zd6 (z = 7.04; M. W. Topping et al. 2025b), CEERS-1019 (z = 8.68; R. Marques-Chaves et al. 2024), GNz9p4 (z = 9.38; D. Schaerer et al. 2024), GHZ9 (z = 10.15; L. Napolitano et al. 2025), GHZ2 (z = 12.34; M. Castellano et al. 2024), and MoM-z14 (z = 14.44; R. P. Naidu et al. 2026). For a review of nitrogen line detections, see D. P. Stark et al. (2025). Such strong nebular N+3 emission requires a relatively hard ionizing radiation field (≳47.4 eV), where models of massive stars predict few photons. On the other hand, N+2 has a lower ionization potential (∼29.6 eV), but statistically significant detections are strikingly rare in integrated galaxy spectra (e.g., D. A. Berg et al. 2018; M. Mingozzi et al. 2022; A. J. Bunker et al. 2023; P. Senchyna et al. 2024) and are only expected to be strong at the highest possible nebular temperatures (∼2.5 × 104 K). Furthermore, the timing of the incredibly high N/O abundances reported for the high-redshift UV N emitters just a few 100 Myr after the Big Bang is unexpected.\r\n\r\nThe discovery of significant, rapid nitrogen enhancement so early in the Universe was surprising because it contradicts our longstanding understanding of N production. In typical chemical evolution modeling, some nitrogen enrichment can occur early on via core collapse supernova (CCSN), but substantial nitrogen enrichment only occurs 100 s of megayears after the onset of star formation via asymptotic giant branch (AGB) stars (e.g., F. Vincenzo et al. 2019; C. Kobayashi et al. 2020). Thus, alternative, faster enrichment methods are needed to explain substantial nitrogen enrichment in early galaxies. As a result, the necessary ionizing flux and conditions to produce the unexpectedly strong N+3 and N+2 emission observed in galaxies beyond z ∼ 5 have been attributed to more extreme sources, such as active galactic nuclei (AGN; R. Maiolino et al. 2024), Wolf Rayet (WR) stars (e.g., P. Senchyna et al. 2024; K. Watanabe et al. 2024; M. L. P. Gunawardhana et al. 2025), globular cluster precursors (e.g., C. Charbonnel et al. 2023; X. Ji et al. 2026), super star clusters (e.g., M. Pascale et al. 2023), very massive stars (VMSs: M⋆ > 102 M⊙; e.g., J. S. Vink 2023; Y. Shi et al. 2026), or supermassive stars (M⋆ > 103 M⊙; e.g., C. Charbonnel et al. 2023; C. Nagele & H. Umeda 2023), tidal disruption events (e.g., A. J. Cameron et al. 2023; K. Watanabe et al. 2024), and more.\r\n\r\nMost of our understanding of WR stars has been built from observations of individual resolved stars in a handful of galaxies in the Local Group, with almost no direct spectroscopic evidence for the prevalence of WR stars in more distant galaxies. To date, only two systems at Cosmic Noon (z ≈ 2–3) have confirmed signatures of WR stars: MARTA-4327 at z = 2.224 (hereafter, M4327; M. Curti et al. 2025b) and the Sunburst Arc at z = 2.37 (T. E. Rivera-Thorsen et al. 2024). Extending such detections to earlier cosmic epochs is crucial for understanding the role of massive stars in shaping the chemical evolution of galaxies in the first Gyr.\r\n\r\nHere, we investigate the z = 6.1 lensed galaxy RXCJ2248-ID3. RXCJ2248-ID was first identified by F. Boone et al. (2013), I. Balestra et al. (2013), and A. Monna et al. (2014) and discovered to be a high-ionization, compact, metal-poor, N-enhanced galaxy by R. Mainali et al. (2017), K. B. Schmidt et al. (2017), and M. W. Topping et al. (2024). We present extremely deep JWST/NIRSpec observations of RXCJ2248-ID3 that provide the highest-redshift spectroscopic evidence of WR nitrogen (WN) stars to date, which provide a physically consistent mechanism driving its extreme nitrogen enrichment (M. W. Topping et al. 2024). The remainder of this paper is organized as follows. The observations and data reduction are briefly described in Section 2.1, followed by a description of the emission-line fits, including the broad lines related to the WR feedback, in Section 2.2. We present the discovery of WN stars at z ∼ 6 via their spectral signatures in Section 3. We determine new nebular properties and O, C, N, and Si abundances in Section 4.3 and compare them to populations of both low- and high-redshift galaxies. We discuss the source of N enrichment in the early Universe and subsequently estimate mass production and timing arguments in Section 5. Finally, we present our conclusions in Section 6. Throughout this work, we adopt cosmological parameters of H0 = 70 km s−1 Mpc−1, Ωm = 0.30, and ΩΛ = 0.7 and the solar abundance pattern from M. Asplund et al. (2021).\r\n\r\n2. JWST/NIRSpec Spectra\r\nRXCJ2248 is a galaxy at z ∼ 6.1 that is lensed into multiple images by the Abell S1063 cluster (α = 22:48:44.13, δ =−44:31:57.50) at a redshift of z = 0.348. We present an analysis of the brightest image, RXCJ2248-ID3 (J = 25.0), which has a magnification of μ ∼ 7 (L. Furtak et al. 2025). RXCJ2248-ID was discovered as a z ∼ 6 candidate (F. Boone et al. 2013; A. Monna et al. 2014) using the 16-band HST photometry of the CLASH Survey and spectroscopically confirmed via VIsible Multi-Object Spectrograph (VIMOS)/VLT observations by I. Balestra et al. (2013). RXCJ2248-ID3 was soon found to be an exciting extreme emission-line galaxy via ground-based spectroscopy (R. Mainali et al. 2017), with strong detections of high-ionization emission such as O iii] λλ1661,1666 and C ivλλ1548,1550 but no He ii, suggesting star formation as the ionizing source rather than an AGN.\r\n\r\nThe early spectra of RXCJ2248-ID3 motivated further rest-UV+optical study with JWST/NIRSpec by M. W. Topping et al. (2024). This work performed direct metallicity calculations to show that RXCJ2248-ID3 is one of the most extreme N/O-enhanced (), metal-poor () galaxies, with high-ionization ([O iii] λ5008/[O ii] λ3728 = 184) and high nebular density (6.4 × 104 ≤ ne(cm−3) ≤3.1 × 105). They also used spectral energy distribution (SED) fitting with a constant star formation history to characterize its low stellar mass (M⋆ ∼ 108 M⊙) and the young-massive star population (∼2 Myr) of RXCJ2248. M. W. Topping et al. (2024), therefore, suggest that the N/O enrichment may be due to a short-lived phase that many z > 6 bursty galaxies experience. In this paper, we build on the work of M. W. Topping et al. (2024) with new, extraordinarily deep rest-optical JWST/NIRSpec observations of RXCJ2248-ID3 from the GLIMPSE-D Survey, a Director’s Discretionary Time (DDT) follow-up program described below.\r\n\r\n2.1. Observations and Reduction\r\nThe work presented here uses both the rest-UV JWST/NIRSpec archival spectra from JWST PID 2478 (PI Stark) and new rest-optical JWST/NIRSpec spectra from the GLIMPSE-D Survey, which is an extension of the GLIMPSE Survey. Properties of RXCJ2248-ID and observation details are presented in Table 1.\r\n\r\nTable 1. Properties of RXCJ2248-ID3\r\n\r\nJWST/NIRSpec Observations\r\nGrating/Filter\t(s)\tPI/PID\r\nG140M/F100LP\t6215\tStark/2478\r\nG235M/F170LP\t1576\tStark/2478\r\nG395M/F290LP\t107,228\tFujimoto & Naidu/9223\r\nMeasured Properties\r\nProperty\tValue\tReferences\r\nR.A.\t+22:48:45.81\tThis work\r\nDecl.\t−44:32:14.95\tThis work\r\nz\t6.1025 ± 0.0013\tThis work\r\nμ\t6.8877\tL. Furtak et al. (2025)\r\nReff (pc)\t\tA. Claeyssens (2025)\r\nM⋆ (M⊙)\t\tA. Claeyssens (2025)\r\nΣ⋆ (M⊙ pc−2)\t\tA. Claeyssens (2025)\r\nSFRHα (M⊙ yr−1)\t3.2\tThis work, Section 5.3\r\nSFRSED,1Myr\t4.7\tA. Claeyssens (2025)\r\nSFRSED,10Myr\t4.1\tA. Claeyssens (2025)\r\nΣSFR (M⊙ yr−1 kpc−2)\t1.34 × 103\tThis work\r\ntage (Myr)\t\tA. Claeyssens (2025)\r\n12+log(O/H)\t7.753 ± 0.025\tThis work, Section 4.3.1\r\nlog(N/O)\t−0.391 ± 0.037\tThis work, Section 4.3.2\r\nNote. Top: JWST/NIRSpec observations of RXCJ2248-ID3, including archival observations from PID 2478 (PI: Stark) and very deep GLIMPSE-D observations from PID 9223 (PI: Fujimoto & Naidu). Columns (1)–(3) list the grating/filter, exposure time, and principle investigator/PID. Bottom: Measured global properties of RXCJ2248-ID3. The R.A. and decl. are the extraction coordinates for RXCJ2248-ID3. The redshift was determined from the GLIMPSE-D spectrum emission lines. GLIMPSE imaging was used to determine the lensing model magnification, μ. Effective radius of the RXCJ2248-ID3 clump, stellar mass, and current massive star population age are from the SED modeling of A. Claeyssens (2025), while the SFR was determined from both the SED fitting and the narrow-component, collisions-corrected Hα flux (see Section 5.3), all corrected for the lensing factor. The star formation rate surface density was determined using the SFRHα. The metallicity and relative N/O abundance were determined using the direct method.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe GLIMPSE Survey is a large Cycle 2 JWST program (PID 3293; PIs Atek & Chisholm) that performed ultradeep NIRCam imaging (∼30.8 mag at 5σ over 0.8–5 μm) in seven broadband and two medium-band filters of the lensing cluster Abell S1063 (H. Atek et al. 2025). A. Claeyssens (2025) performed size and photometric measurements of RXCJ2248-ID in the different multiple images. The SED fitting was performed with the Bayesian Analysis of Galaxies for Physical Inference and Parameter Estimation (BAGPIPES; A. C. Carnall et al. 2018) code with Binary Population and Spectral Synthesis (BPASS v2.14, J. J. Eldridge et al. 2017) stellar population synthesis burst models and cloudy v23.01 photoionization models (M. Chatzikos et al. 2023; C. M. Gunasekera et al. 2023). Priors were used to be physically consistent with the source, i.e., high-ionization parameter (), low extinction (Av < 0.5 mag), low metallicity (Z < 0.4 Z⊙), and bursty star formation (τ = 1 Myr, i.e., close to a single burst, or τ = 10 Myr). The resulting best fit has a young age ( Myr) and low stellar mass of but within a compact size of pc such that the stellar mass surface density is . This value is akin to the highest densities found in globular clusters, similar to the ones reported for young star clusters and clumps at high redshift (A. Claeyssens et al. 2025; M. Messa et al. 2026), and broadly consistent with the conclusions presented in M. W. Topping et al. (2024).\r\n\r\nSubsequent medium-resolution (R ∼ 1000) spectra of RXCJ2248-ID3 were obtained as part of the follow-up GLIMPSE-D Survey: JWST DDT Program 9223 (PIs Fujimoto & Naidu) targeting a Pop III candidate in S. Fujimoto et al. (2025) using NIRSpec Multi-Object Spectroscopy (MOS) with the G395M grating and F290LP filter. As part of this program, RXCJ2248-ID3 was observed for a total of 13 exposures using a 3-point nod pattern and NRSIRS2 readout, totaling ∼30 hr of integration. The MSA slit positions covering RXCJ2248-ID3 of the three pointings are shown in Figure 1.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. JWST/NIRSpec MSA slits targeting RXCJ2248-ID3 for each of the three exposures in the GLIMPSE-D program. The two pointings that are closely aligned (solid purple regions) have the same wavelength coverage, while the pointing offset to the lower left (dashed region) has somewhat reduced blue coverage. All three pointings were used in the spectrum coaddition.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nWe augment the rest-optical GLIMPSE-D data with archival rest-far-UV G140M/F100LP and rest-near-UV G235M/F170LP observations from PID 2478 (PI Stark), covering the rest-frame ∼1400–4000 Å range. This program also observed the G395M/F290LP setting, but we only use the significantly deeper GLIMPSE-D G395M observations here. Multiple images of RXCJ2248 were identified and observed in program #2478. M. W. Topping et al. (2024) utilized these data by coadding the spectra of the individual images. In contrast, only the brightest image (ID3) was observed in the GLIMPSE-D Survey. To ensure consistency, we therefore restricted our analysis to the G140M and G235M spectra of ID3 obtained in program #2478. As a result, our G140M and G235M measurements are not directly comparable to those presented by M. W. Topping et al. (2024).\r\n\r\nThe data were reduced using v0.9.8 of the msaexp pipeline (G. Brammer 2022), following the standard routines described in A. de Graaff et al. (2025), K. E. Heintz et al. (2025), and F. Valentino et al. (2025). Briefly, level-2 calibrated products from MAST are subject to a series of custom corrections that account for, e.g., 1/f noise, bar vignetting, and detector bias. We used the “local” nodded background subtraction. The 2D spectra were drizzled onto a common wavelength grid and 1D spectra were optimally extracted using a profile model that accounts for, e.g., the wavelength-dependent PSF and offsets from the nominal position expected from the catalog. Line centers were measured for the strongest emission lines in the G395M spectrum (i.e., Hδ, Hγ, [O iii] λ4364, Hβ, [O iii] λλ4960,5008, He iλ5877, Hα, He iλ7067) and used to determine a redshift of z = 6.1025 ± 0.0013. Note that the bluest portion of the G395M tends to favor a slightly lower redshift (i.e., z ∼ 6.1000), while the reddest portion favors a slightly higher redshift (i.e., z ∼ 6.1034). The three individual 1D extracted spectra were then normalized to the common continuum flux scale of the first spectrum at rest-wavelengths of ∼6000–62000 Å prior to coadding. Spectral coaddition was performed as a weighted average using the inverse variance as the weight.\r\n\r\nThe resulting spectrum, shown in Figure 2, covers an observed wavelength range ∼2.8–5.5 μm, which corresponds to a rest-optical range of ∼3900–7740 Å. Note that the third pointing (dashed slits in Figure 1) has reduced wavelength coverage such that the blue end begins at ∼4265. The deep GLIMPSE-D spectra provide unparalleled signal-to-noise ratio (S/N; >5 at 5100 Å continuum) that enable rest-optical diagnostics typically reserved for nearby galaxies.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 2. JWST/NIRSpec rest-frame UV and optical spectra of RXCJ2248-ID3 highlighting the first object known with simultaneously detected emission from N+, N+2, and N+3 (see, also, M. W. Topping et al. 2024) and WR features. The second row shows the main emission UV emission-line detections from the archival G140M/F100LP spectrum, with significant detections of several high-ionization emission lines, including N iv] λλ1483,1486, C iv λλ1548,1550, He ii λ1640, O iii] λλ1661,1666, N iii] λ1750, and C iii] λλ1907,1909. The third row shows the blue end of the optical spectrum, where the left-hand panel shows the archival G235M/F170LP spectrum, which includes the low-ionization [O ii] λλ3727,3730 doublet. The right-hand panel of the third row and the fourth row shows the extremely high S/N GLIMPSE-D optical spectrum, enabling detections of several weak features. Note that some of the important features to this work are highlighted in the zoom in panels in the top row. In particular, the last panel reveals the most distant WR detection to date, with the λ4650 WR bump showing emission from N iii λ4642, indicative of nitrogen enrichment from WN stars. Note that not all of the labeled lines correspond to line detections.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n2.2. Emission-line Measurements\r\nIn order to perform a consistent analysis of our data, we measure emission-line fluxes for both the archival spectra and the new GLIMPSE-D spectra presented here. We fit neighboring emission lines simultaneously using Gaussian profiles with the lmfit package (M. Newville et al. 2015) in Python. Purely nebular lines (i.e., lines without possible stellar contributions or resonant effects) close in wavelengths were constrained to have the same full width at half-maximum (FWHM) velocity widths. Additionally, the relative wavelength spacing between lines was constrained to laboratory values and doublets with constant flux ratios set by atomic physics were constrained to their theoretical values, with small uncertainty allowances. The uncertainties on the line fluxes were estimated as the standard error derived from the least-squares minimization in lmfit, which considers the uncertainty on the Gaussian profile and linear continuum.\r\n\r\nBroad emission components are clearly visible at the base of some of the emission lines in the GLIMPSE-D spectrum of RXCJ2248-ID3. Such broad emission features can be produced by stellar winds, shocks, or turbulence. Since He iiλ1640 and λ4687 emission lines can be affected by stellar winds, we fit these features with an unconstrained Gaussian width. Using the jwst-msa package (A. de Graaff et al. 2024), we deconvolved all measured FWHMs with the modeled wavelength-dependent line spread function (LSF). We found the He ii lines to be broadened compared to purely nebular lines. For the He iiλ 4687 line, the velocity width is 528 ± 100 km s−1, which is more than two times broader than the narrow nebular Hβ component with vFWHM = 243 ± 25 km s−1.\r\n\r\nThe strongest rest-optical H (Hγ, Hβ, and Hα) and [O iii] (λ4364, λλ4960,5008) emission lines have complex profiles with both narrow and broad emission components. Such broad components may also be present in the rest-UV and fainter rest-optical emission lines, but none are obvious given the lower S/N of these emission features and/or underlying continuum. To fit these profiles, we tested three different multicomponent profile combination fits for the Hα + [N ii] complex. For all three fits, the narrow Hα and [N ii] λλ6550,6585 lines were fit by Gaussians with a single velocity width, but the broad component was fit with either: (1) a single Gaussian profile, (2) two Gaussian profiles, or (3) a single exponential profile. The single broad Gaussian profile fit had strong residuals near the center of the broad component, so did not provide a good fit to the observed emission profile. Both the double Gaussian profile and the exponential profile provided relatively good visual fits, but the double Gaussian fit had a lower reduced chi-squared ( vs ) and Bayesian inference criteria (BIC2Gauss = 36 versus (BICexp. = 87), and so was adopted as the better statistical fit.\r\n\r\nThe right panel of Figure 3 shows the best multicomponent fit to the Hα + [N ii] complex. Since all kinematically similar lines in the Balmer emission series arise from the same gas, we expect the Hβ and Hγ profiles to be well fit by scaling the Hα best fit. Therefore, we constrained the velocity widths of the Hβ and Hγ emission components to match the narrow + double broad Gaussian Hα fit, accounting for the wavelength-dependent LSF. We found excellent fit results, with similarly small reduced-χ2 and BIC values. This means that the H i lines are well fit by a profile with (1) a strong, narrow (∼250 km s−1) nebular component, (2) a moderate (∼20% of total flux), broad component (∼670 km s−1), and (3) a weak (∼10% of total flux), very broad (∼2530 km s−1) component.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Multicomponent emission-line fits to the GLIMPSE spectrum of RXCJ2248-ID for Hα λ6565 + [N II] λλ6549,6585 (left panels), Hβ λ4863 + [O III] λλ4960,5008 (middle panels), and Hγ λ4342 + [O III] λ4364 (right panels). When fit with single, narrow Gaussian components (e.g., purple and yellow filled Gaussians), all three line complexes show strong, broad component residual flux. The resulting best fit to each line is comprised of a single narrow Gaussian plus two broad Gaussians, where the relevant component velocity widths are tied together: The Hα λ6565 + [N ii] λλ6549,6585 complex fit provided the velocity width constraints for the H Balmer line narrow (purple Gaussians) and broad components (blue and green Gaussians) and, subsequently, the Hβ λ4863 + [O iii] λλ4960,5008 fit constrained the [O iii] narrow (yellow Gaussian) and broad (orange and red Gaussians) velocity widths that were then used in the Hγ λ4342 + [O iii] λ4364 fit. Note that additional faint lines (e.g., He i λ5017) were included in the fit in the middle panel. Careful accounting for the residual broad flux has a significant impact on the derived nebular reddening, temperature, metallicity, and N/O abundance.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nThe [O iii] λλ4960,5008 doublet lines are also well fit by a narrow Gaussian plus double Gaussian broad component profile, with the relative fluxes of each component constrained to the theoretical ratio. While the narrow-component FWHM was set to the velocity width of the narrow Balmer lines, convolved with the LSF, we allowed the FWHM of the two broad [O iii] components to vary freely and found widths of ∼890 km s−1 and ∼2980 km s−1, respectively. The similarity between the [O iii] and H i velocity widths of the broad components argues against emission from an AGN directly (where high densities cause collisional de-excitation of [O iii]) and is more consistent with stellar or AGN driven winds (e.g., Y. I. Izotov & T. X. Thuan 2008; G. Gräfener & J. S. Vink2015; G. Gräfener et al. 2017; C. J. Burke et al. 2021). Interestingly, the broad components of the H i lines compose a larger fraction of their total flux (∼20% and 10%, respectively) than [O iii] (∼10% and 5%, respectively).\r\n\r\nThe resulting fit to the Hβ + [O iii] λλ4960,5008 complex is shown in the middle panel of Figure 3 to be an excellent fit, with minimal residuals. The exquisite S/N of the GLIMPSE spectrum also reveals broad wings on the [O iii] λ4364 profile, as seen in the left panel of Figure 3. Therefore, we also applied the narrow Gaussian plus double Gaussian broad component profile to [O iii] λ4364, constraining the velocity widths to the values measured for [O iii] λλ4960,5008.\r\n\r\nDouble broad components with similar velocity widths (750 and 2500 km s−1, respectively) are seen in the z ∼ 0 extreme emission-line galaxies, J1044+0353 and J1418+2102, reported in D. A. Berg et al. (2021). However, each broad component observed in these nearby analogs only accounts for 1%–3% of the total H i flux. This sort of broad component emission from the Balmer H and [O iii] lines with widths (1000–2000 km s−1) and fractional fluxes of 1%–2% is commonly found in spectra of blue compact dwarf galaxies (BCDs; e.g., Y. I. Izotov et al. 2006, 2007). This suggests that bulk motion of the gas is typical in these metal-poor, bursty environments, but for a larger mass of gas in RXCJ2248-ID3.\r\n\r\nThe sensitive accounting of broad component emission afforded by the deep GLIMPSE-D spectra is important because even a small fraction of broad emission around H emission line can significantly affect the fit to weak lines such as [N ii] λλ6550,6585 (e.g., D. A. Berg et al. 2021). In RXCJ2248-ID, the broad components compose a significant fraction of the total H and [O iii] fluxes, and so are critical to properly measure not only the [N ii] λ6585 emission but also the [O iii] λ4364, Hβ, [O iii] λλ4960,5008, and Hα narrow-line fluxes. For this reason, we adopt the narrow-line fluxes from our best multicomponent fits for the remaining analysis; we reserve further investigation of the the broad emission for a forthcoming paper.\r\n\r\nAs noted above, the UV spectra do not have sufficient S/N to decompose narrow and possible broad components. As a result, density diagnostics and relative abundance ratios determined from UV line ratios may include contributions from multiple kinematic components. If the broad components arise from gas with distinct physical conditions, this could introduce systematic offsets. We test the level of bias possible due to broad component contamination of narrow-line fluxes by adopting the relative narrow and broad component profiles of [O iii] λ5008 as a template for collisionally excited lines. The broad component areas overlap with the narrow profile such that the broad components are responsible for 8.6% and 2.2% of the narrow-component flux, or 10.8% in total. We use this fraction to set the upper contamination limit of potential broad components to the UV emission lines and determine the impact on nebular density, temperature, and abundance calculations in Section 4.4.\r\n\r\n2.3. Reddening Correction\r\nThe observed Balmer decrement of the narrow Hα/Hβ lines is FHα/FHβ = 3.48, implying either a moderate amount of dust is present or collisional enhancement of Hα. This value disagrees with the results of M. W. Topping et al. (2024), who measured an observed decrement of 2.55 ± 0.05 that they found to be consistent with no dust attenuation. Similarly, A. Crespo Gómez et al. (2025) used high-resolution NIRSpec/G395H data to fit multiple component Balmer decrements for RXCJ2248-ID3, finding a narrow-component FHα/FHβ = 2.7 that is consistent with no attenuation, but broad- and very broad-component decrements of 4.3 and 6.6, respectively, that imply differential extinction. We too find higher FHα/FHβ ratios for the broad components, but the source of this increase is not clear; it could indicate higher dust in the broad component gas, as suggested by A. Crespo Gómez et al. (2025), or result from significant collisional enhancement of Hα.\r\n\r\nFortunately, the GLIMPSE-D spectrum provides a significant increase in S/N in the continuum, allowing for more robust fitting of broad components, including in the Hγ and [O iii] λ4364 and λ5008 lines. Fitting the broad components directly in the [O iii] lines offers the advantage over previous works that we do not need to correct for broad component contamination with differential extinction in our Te calculation. Furthermore, by fitting the broad components in Hγ we were able to examine the narrow-component Hβ/Hγ ratio, finding a decrement of FHβ/FHγ = 2.16 that is consistent with very little dust (see Table 2). Note that we do not consider the Hβ/Hδ ratio here because the Hδ line is not strong enough to robustly fit the broad components in a consistent manner with the profile fitting of the Hγ, Hβ, and Hα lines.\r\n\r\nTable 2. Rest UV+Optical Emission-Line Fluxes\r\n\r\nIon+Wavelength\tI(λ)/I(C iii])\tEW\r\n(Å)\t \t(Å)\r\nN iv] λ1483.33\t42.78 ± 1.61\t6.67\r\nN iv] λ1486.50\t102.0 ± 0.82\t15.9\r\nHe iiλ1640.42\t22.46 ± 197\t4.88\r\nO iii] λ1666.15\t85.84 ± 0.59\t18.9\r\nN iii] λ1750a\t38.59 ± 0.64\t9.18\r\nSi iii] λ1883.00\t5.01 ± 3.25\t1.32\r\nSi iii] λ1892.03\t8.25 ± 1.98\t2.21\r\nC iii] λ1906.68\t35.11 ± 0.31\t9.65\r\n[C iii] λ1908.73\t64.89 ± 0.25\t17.9\r\nIon+Wavelength\tI(λ)/I(Hβ)\tEW\r\n(Å)\t \t(Å)\r\n[O ii] λ3728a\t4.09 ± 2.05\t6.22\r\nHγ λ4341.66b\t47.41 ± 3.07\t73.8\r\n[O iii] λ4364.44b\t42.45 ± 1.92\t66.5\r\nHe i λ4472.73\t8.90 ± 0.39\t27.8\r\nN iii λ4641.94\t1.40 ± 0.20\t4.4\r\nHe ii λ4687.01\t1.33 ± 0.29\t4.2\r\n[Ar iv] λ4712.69c\t2.30 ± 0.27\t10.3\r\nHe i λ4714.46c\t1.91 ± 0.19\t3.0\r\n[Ar iv] λ4741.49\t4.10 ± 0.26\t13.0\r\nHβ λ4862.71b\t100.0 ± 4.4\t356\r\n[O iii] λ4960.29b\t230.5 ± 9.0\t877\r\n[O iii] λ5008.24b\t708.9 ± 27.5\t2791\r\nHα λ6564.60b,d\t331.8 ± 14.4\t1755\r\nHα λ6564.60b,e\t274.1 ± 11.9\t1457\r\n[N ii] λ6585.27\t7.08 ± 0.91\t12.8\r\n[S ii] λ6718.29\t0.68 ± 0.29\t4.78\r\n[S ii] λ6732.67\t0.81 ± 0.30\t4.74\r\nE(B − V)\t\t⋯\r\nFC III]\t11.58 ± 0.49\t⋯\r\nb\t6.94 ± 0.15\t⋯\r\nNotes. Reddening-corrected emission-line intensities of lines used in this analysis from the archival rest-UV and GLIMPSE rest-optical JWST/NIRSpec spectra for RXCJ2248-ID3. Note that no scaling was performed between the archival UV and GLIMPSE-D optical pointings (not needed for this work). Thus, UV fluxes are given relative to the FC III]λλ1907,09 × 100 and optical fluxes are given relative to FHβ × 100. The last three rows list the dust attenuation derived using the J. A. Cardelli et al. (1989) reddening law and the rest-frame C iii] λλ1907,09 and Hβ flux in units of 10−18 erg s−1 cm−2. Additionally, the fluxes reported here are for a single image of RXCJ2248 (ID3), whereas M. W. Topping et al. (2024) report fluxes for coadded spectra of multiple images. aNote that N iii] λ1750 and [O ii] λ3728 fluxes are the integrated values for the N iii] λλ1746,1748,1749,1752,1754 quintuplet and [O ii] λλ3727,3730 doublet, respectively. bEmission-line profile was best fitted with a narrow Gaussian and two broad Gaussian components; only the corrected narrow-line flux is listed here (see Section 2.2 and Figure 3). c[Ar iv] λ4713+He iλ4714 is a blended line profile at the observed resolution. Thus, the [Ar iv] λ4713 is determined by subtracting the He iλ4714 flux, which is predicted from the He i λ4473 flux. dUncorrected for collisional excitation. eCorrected for collisional excitation.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe reddening due to dust, characterized by E(B − V), was determined by comparing the observed Balmer decrements with the theoretical Balmer ratios assuming case B and an extinction law, for which we tested the parameterization from both J. A. Cardelli et al. (1989) and D. Calzetti et al. (2000). The E(B − V) value for a given Balmer ratio was determined iteratively until convergence, recomputing the H i theoretical ratio using the updated electron temperature from the reddening-corrected [O iii] λ4364/λ5008 flux ratio and density from the reddening-corrected N iv] λ1483/λ1487 flux ratio in each iteration. In this way, the reddening, electron temperature, and electron density were solved for simultaneously and consistently.\r\n\r\nA greater enhancement of the observed FHα/FHβ decrement than of the FHβ/FHγ decrement can arise under high-density conditions, where collisional excitation selectively enhances the lowest excited level (n = 2; requires lowest energy to excite), leading to higher Hα flux relative to Hβ and Hγ. To assess whether such an enhancement is physically plausible, we examined the Cloudy photoionization models (M. Chatzikos et al. 2023; C. M. Gunasekera et al. 2023) presented in Z. Martinez et al. (2025), which span a wide range of nebular densities (up to ne = 109 cm−3). For the nebular conditions determined in this work (i.e., Te, , Z, N/O; see Section 4), densities of ne ∼ 106 cm−3 are needed to produce the observed Hα enhancement while minimally affecting Hβ and Hγ. Although this density is roughly an order of magnitude higher than the values measured in M. W. Topping et al. (2024) and in this study (see Section 4.1 and Table 3), it could indicate that the interstellar medium (ISM) contains unresolved clumps of even higher density than the volume-weighted values probed by the density diagnostics used in this work. We, therefore, attribute the observed Hα excess to collisional enhancement.\r\n\r\nTable 3. Nebular Conditions and Abundances for RXCJ2248-ID3\r\n\r\nProperty\tIon. E\tUsed\tValue\r\n \t(eV)\t \t \r\nTemperatures:\t \t \r\nTe,high meas. (K)\t35.11–54.93\tne(N+3)\t1.97 ± 0.03 × 104\r\nTe,int. used (K)\t23.33–34.83\tD. R. Garnett (1992)\t1.81 ± 0.02 × 104\r\nTe,low used (K)\t13.62–35.11\tD. R. Garnett (1992)\t1.68 ± 0.02 × 104\r\nDensities:\t \t \t \r\nne(N+3) (cm−3)\t47.45–77.47\tTe,high\t\r\nne(Ar+3) (cm−3)\t40.74–59.81\tTe,high\t\r\nne(C+2) (cm−3)\t24.38–47.89\tTe,int.\t\r\nne(Si+2) (cm−3)\t16.35–33.49\tTe,int.\t\r\nne(S+) (cm−3)\t10.36–23.33\tTe,low\t\r\nO Abundances:\r\nO+/H+ (×10−5)\t13.62–35.11\tTe,low; ne(Si+2)\t0.186 ± 0.148\r\nO+2/H+ (×10−5)\t35.11–54.93\tTe,high; ne(Ar+2)\t5.473 ± 0.261\r\n \t \t7.753 ± 0.023\r\nIonization Parameters:\r\nlogUint.(O32)\t13.62–54.93\tne = 104 cm−3\t−1.24 ± 0.23\r\nlogUhigh(N43)\t29.60–77.47\tne = 105 cm−3\t−0.69 ± 0.10\r\nN Abundances:\r\nN+3/O+2\t47.45–77.47\tTe,high; ne(N+3)\t0.277 ± 0.043\r\nN+2/O+2\t29.60–47.45\tTe,high; ne(C+2)\t0.145 ± 0.070\r\nN+/O+\t14.53–29.60\tTe,low; ne(Si+2)\t0.367 ± 0.259\r\nICF(N+3/O+2)\t47.45–77.47\tTe,high; ne(N+3)\t1.542\r\nICF(N+2/O+2)\t29.60–47.45\tTe,high; ne(C+2)\t2.547\r\nICF(N+/O+)\t14.53–29.60\tTe,low; ne(Si+2)\t0.814\r\nlog(N/O)\t⋯\t⋯\t−0.368 ± 0.062\r\nlog(N/O)\t⋯\t⋯\t−0.434 ± 0.071\r\nlog(N/O)\t⋯\t⋯\t−0.525 ± 0.257\r\nlog(N/O)all\t⋯\t⋯\t−0.375 ± 0.056\r\n⋯\t⋯\t−0.390 ± 0.035\r\nC Abundance:\r\nC+2/O+2\t24.38–47.89\tTe,int; ne(C+2)\t0.107 ± 0.014\r\nICF(C+2/O+2)\t24.38–47.89\tTe,int; ne(C+2)\t1.498\r\nlog(C/O)\t \t \t−0.795 ± 0.052\r\nSi Abundance:\r\nSi+2/O+2\t16.35–33.49\tTe,low; ne(Si+2)\t0.005 ± 0.001\r\nICF(Si+2/O+2)\t16.35–33.49\tTe,low; ne(Si+2)\t3.507\r\nlog(Si/O)\t⋯\t⋯\t−1.781 ± 0.157\r\nNote. Ionic and total abundances for RXCJ2248-ID3. Column (1) lists the property, while Column (2) lists the associated ionization potential energy range (eV), Column (3) lists the temperature and/or density used in the calculation, and Column (4) provides the final values. All calculations reported here only used the narrow components when multicomponent fits were performed. Note that the temperatures for the intermediate- and low-ionization zones were inferred from Te,high using the Te–Te relationships of D. R. Garnett (1992). Two ionization parameters are reported for the O32 and N43 indicators from Z. Martinez et al. (2025). The oxygen abundance was determined using the archival [O ii] λ3728 detection and the new [O iii] λ5008 fit. N/O was determined using four different ion+ICF (from Z. Martinez et al. 2025) combinations: (1) optical N+/O+; (2) UV N+2/O+2; (3) UV N+3/O+2; and (4) combination (N++N+2+N+3)/(O++O+2). C/O and Si/O were determined from the archival UV emission lines only.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nAccordingly, we adopted the reddening derived from Hγ/Hβ, mag using J. A. Cardelli et al. (1989) (the D. Calzetti et al. (2000) value is similar at E(B − V) = 0.050 ± 0.1215 mag), and corrected all emission lines for the resulting (minimal) dust attenuation. We used the D. Calzetti et al. (2000) reddening law for the rest-UV emission lines (λ < 3200 Å) and the J. A. Cardelli et al. (1989) reddening law for the rest-optical emission lines (λ > 3200 Å). After applying the reddening correction, the Hα/Hβ ratio still shows a collisional excess of 0.204 above the theoretical value; we correct for this excess and report a final FHα = 1.985 × 10−17 erg s−1 cm−2.\r\n\r\nThe adopted reddening and dereddened line intensities are listed in Table 2 for all line fluxes used in this work. Note that rest-UV and rest-optical lines should not be compared or combined in line ratios. Since the rest-UV and rest-optical spectra were obtained during different observing runs with distinct pointings and strategies, we report the UV lines relative to FCIII]λλ1907,1909 × 100 and the optical lines relative to FHβ × 100, without applying any relative scalings between the two datasets.\r\n\r\n3. Wolf Rayet Stars at z = 6.1\r\nThe WR stage of massive star evolution is an important, short-lived phase that can have significant effects on the chemical composition of the local ISM. We provide a brief overview here (see, e.g., P. A. Crowther 2007, for a more thorough review). WR stars are massive stars that have entered the core He-burning phase and have lost their outer envelope either via strong stellar winds or due to binarity effects (i.e., stripping via Roche Lobe overflow or mergers). The first phase of WR stars occurs when the outer H layer has been ejected, revealing the H core-burning products such that their spectra are characteristically He and N rich but are H-poor. Such stars are known as nitrogen-type WR, or WN, stars, and are often identified by strong N iii, N iv, and N v emission lines, especially the broad optical “blue bump” near λ4650. The blue bump is a complex of features, including N iii λλ4634,4642, C iii λ4649,4667, Fe iii λ4660, and He ii λ4687. Subsequently, stars that are massive enough for core He-burning and for their winds to remove their outer He envelope and expose the produced C enter the WR carbon (WC) phase. WC stars also have strong, broad He ii emission and strong C and O emission, such that they are identified by the optical WR C iv λλ5803,5814 doublet (the “red bump”). As a result, the typically very strong winds of the WR phase can produce significant N enrichment during the WN phase and drive strong C ejection during the WC phase. After the WC phase, a WR-oxygen phase may ensue, but we forgo discussion of this phase here.\r\n\r\nThe rest-frame UV and optical spectra shown in Figure 2 can be used to characterize the WR nature of the stellar population in RXCJ2248-ID3. Both the UV and optical He ii emission features are kinematically broadened compared to the narrow nebular emission features in RXCJ2248-ID3, indicative of WR or VMS winds. F. Martins et al. (2023, 2025) have shown that young star-forming regions dominated by VMSs can be distinguished from WR stars using the morphology of the blue and red bumps. In particular, VMSs produce blue bumps with He ii λ4687 emission but little to no N iii emission and red bumps with narrow C iv λλ5803,5814 emission. Thus, strong detections of N iii in the blue bump favor a WN interpretation (e.g., F. Martins et al. 2023; D. A. Berg et al. 2024; T. E. Rivera-Thorsen et al. 2024).\r\n\r\nThe upper right-hand panel of Figure 2 highlights the blue bump spectral regime, showing weak, broad He ii and N iii λ4642 in RXCJ2248-ID3, both of which are characteristic of metal-poor WN stars. Just redward of the N iii λ4642 line in the blue bump (but blueward of [Fe iii]), a second less prominent emission feature is seen, but it is difficult to determine whether this is due to C iii or O ii emission, or both. Furthermore, the red C iv bump is not detected, suggesting little to no contributions from WC stars or VMSs in the spectrum. Thus, we only significantly detect the blue WR bump, suggesting that WN stars are likely present.\r\n\r\n4. Nebular Properties\r\nUsing the updated narrow-component emission-line fits presented in Section 2.2, we determined the nebular properties of RXCJ2248-ID3. Following D. A. Berg et al. (2021), we adopt the four-zone ionization model to account for the high-ionization emission observed. In this model, the ionization potential energy ranges of N+, S+2, O+2, and He+2 define the low-, intermediate-, high-, and very high-ionization zones, respectively. For all calculations, we use the PyNeb package in Python with the atomic data adopted in D. A. Berg et al. (2019), which includes a six-level atom model for oxygen in order to utilize the UV O iii] λ1666 line. Below, we determine temperatures and densities, although Te(O+2) and ne(N+3) were codetermined during the iterative reddening calculation (see Section 2.3) in Section 4.1, ionization parameters in Section 4.2, and abundances in Section 4.3.\r\n\r\nWe note that the UV spectra do not have sufficient S/N to decompose narrow and broad components following the same method as the optical lines. As a result, density diagnostics and abundances determined from UV lines may include contributions from multiple kinematic components, while optical temperatures, densities, and abundances are derived from narrow components alone. If the broad component arises from gas with distinct physical conditions, this could introduce systematic offsets. For this reason, we examine the potential impact of UV broad components in Section 4.4.\r\n\r\n4.1. Temperature and Density\r\nOne of the unique characteristics of RXCJ2248-ID3 is its large number of density-sensitive emission-line ratios. M. W. Topping et al. (2024) previously reported densities from the three UV line ratios of Si iii] λ1883/λ1892, characterizing the intermediate-ionization zone, C iii] λ1907/λ1909, characterizing the intermediate- to high-ionization zone, and N iv] λ1483/λ1486, characterizing the high- to very high-ionization zone. The new high-S/N optical spectra enables us to measure, for the first time, densities from the low-ionization [S ii] λ6717/6731 ratio and the high- to very high-ionization [Ar iv] λ4713/λ4741 ratio.\r\n\r\nWe use our narrow-component dereddened flux measurements to compute densities for all five line ratios and the high-ionization zone temperature from the [O iii] λ4364/λ5008 ratio. The high-ionization zones Te(O+2) and ne(N+3) were simultaneously determined during the iterative reddening calculation in Section 2.3 to account for the sensitivities of both diagnostics. If the low density limit was assumed instead (ne ≲ 102 cm−3), as is common practice at low-redshift, the observed [O iii] λ4364/λ5008 flux ratio would lead to unphysical temperatures (i.e., above the limit set by H cooling of ∼2.5 × 104 K). Thus, a physical and robust solution requires high densities to properly account for the reduced λ5008 flux due to collisional de-excitation. Furthermore, Z. Martinez et al. (2025) recently showed that densities derived from both optical and UV diagnostics underpredict the true volume-averaged density in multiphase, high-density systems, with more severe underprediction from the optical diagnostics. Therefore, it is necessary to use UV density diagnostics in high-density environments, though the true density will still be underestimated in multiphase gas (see, e.g., Figure 11 of Z. Martinez et al. 2025).\r\n\r\nFor the high-ionization zone, we found a Te(O+2) = 1.97 ±0.03 × 104 K and ne(N+3) cm−3, which is consistent with the density of ne(N+3) cm−3 reported by M. W. Topping et al. (2024), but lower than their temperature of 2.46 ± 0.26 × 104 K due to our broad component fits of both [O iii] λ4364 and λ5008. Adopting our Te(O+2) as the high-ionization temperature (Te,high), we then applied the Te–Te relations of D. R. Garnett (1992) to estimate the intermediate-ionization temperature (Te,int.) and low-ionization temperature (Te,low).\r\n\r\nThe determined temperatures were used for the subsequent density calculations in their respective ionization zones. Note that the [Ar iv] λ4713 and He i λ4714 lines are blended in the G395M grating. Therefore, we corrected the [Ar iv] λ4713 flux for the He i λ4714 contribution, predicting the He i λ4714 flux from the measured He i λ4473 flux and the theoretical He i λ4714/λ4473 ratio (∼0.21 for the conditions in RXCJ2248-ID). The resulting densities, all of which fall within their respective diagnostic ranges, and temperatures are reported in Table 2.\r\n\r\nRemarkably, RXCJ2248-ID3 is one of few galaxies, and the only galaxy yet at high redshifts, to have significant (>3σ) electron density measurements from five different ions that span a large ionization range (∼10–77 eV). Furthermore, the densities in RXCJ2248-ID3 appear to be organized into an interesting nebular stratification. The UV emission lines trace the densest gas, with ne(N+3) = 2.65 × 105 cm−3 in the highest-ionization gas, followed by ne(C+2) = 7.94 × 104 cm−3 and ne(Si+2) = 4.77 × 104 cm−3. In contrast, the optical high-ionization lines are emitted from regions of lower densities: the optical [Ar iv] diagnostic has an overlapping ionization energy range with the UV N iv] diagnostic but a density that is an order of magnitude lower.\r\n\r\nThere are two possible interpretations of the measured array of densities. First, since the UV lines also have higher excitation energies, they could originate preferentially from hotter, denser clumps. This would imply a strongly inhomogeneous ISM, in which compact, high-pressure structures dominate the UV line emission while somewhat more diffuse gas produces much of the optical emission. Alternatively, the multiphase ISM may span a smaller dynamic range of densities than we measure due to the suppression of the optical diagnostics. Z. Martinez et al. (2025) showed that for an ISM with a mix of low- (e.g., 103 cm−3) and high-density gas (e.g., 105 cm−3) that has a true volumetric density that is somewhere in between, the low-ionization optical diagnostics will always be significantly biased low, close to the low-density gas value, until the fraction of high-density gas is very high (e.g., >95%). This effect occurs when ne-diagnostic line ratios have low critical densities (e.g., ne,crit([S ii])≈2 × 103–5 × 103 cm−3), such that emission from the high-density gas is collisionally suppressed beyond detection. The magnitude of this effect decreases with increasing critical density such that [S ii] is significantly affected, [Ar iv] is moderately affected (ne,crit ≈ 2 × 104–2 × 105 cm−3), and the UV Si iii], C iii], and N iv] (ne,crit ≈ 5 × 104–5 × 1010 cm−3) are minimally affected, albeit still biased low. In this scenario, there would still be density stratification, but with smaller differences.\r\n\r\nAll together, the nebular diagnostics in RXCJ2248-ID3 support a picture of a multiphase nebula with density and temperature stratification, likely reflecting a clumpy ISM shaped by the feedback and local radiation field variations of bursty star formation (see, also, N. Choustikov et al. 2025; Y. Harikane et al. 2025b; M. Usui et al. 2025). This picture is also consistent with the density stratification that has been reported for dwarf galaxies both near and far (e.g., B. L. James et al. 2016; D. A. Berg et al. 2021; M. Mingozzi et al. 2022; X. Ji et al. 2024; M. W. Topping et al. 2024), but with typical densities increasing with redshift (e.g., Y. Isobe et al. 2023; Abdurro’uf et al. 2024; Z. Martinez et al. 2025; M. W. Topping et al. 2025a).\r\n\r\n4.2. Ionization Parameter\r\nThe ionization parameter of RXCJ2248-ID3, , determined using the typical O32 = Iλ5008/Iλ3728 diagnostic is reported in M. W. Topping et al. (2024) to be in the high range of to −1. We recompute the ionization parameter for RXCJ2248-ID3 using the O32 and N43 = Iλλ1483,1486/Iλ1750 diagnostics from Z. Martinez et al. (2025) that are calibrated for densities in the 102 ≤ ne(cm−3) ≤ 106 range. We estimate a using O32, which is consistent with the value reported by M. W. Topping et al. (2024), and using N43. Note, however, that the O32 diagnostic is very sensitive to the assumed density (Z. Martinez et al. 2025), making this value highly uncertain in dense gas. For example, densities of ne = 103–105 cm−3 would lead to a range of to −2.04, respectively.\r\n\r\n4.3. Abundances\r\nHere, we present direct-method abundances of oxygen-to-hydrogen (O/H) (Section 4.3.1), N/O (Section 4.3.2), carbon-to-oxygen (C/O) (Section 4.3.3), and silicon-to-oxygen (Si/O) (Section 4.3.4) for RXCJ2248-ID3 using narrow-line flux ratios and the measured temperatures and densities presented in Section 4.1. Nearly all of the optical lines used in this work have sufficient S/N to simultaneously constrain broad and narrow emission components, but there are a few exceptions, all of which are low-ionization lines. The [O ii] λ3728 line was not covered by the GLIMPSE-D spectrum and so lacks the S/N to fit broad components. Both [N ii] λ6585 and [S ii] λλ6718,6733 are covered in the high-S/N GLIMPSE-D spectrum but are either blended with stronger features or too weak to fit broad components. On the other hand, the [O ii] and [S ii] lines have low critical densities around ne,crit ∼ 103 cm−3 such that any moderate to high-density broad components are likely collisionally de-excited away. Their narrow-component fluxes could also be significantly reduced by collisional de-excitation; however, the missing [O ii] emission is likely small in the absolute sense for such a high-ionization object. Emission from [N ii] is less likely to be collisionally de-excited (ne,crit ∼ 105 cm−3), so a hidden broad component could lead to an overestimate of the N/O abundance, but this effect would be somewhat countered by the underestimated [O ii] flux. In the end, the consistency of N/O derived independently from UV and optical tracers in Section 4.3.2 below suggests that these effects do not significantly impact our results.\r\n\r\nTo calculate the total or relative abundance of an element, we determine and sum the individual observed ions and then apply an ionization correction factor to account for unseen prominent ionization states. The abundance of an individual ionic species, Xi, relative to hydrogen is determined as\r\n\r\nwhere jλ(i) is the emissivity determined for the appropriate ionization zone temperature and density. Given the tendency of the optical density diagnostics to severely underestimate the density in high-density environments, we instead adopt the UV-derived densities. Note that the abundances presented below have not been corrected for the fraction of atoms embedded in dust. However, the level of depletion onto dust grains is expected to be small for the low metallicity of RXCJ2248-ID3 (e.g., A. Rémy-Ruyer et al. 2014; F. Galliano et al. 2018; J. Roman-Duval et al. 2022). Y. Isobe et al. (2026) also infer negligible dust depletion for RXCJ2248-ID3 based on the high value of Si/O that that they determine, but this is inconsistent with the value we determine below. Details of elemental abundance determinations are given below.\r\n\r\n4.3.1. Oxygen Abundance\r\nWe determine the total O/H abundance as the sum of the O+/H+ and O+2/H+ ionic abundances, determined from the [O ii] λ3728 and [O iii] λλ4960,5008 optical emission lines. We observe no strong O0 or O+3 emission, indicating that contributions from other ions are negligible. The resulting ionic and total oxygen abundances are presented in Table 2. Similar to M. J. Hayes et al. (2025) and Z. Martinez et al. (2025), we find that one of the most significant effects of accounting for high densities is the resulting decrease in electron temperature and subsequent increase in oxygen abundance (see, also, H. Katz et al. 2023). In our work, this results both from accounting for the missing [O iii] λ5008 flux due to collisional de-excitation and from correcting the narrow emission for broad emission components at their base. M. W. Topping et al. (2024) also incorporated the high densities seen in RXCJ2248-ID3 but did not have the S/N to fit the broad emission components in both [O iii] λ5008 and λ4364. As a result, we measure an oxygen abundance of . Note that if unresolved high-density clumps (ne ≳ 105 cm−3) are present (as suggested in, e.g., Section 2.3), it could introduce additional uncertainty by biasing the luminosity-weighted [O iii] λ4364/λ5008 ratio to higher densities, which would drive the derived Te higher and O/H abundance lower. However, Z. Martinez et al. (2025, see Figure 11), showed that the use of high-critical density UV density diagnostics largely mitigate this effect in a density stratified medium.\r\n\r\n4.3.2. Relative N/O Abundance\r\nThe extraordinary simultaneous detections of [N ii] λ6585, N iii] λ1750, and N iv] λλ1483,1487 enable multiple determinations of the N/O abundance. Therefore, we calculate N/O abundances using four different ionic methods\r\n\r\n\r\n\r\n\r\nwhere [O ii] λ3728 is used for the N+/O+ determination, O iii] λ1666 is used for the N+2/O+2 and N+3/O+2 calculations, and X(N+i) and X(O+i) are the N and O ionization fractions, respectively. We use the density-dependent ICFs from Z. Martinez et al. (2025), who provide prescriptions for densities of ne = 102, 103, 104, 105, and 106 cm−3. We, therefore, round our density measurements to the nearest order of magnitude and use the intermediate-ionization for the N+/O+ ICF and the high-ionization for the N+2/O+2 and N+3/O+2 ICFs. The resulting N ICFs and N/O abundances are reported in Table 3.\r\n\r\nThe four N/O determinations of RXCJ2248-ID3 are in close agreement, far above the expected value for its metallicity. Visually, this is shown in the upper left-hand panel of Figure 4, which plots the relative N/O versus O/H abundance with RXCJ2248-ID3 marked by purple diamonds. The traditional N/O–O/H trend has been established by many z ∼ 0 studies of H ii regions and galaxies (gray points: C. Esteban et al. 2002, 2009, 2014; L. S. Pilyugin & T. X. Thuan 2005; L. van Zee & M. Haynes 2006; J. García-Rojas & C. Esteban 2007; Á. R. López-Sánchez et al. 2007; D. A. Berg et al. 2012, 2016,2019, 2020). The empirical trend is a bimodal relationship, with a flat trend due to primary (or metallicity-independent) N production at low metallicities () and an increasing N/O trend with O/H as secondary (or metallicity-dependent) N production becomes increasingly important at higher metallicities (). As a visual guide, the primary N/O plateau from D. A. Berg et al. (2019, dashed purple line) is shown and the empirical stellar curve from D. C. Nicholls et al. (2017, solid green line) is shown as an example of the full primary and secondary curve.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. Relative C and N abundance trends versus metallicity. Nitrogen to oxygen ratio versus oxygen abundance for star-forming galaxies is plotted in the left panels, while C/O ratio versus oxygen abundance is plotted in the middle panels, and carbon to nitrogen abundance versus oxygen abundance is plotted in the right panels. Top row: RXCJ2248-ID3 is shown relative to the observed z ∼ 0 trend and other high-z galaxies. The abundances for RXCJ2248-ID3 are shown as purple diamonds, where multiple N/O points show the measurements for each ionic N/O calculation method. For comparison, we also plot the abundances derived for RXCJ2248-ID3 by M. W. Topping et al. (2024) as turquoise squares. The typical bimodal N/O trend is characterized by local dwarf (gray diamonds; L. van Zee & M. Haynes 2006; D. A. Berg et al. 2012, 2016, 2019) and spiral galaxy (gray circles; C. Esteban et al. 2002, 2009, 2014; L. S. Pilyugin & T. X. Thuan 2005; J. García-Rojas & C. Esteban 2007; Á. R. López-Sánchez et al. 2007; D. A. Berg et al. 2020) H ii region measurements. The primary N/O plateau from D. A. Berg et al. (2019) is shown as a dashed purple line, while the solid green line is the empirical stellar curve from D. C. Nicholls et al. (2017). Additional C/O literature measurements for dwarf galaxies are from M. A. Peña-Guerrero et al. (2017) and P. Senchyna et al. (2017). Abundances for z > 2 galaxies from Z. Martinez et al. (2025) are plotted as blue plus signs for galaxies with UV N+2/O+2 derived abundances and pentagons for optical N+/O+ derived abundances. Bottom row: The same observed samples are shown as the top row, but with the z ∼ 0 sample represented by the shaded gray regions. The observed abundances of RXCJ2248-ID3 are compared to updated dual-burst chemical evolution models of C. Kobayashi & A. Ferrara (2024, string of circles), color coded by age since onset of the second burst. The models have been modified to reproduce both the enhanced N/O and relatively deficient C/O observed for RXCJ2248-ID3, which requires enrichment from WN but very little WC enrichment, as expected at low metallicities.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nFor comparison, we plot the high-quality high-redshift N/O measurements that were calculated in a consistent manner as the present work (with direct-method Te and ne determinations and ne-dependent ICFs) by Z. Martinez et al. (2025). N/O abundances determined using N+2/O+2 are plotted as blue + symbols, while N+/O+ determinations are plotted as blue pentagons. Of these galaxies, the closest comparison to RXCJ2248-ID3 is CEERS-1019 (see, also, R. Marques-Chaves et al. 2024), while only GDS 3073 and GN-z11 have higher relative N/O abundances and only GDS 3073 is more enhanced in N/O for its O/H abundance.\r\n\r\nWe find that all four ionic methods produce consistently high N/O values within their uncertainties, with a weighted mean of . This is an important result because RXCJ2248-ID3 is the first galaxy to have consistently enhanced N/O abundances measured from both the rest-frame UV high-ionization and the optical low-ionization emission lines. Furthermore, measuring consistent N/O values from three different ionic methods strengthens our confidence in the robustness of the N/O measurement, although uniform N/O across the ionization structure of the nebula is not a given in a stratified medium. While there is strong evidence for a stratified, or perhaps very clumpy, density structure in RXCJ2248-ID, the N/O abundance appears to be well mixed.\r\n\r\n4.3.3. Relative C/O Abundance\r\nMeasuring the C/O abundance provides a crucial comparative baseline for interpreting the origin of elevated N/O in RXCJ2248-ID3. Similar to N, C has a pseudosecondary17 production pathway, but the dominant nucleosynthetic sources and timescales differ for C and N. Briefly, both C and O are primarily produced in massive stars (>8 M⊙) on relatively short timescales such that the C/O ratio is a relatively stable tracer of massive star yields, although some C is produced via low- to intermediate-mass AGB stars (∼1.5–3 M⊙). In contrast, some N is produced by massive stars (e.g., through rotational mixing and WR winds) but most N comes from intermediate-mass AGB stars (∼4–8 M⊙), which release N on longer timescales (∼200 Myr). Therefore, N/O and C/O together serve as diagnostics of the recent star formation history, constraining the recent enrichment mechanisms of galaxies (e.g., D. R. Garnett 1990; R. B. C. Henry et al. 2000; C. Chiappini et al. 2003; E. Pérez-Montero & T. Contini 2009; D. A. Berg et al. 2019; E. Pérez-Montero et al. 2021).\r\n\r\nRelative C/O abundances are typically determined using the C iii] λλ1907,1909/O iii] λ1666 ratio to calculate C+2/O+2 and assuming that C/O ≈ C+2/O+2. This method is sometimes used alone owing to the fact that (1) C+2 and O+2 have somewhat similar ionization potentials (24.38 and 35.12 eV, respectively), (2) the upper levels of the λ1666 and λλ1907,1909 transitions have similar excitation potentials (∼6.5 and ∼7.5 eV, respectively), and (3) the integrated fluxes of λ1666 and λλ1907,1909 are not sensitive to collisional de-excitation for the densities measured here. However, for the high-ionization nebulae in RXCJ2248-ID3, it is important to account for contributions from the C+3 species and any unseen species. We note that the C iv λλ1548,1550 doublet is clearly observed in the rest-UV spectrum of RXCJ2248-ID3, but these lines are resonant and can be affected by the C iv stellar wind feature and ISM absorption, and so determining the intrinsic flux and subsequent C+3 abundance is challenging. Instead, we use an ICF determined from the photoionization models presented in Z. Martinez et al. (2025) such that\r\n\r\nWe used the and a density of ne(C+2) ∼ 105 cm−3 to determine the C ICF. The resulting C ICF and C/O abundance are reported in Table 3.\r\n\r\nThe C/O and C/N abundances for RXCJ2248-ID3 are plotted in the upper middle and right-hand panels of Figure 4. Empirical trends of C/N at z ∼ 0 are found to be flat, albeit with significant scatter (see shading in Figure 4), suggesting that the dominant nucleosynthetic mechanisms of C are similar to those of N (e.g., D. R. Garnett et al. 1999; C. Esteban et al. 2014; D. A. Berg et al. 2016, 2019). However, while the production of both C and N appear to be metallicity-dependent, the scatter in their trend is consistent with differing production timescales due to stars of different masses. Thus, the variations observed in CNO abundance patterns of high-redshift galaxies may be the result of taking a snapshot of many galaxies at different times since their most recent onset of star formation.\r\n\r\nRXCJ2248-ID3 appears to have a similar CNO abundance pattern to other high-redshift N emitters, characterized by enhanced N/O but relatively deficient C/O such that their C/N is very deficient compared to the expectations from low-redshift trends. This suggests that these high-redshift N-emitting galaxies are enhanced in N relative to both O and C. If massive stars in the WN phase are present, they will have recently produced 14N at the expense of 12C through the CNO cycle, meaning C used as a catalyst in the cycle initiation will have been consumed as N is removed during the bottleneck step via dredged up, preventing the return of C at cycle completion. Thus, C/N-deficiency is consistent with a recent, intense episode of N enrichment and C consumption from WN stars. Conversely, if both N/O and C/O were elevated in tandem, it could point to broader enrichment by massive stars, such as enrichment from both WN and WC stars, whose contributions increase at higher metallicities.\r\n\r\n4.3.4. Relative Si/O Abundance\r\nDetecting Si iii] λλ1883,1892 in RXCJ2248-ID3 enables the rare opportunity to measure the silicon-to-oxygen (Si/O) abundance in a z > 5 galaxy (see, also, Y. Isobe et al. 2026, for Si/O in GN-z11). Silicon abundances are important for multiple reasons. Silicon is highly refractory, making the Si/O ratio a sensitive probe of dust depletion. Additionally, Si probes different channels of chemical enrichment than CNO elements, as it is primarily an α-element produced by CCSNe, but Type Ia SNe, AGB stars, and even pair-instability SNe are all expected to contribute to the total Si abundance. For RXCJ2248-ID3 we determine the Si/O abundance using the observed Si iii] λλ1883,1892/O iii] λ1666 ratio to calculate Si+2/O+2. Because Si+2 and O+2 have rather different ionization potentials (16.3 eV versus 35.1 eV, respectively), a Si ICF is required to convert Si+2/O+2 to total Si/O via\r\n\r\nSi ICFs have been reported previously (e.g., D. R. Garnett et al. 1995), but none account for the high-density conditions observed in RXCJ2248-ID3. Therefore, we determined a Si ICF = 3.507 using the photoionization models presented in Z. Martinez et al. (2025) using the and a density of ne(Si+2) ∼ 104 cm−3. Reported in Table 3, the resulting (Si/O) = −1.781 ± 0.157 abundance is typical of metal-poor dwarf galaxies (e.g., D. R. Garnett et al. 1995; Y. I. Izotov & T. X. Thuan 1999), consistent with normal massive star production and low dust depletion.\r\n\r\n4.4. Potential Impact of UV Broad Components\r\nThe exceptionally high S/N of the rest-optical GLIMPSE-D spectrum allows for broad emission component fits that the rest-UV spectrum does not. In Section 2.2, we found the broad emission component contribution to the narrow [O iii] λ5008 flux to be 10.8%. To examine the possible effects such contamination has on calculations of nebular conditions and abundances, we adopt 10.8% as the contamination upper limit to the UV emission lines. We first consider the impact on the UV density determinations, where we allow the broad components of the UV density-sensitive emission-line ratios to have densities ranging from 102–106 cm−3. After subtracting the potential broad component contribution, the revised densities change up to Δne(Si+2), Δne(C+2), and Δne(N+3) over the range of broad component densities considered. These values are within the reported uncertainties in Table 3, with the exception of the ∼1.2σ deviation for Δne of C+2.\r\n\r\nNext, we tested the subsequent impact of UV densities that have been revised for possible broad components on the properties determined from rest-optical emission lines: Te(O+2), O/H, and N/O. For the range of Δne(N+3) above, the resulting K, which is within 1σ–2σ of the reported value in Table 3. Similarly, the impact of the revised densities and temperatures on the oxygen abundance, dex, is also within 1σ–2σ. The impact is even smaller for the nitrogen abundance, with dex being much smaller than the N/O uncertainty.\r\n\r\nRelative UV abundances are impacted by changes in both the nebular conditions and the relevant abundance emission-line ratio. However, the resulting abundance deviations are small and within the original uncertainties: dex, dex, and dex. Thus, we conclude that while considering the impacts of hidden broad component contributions to the measured UV fluxes is important, the potential biases do not affect the main results or conclusions of this work.\r\n\r\n5. A Short Window of Intense WR Nitrogen Enrichment\r\nWe have presented evidence for WN stars in RXCJ2248-ID3 in two forms: first, the rest-frame optical WR blue bump discussed in Section 3 and shown in Figure 2; and second, a qualitative comparison of the CNO abundances to patterns expected for WR stars in Section 4.3 and Figure 4. Below, we examine the plausibility and impact of these WN stars by comparing RXCJ2248-ID3 to expected trends for WR stars with metallicity (Section 5.1), testing whether stellar yields can reproduce the observed CNO abundance pattern (Section 5.2) and assessing whether RXCJ2248-ID3’s stellar population can produce its inferred mass of ionized N (Section 5.3). Together, these lines of investigation suggest that the enhanced N/O and suppressed C/O in RXCJ2248-ID3 represent a short-lived enrichment phase, unique to metal-poor, highly star-forming galaxies in the early Universe (Section 5.4).\r\n\r\n5.1. WN Stars: The Dominant WR Phase at Low Metallicity\r\nTo date, no individual resolved WR stars have been directly observed at metallicities as low as RXCJ2248-ID3 (Z ∼ 0.1Z⊙). This is due, in part, to the lack of sufficiently close (D ≲ 1 Mpc for the young, crowded clusters hosting WR stars), metal-poor, star-forming galaxies (see C. Kehrig et al. 2013 for the closest metal-poor WR galaxy), but a scarcity of WR stars in metal-poor environments is also expected because mass loss through stellar winds scales with metallicity. We show the trend of the number of WC/WN stars as a function of metallicity in Figure 5. The observed number of WC/WN stars in M31 (∼175% Z⊙), the Milky Way (MW; Z⊙), M33 (∼40%–110% Z⊙), the Large Magellanic Cloud (LMC; ∼40% Z⊙), and the Small Magellanic Cloud (SMC; ∼20% Z⊙) suggest that the number of the WN/WC number ratio increases with decreasing metallicity (e.g., G. Meynet & A. Maeder 2005; P. A. Crowther 2007; P. Massey et al. 2015; K. Neugent & P. Massey 2019). This is because weaker metal line-driven winds, rotation, or binary effects in metal-poor stars may be able to expose their nitrogen-rich layers and initiate the WN phase but be insufficient to strip the stellar He atmosphere and reveal the carbon-rich core to initiate the WC phase. Thus, if WR stars form at Z ∼ 10% Z⊙, they are expected to be overwhelmingly WN-type. Additionally, A. A. C. Sander et al. (2026) recently discovered a new class of WN–WO stars that point to a low-metallicity WR evolutionary channel in which stars pass directly from the WN to WO phase, potentially explaining spectra that show evidence for WN-like enrichment and hard ionizing radiation without clear WC signatures.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 5. Observed and theoretical ratios of WC/WN star numbers as a function of metallicity. Observed values for the SMC, LMC, MW, and M31 were compiled by K. Neugent & P. Massey (2019), while newer values for M33 come from K. F. Neugent & P. Massey (2023). For comparison, we also plot the trend presented in P. Massey et al. (2017) for BPASS v2.0 binary stellar population synthesis burst models for 12+log(O/H) > 8 (solid line green line), which we extrapolate to lower metallicities (dashed line). Enrichment from WR stars was used to explain the CNO abundances in GN-z11 by C. Kobayashi & A. Ferrara (2024). We note the metallicity for GN-z11 determined by Z. Martinez et al. (2025) is consistent with a WC/WN ratio of ∼0.1–0.2 and the metallicity for RXCJ2248-ID3 from the current work, which predicts a much lower WC/WN ratio of ∼0.03–0.10. Therefore, very little carbon enrichment from WC stars is expected for RXCJ2248-ID3.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nThe spectral features of RXCJ2248-ID3 support the picture of WN star feedback at low metallicity. As shown in Figure 2, the He ii emission is moderately broadened, the N iii λ4642 line in the blue bump is prominent, and there is no evidence for the red bump C iv feature, all consistent with the presence of WN stars at low metallicity. The weakness of the He ii emission in terms of both flux and velocity width is expected for the low-metallicity environment of RXCJ2248-ID3 (∼10% Z⊙) due to reduced wind velocities and mass-loss rates (e.g., A. A. C. Sander et al. 2020). Similarly weak WN features have also been reported in the nearby metal-poor galaxy SBS 0335-052 (Y. I. Izotov et al. 2006) and, at cosmic noon, the z ∼ 2.37 lensed galaxy the Sunburst Arc (T. E. Rivera-Thorsen et al. 2024) and the z ∼ 2.22 M4327 galaxy (M. Curti et al. 2025b).\r\n\r\nWe plot the WR blue bump profile of RXCJ2248-ID3 relative to the Sunburst Arc and M4327 in Figure 6. For ease of comparison, we convolve the Sunburst Arc R ∼ 2700 JWST/NIRSpec G140H spectrum to the R ∼ 1000 resolution of the RXCJ2248-ID3 spectrum. For M4327, we retrieved the G140M spectrum obtained as part of the Measuring Abundance at High Redshift with the Te Approach Survey (MARTA; E. Cataldi et al. 2025) from the Dawn JWST Archive (DJA; K. E. Heintz et al. 2024; A. de Graaff et al. 2025). Both the Sunburst Arc and M4327 spectra were scaled to similar He ii strengths as RXCJ2248-ID3. These spectra immediately reveal similar profiles, but with three distinct differences: (1) RXCJ2248-ID3 exhibits higher gas ionization, as evidenced by the strong [Ar iv] λλ4713,4741 emission; (2) the He ii stellar wind feature is significantly broader in both the Sunburst Arc (FWHM = 1370 km s−1) and M4327 (FWHM = 1460 km s−1) than RXCJ2248-ID3 (FWHM = 530 km s−1), consistent with stronger stellar winds at the higher metallicities of the Sunburst Arc: (or Z ∼ 0.7 Z⊙; Z. Martinez et al. 2025) and M4327: (or Z ∼ 0.3 Z⊙; M. Curti et al. 2025b); and (3) the WR N iii λ4642 line is much stronger in RXCJ2248-ID3, which lacks WR C iv λλ5803,5814 emission, while the Sunburst Arc and M4327 exhibit both N iii and C iv emission. These differences support a scenario in which the z ∼ 2 WR galaxies hosts both WC and WN stars, but the more metal-poor RXCJ2248-ID3 hosts a young population of WN stars with no or very little WC contribution.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. The blue WR region of the optical spectrum of RXCJ2248-ID3 (purple) is shown in comparison to the z ∼ 2.37 Sunburst Arc spectrum from T. E. Rivera-Thorsen et al. (2024, blue), which has been convolved to R ∼ 1000 to match RXCJ2248-ID3, and the z = 2.22 M4327 spectrum obtained from the DJA, but originally presented in M. Curti et al. (2025b, turquoise). All three galaxies show characteristic signs of hosting WN stars but RXCJ2248-ID3 shows striking N iii λ4642 emission that is much stronger than both the Sunburst Arc and M4327. On the other hand, the Sunburst Arc and M4327 show broader He ii emission, which is expected for more metal-rich galaxies as stellar winds scale with metallicity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n5.2. Relative Chemical Enrichment from WN Stars\r\nWith the highest redshift detection of WN stars to date, we now explore their chemical yields as a source of the abundance pattern in RXCJ2248-ID3. C. Charbonnel et al. (2023) performed a comparable analysis for the extreme N/O ratio observed in GN-z11 and found that such rapid nitrogen enrichment could arise from normal massive stars with M⋆ ∼ 20–120 M⊙ or from supermassive stars (M⋆ ≳ 1000 M⊙) in protoglobular cluster environments. Their results and those of R. Marques-Chaves et al. (2024) further demonstrated that the short-lived WN-like phase can produce large N/O ratios within a few megayears of the burst, consistent with the timescales inferred here, but that the observed C/O ratios are only compatible over a very short time interval. Building on this theoretical groundwork, C. Kobayashi & A. Ferrara (2024) showed that a dual-burst chemical evolution model with a short WR-dominated enrichment phase could also match GN-z11’s enrichment pattern. Similarly, R. Marques-Chaves et al. (2024) used N yields from rotating massive stars to demonstrate that a young, WR-dominated stellar population could reproduce the observed CNO enrichment pattern in CEERS-1019.\r\n\r\nThe models above provide a valuable physical framework for linking stellar yields to galaxy-scale abundance evolution at early times. To extend the methodologies outlined by these works to RXCJ2248-ID3, we first examine the dual-burst chemical evolution model of C. Kobayashi & A. Ferrara (2024), which was fine-tuned to reproduce the enhanced N/O in GN-z11 (reported by R. Maiolino et al. 2024). This model invokes two bursts of star formation, where the second triggers a narrow (≲1 Myr) phase of WR-dominated enrichment. While the model can easily reach the N/O enrichment level of RXCJ2248-ID3, it was also designed to yield the higher O/H and C/O abundances observed in GN-z11 than in RXCJ2248-ID3, which was achieved, in part, by enrichment from WC stars. The updated O/H abundance for GN-z11 determined by Z. Martinez et al. (2025) makes it consistent with some carbon enrichment from WC stars, as shown in Figure 5. However, with a metallicity of only Z ∼ 0.10 Z⊙, the WR population in RXCJ2248-ID3 is expected to consist of few WC stars, and so an updated chemical evolution model is needed to match its unique CNO abundance pattern.\r\n\r\nWe modify the C. Kobayashi & A. Ferrara (2024) dual-burst model to be more appropriate for the metal-poor conditions in RXCJ2248-ID3. In particular, the galactic chemical evolution (GCE) model uses the same star formation history and the standard IMF (for 0.01–120 M⊙) as in the fiducial model in C. Kobayashi & A. Ferrara (2024) but reduces the contribution from WC stars. C/O ratios of the nucleosynthesis yields vary depending on the uncertain nuclear reaction rates (e.g., 12C(α, γ)16O) and the treatment of convection and mass loss (C. Kobayashi et al. 2006). In the updated model, 12C and 16O yields are taken from C. Kobayashi et al. (2020) for all mass ranges of stars but the contributions from the WC wind phase is scaled to ∼15% in order to match the empirical trends and theoretical expectations that most massive stars will have insufficient winds to remove their He envelopes at such low metallicities.\r\n\r\nWe plot the updated metal-poor dual-burst model in the bottom row of Figure 4 as a time-series of points that are color coded by the age since the onset of the second burst. In this model, the observed N/O, O/H, and C/O abundances of RXCJ2248-ID3 are reached simultaneously ∼4.2 Myr after the onset of the second burst. This young age is consistent with enrichment from WN stars and with the derived clump age of Myr (A. Claeyssens 2025). Thus, the N/O-enhanced and relatively C/O-deficient conditions in RXCJ2248-ID3 are produced by a short-lived evolutionary phase following intense, bursty star formation.\r\n\r\nWe note that the duration and impact of the WN phase may be significantly extended if the stars evolve in binary systems. In the M. Limongi & A. Chieffi (2018) single-star models, the WN phase typically lasts ∼0.03–0.3 Myr and, due to the metallicity-dependent winds, require high initial masses (∼40 M⊙) to expose the He- and N-rich layers. However, in close binaries, envelope stripping via mass transfer or common-envelope evolution can induce WR phases in lower-mass stars (20–30 M⊙), largely independent of the stellar metallicity. This channel can significantly prolong the WN lifetime (up to ∼1 Myr) depending on the binary mass ratio and separation (e.g., J. J. Eldridge et al. 2017; Y. Götberg et al. 2019; D. R. Aguilera-Dena et al. 2022). As a result, binary evolution may enhance both the frequency and duration of the chemically selective N/O enrichment phase, such as that observed in RXCJ2248-ID. On the other hand, L. Boco et al. (2025) successfully modeled observations of single WR stars in the SMC, suggesting that binary stripping may not be required to produce WR stars at low metallicity. Clearly, the frequency, lifetimes, and formation channels of WR stars in low-metallicity environments are not yet well understood. Future work incorporating current binary and single star WR pathways into chemical evolution models may, therefore, be essential for capturing the full range of nitrogen feedback in low-metallicity starbursts at high redshift.\r\n\r\nTaken together, the massive star enrichment scenario presented here, and explored in C. Charbonnel et al. (2023), R. Marques-Chaves et al. (2024), and C. Kobayashi & A. Ferrara (2024), demonstrates that selective enrichment of nitrogen by WN-dominated feedback can naturally reproduce the observed CNO abundance pattern in compact, low-metallicity starbursts such as RXCJ2248-ID3. We can now paint a full picture of the ISM in RXCJ2248-ID3. The consistency of N/O across ions spanning a wide range of ionization potentials suggests that the WN-enriched material has been efficiently mixed throughout the ionized gas. This apparent chemical homogeneity does not contradict the strong density and temperature stratification inferred from our diagnostics: a clumpy or multiphase ISM can remain compositionally uniform if the enriched ejecta are well dispersed. Given the extreme compactness of RXCJ2248-ID3 (Re ≈ 20 pc), the characteristic dynamical and sound-crossing times are only a few ×105 yr, comparable to or shorter than the duration of the WN phase itself. Under such conditions, turbulent and radiative mixing can rapidly homogenize the heavy-element yields, producing a chemically uniform yet physically structured nebula.\r\n\r\n5.3. The N Mass Budget\r\nA crucial point of validation is whether an intense burst of star formation so early in the Universe could have produced the amount of N present in RXCJ2248-ID3. Similar to the analysis in R. Marques-Chaves et al. (2024), we test this by first estimating the ionized nitrogen mass using\r\n\r\nwhere the atomic mass ratio is mN/mH = 14 and N/H is the nitrogen abundance of the ionized gas. The hydrogen gas mass MH is derived from the Hα luminosity as\r\n\r\nwhere mH = 1.67 × 10−27 kg, h = 6.626 × 10−27 erg s−1, νHα is the frequency of the Hα emission line, and cm3 s−1 is the Case B effective recombination coefficient for Hα assuming a Te = 1.97 × 104 K. We estimate the Hα luminosity using a luminosity distance of dL(z = 6.1025) =1.817 × 1029 cm, the collision-corrected narrow-component Hα flux, and a magnification of μ = 6.8877 (L. Furtak et al. 2025) to be LHα =  1.20 × 1042 erg s−1. Combining this LHα with the equivalent width (EW)(Hα) = 1457 Å, we derive the star formation rate (SFR) using the simulation-based SFR(Hα) calibration from I. G. Kramarenko et al. (2026). This method was developed to be more appropriate for the bursty conditions at high redshift than traditional calibrations and gives SFR = 3.2 M⊙ yr−1, similar to the SED-derived SFRs assuming a constant SFH for 1 Myr () and 10 Myr (; see Table 1). Adopting a filling factor of ε = 0.01-0.10, assuming a compact starburst (e.g., R. C. Kennicutt 1984; G. Stasińska & D. Schaerer 1997), a density of 104 cm−3, and the measured N/H value, we calculate the ionized nitrogen mass to be .\r\n\r\nWe then compute the total nitrogen mass that can be produced by the recent burst of star formation using the integrated nitrogen yield produced by the modified C. Kobayashi & A. Ferrara (2024) model for the SED-derived stellar mass of assuming a continuous SFH over the duration of the second burst (∼4.2 Myr). This results in a total N mass of 435 M⊙, implying that ∼% of the gas is retained from the WN winds and ionized when matched to the expected ionized N mass (∼) from the crudely calculated observed value. Thus, WN stars formed in a recent burst within a compact, high-density, and very clumpy/inhomogeneous (low-filling-factor) environment can plausibly explain the N mass in RXCJ2248-ID3, even at low metallicity (∼10% Z⊙), without invoking a top-heavy IMF or exotic enrichment channels.\r\n\r\n5.4. The Ephemeral Imprint of WN Star on High−z Galaxies\r\nThe prominence of N/O enhancement at z ≳ 5 but relative rarity in local star-forming galaxies likely reflects a combination of environmental conditions and evolutionary factors that are unique to the early Universe. To examine the likely environments, we plot the SFR surface density (ΣSFR) versus EW of Hβ in Figure 7 for both z ≳ 6 N emitters (RXCJ2248-ID3: M. W. Topping et al. 2024, this work; GNz9p4: D. Schaerer et al. 2024; GN-z11, EW(Hβ) inferred from Hγ: A. J. Bunker et al. 2023; S. Tacchella et al. 2023; GDS 3073: E. Vanzella et al. 2010; H. Übler et al. 2023; X. Ji et al. 2024; CEERS-1019: R. L. Larson et al. 2023; R. Marques-Chaves et al. 2024; A1703-zd6: M. W. Topping et al. 2025b) and local star-forming galaxies with enhanced SFRs from the COS Legacy Archive Spectroscopic SurveY (CLASSY; B. L. James et al. 2021; D. A. Berg et al. 2022; N/O from K. Z. Arellano-Córdova et al. 2025). The high-redshift galaxies, such as RXCJ2248-ID3, exhibit compact morphologies (Re ≲ 102 pc) that lead to much higher SFR surface densities than seen at z ∼ 0, as well as bursty star formation histories that favor the rapid buildup of massive stars capable of entering the short-lived WN phases (M⋆ > 20 M⊙). The high-redshift N emitters also have high Hβ EWs (>200 Å) that are indicative of young current bursts of star formation (<5 Myr). This suggests that compactness alone is not enough to observe enhanced N/O; we must also observe these galaxies at the fleeting moments of very young bursts when WR stars are most active.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 7. SFR surface density versus Hβ EW for high-redshift (z > 5) N emitters versus z ∼ 0 galaxies from the CLASSY survey (SFR: D. A. Berg et al. 2022; N/O: K. Z. Arellano-Córdova et al. 2025), which have enhanced SFRs similar to z ∼ 2–3 galaxies. High-redshift N emitters are only observed at young ages (≲5 Myr), as indicated by the high Hβ EWs (EW> 200 Å), and in compact, dense environments (ΣSFR > 10 M⊙ yr−1 kpc−1). Note that RXCJ2248-ID3 is plotted here using the properties derived from M. W. Topping et al. (2024) for continuous star formation to be consistent with the other N-emitter measurements.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nFigure 7 suggests a scenario of elevated N/O at low metallicity being preferentially seen in galaxies with high SFR surface densities and young stellar ages (e.g., D. Schaerer et al. 2024; M. W. Topping et al. 2024; Z. Martinez et al. 2025). R. Marques-Chaves et al. (2024) also suggest that the elevated N/O and high-ionization spectrum of CEERS-1019 trace a short evolutionary window of a ≲5 Myr burst dominated by WN-like feedback. Furthermore, the theoretical models of C. Charbonnel et al. (2023) predict that such phases are characteristic of young, dense stellar systems, potentially analogous to protoglobular clusters, reinforcing that our observed WN-driven enrichment is a natural outcome of clustered, bursty star formation at early times.\r\n\r\nAt low metallicity, weaker stellar winds require higher initial masses for stars to reach the WR phase, so a larger total stellar mass must form in a burst to produce a detectable population of WN stars. In compact galaxies beyond cosmic noon, this condition is naturally met in systems with high SFR surface densities, which statistically sample the upper IMF more fully and produce a detectable population of WN stars (e.g., J. Brinchmann et al. 2008; M. Shirazi & J. Brinchmann 2012). Furthermore, the WR enrichment signature is short-lived: it must be captured during the brief WN-dominated phase (tburst ≲ 5 Myr and ΔtWN ≲ 0.3 Myr), before dilution from WC stars, CCSNe, or delayed AGB enrichment. These timing constraints imply that only a small fraction of the star-forming galaxies in the distant Universe will be caught in this phase. The detection of WR-driven N/O enhancement at high redshift thus reflects a brief evolutionary stage where intense, rapid feedback from a large number of WN stars briefly imprints nonuniform elemental enrichment patterns (i.e., elevated N/O), which are expected to be quickly washed away. As soon as the system evolves beyond the WN phase, subsequent WC or CCSN yields will rapidly dilute the N excess and alter the overall abundance patter (e.g., increasing C/O, lowering N/C).\r\n\r\nRecently, M. W. Topping et al. (2025b) showed that galaxies with significant N iv] emission (corresponding to extreme N/O enhancement), are found exclusively among galaxies with extreme [O iii]+Hβ EWs of 2600–4200 Å. Galaxies with such high [O iii]+Hβ EWs are in the upper 2% tail of the EW distribution at z ≳ 4 and are outliers at z ∼ 0. This strongly suggests that high N/O outliers are confined to the youngest stellar populations undergoing their most intense bursts of star formation in the early Universe (e.g., R. Endsley et al. 2023, 2025; J. Matthee et al. 2023; M. W. Topping et al. 2025b).\r\n\r\nIn this context, M. W. Topping et al. (2025b) found that 30% of galaxies with EW[O III] + Hβ > 2000 Å show strong nitrogen emission, corresponding to ∼0.6% of their UV-selected parent population. If this 0.6% population corresponds to enhanced N/O during the ΔtWN ∼ 0.3 Myr WN phase, it would imply a characteristic burst timescale of ∼50 Myr. A practical consequence is that young bursts substantially increase the light-to-mass ratios and, thus, the likelihood of detection in flux-limited samples (e.g., C. A. Mason et al. 2023; J. B. Muñoz et al. 2023; G. Sun et al. 2023). Therefore, the observed frequency of strong nitrogen emitters at fixed MUV is likely biased high relative to their intrinsic abundance (e.g., at fixed stellar mass). Given the detectability bias toward burst phases, this tburst may represent a lower limit, with the true interval plausibly longer. This timescale is supported by recent analyses of the scatter in the star-forming main sequence and time-resolved SFR indicators at z ∼ 3–9 that suggest burst cycles of tens-of-megayear timescales (albeit with broad distributions, e.g., C. Simmonds et al. 2025). Thus, the combination of extreme-EW selection and N iv] frequency provides a novel timing argument that WN-driven enrichment is tightly coupled to very young, transient starburst phases beyond cosmic noon.\r\n\r\nTaken together, the arguments presented in this work suggest that nitrogen outliers are not exotic exceptions, but rather a brief, WN-enriched phase that any high-redshift galaxy with sufficiently high SFR surface density can pass through. In contrast, numerous low-redshift WR galaxies exhibit young populations that include WN and WC stars but show little or no N/O enhancement (e.g., Y. I. Izotov et al. 2006; C. Kehrig et al. 2013). This difference underscores that similar stellar populations do not guarantee the same chemical signatures; instead, the extreme densities, compactness, and rapid mixing timescales of high-redshift starbursts likely make WN-driven enrichment both more pronounced and more transient. In this view, N/O outliers in the early Universe are not anomalies, but rather are the chemical fingerprints of galaxies caught midburst, showing fleeting yet inevitable markers of early galaxy evolution.\r\n\r\n6. Conclusions\r\nWe have presented a detailed enrichment scenario by WN stars that explains the extreme nitrogen enrichment in the metal-poor (∼10% Z⊙), high surface-density (1.34 × 103 M⊙ pc−2), high-redshift (z = 6.1025), lensed galaxy RXCJ2248-ID3. These measurements were made possible by exceptionally deep JWST/NIRSpec medium-resolution spectroscopy of RXCJ2248-ID3, obtained as part of the GLIMPSE-D survey. The unprecedented depth and S/N of the GLIMPSE-D spectrum allow spectral measurements typically limited to the nearby Universe, including consistent broad components in the Balmer series and [O iii] λ4364 and λλ4960,5008 lines, faint [Ar iv] λλ4713,4741 emission, and signatures of WR stars. Specifically, we detected the emission characteristic of WN-type stars, including strong N iii λ4642 and broadened He ii λ1640 and λ4687 emission, marking RXCJ2248-ID3 as the most distant galaxy to date with spectroscopic detections of WR stars.\r\n\r\nWe performed a detailed nebular analysis, self-consistently measuring the reddening, high-ionization temperature (Te(O+2)), and densities from five different diagnostics across a wide ionization range. We measure a low reddening value of from the Hγ/Hβ ratio but find an excess in the Hα/Hβ ratio of 0.204 due to collisional excitation of Hα. The measured densities span the range of 1.15 × 103 cm−3 ≤ ne ≤ 2.65 × 105 cm−3 and show strong evidence for nebular density stratification, with systematically higher densities in the highest-ionization gas and UV emission tracing gas at higher densities than those traced by optical diagnostics. This structure implies a highly clumpy, multiphase ISM. We note that such high-density, multiphase gas leads to densities from optical diagnostics that are biased to the low end of the density range due to their low critical densities. Therefore, we recommend using UV density diagnostics because they are more robust in high-density environments: ne(Si+2), ne(C+2), and ne(N+3) trace the densities in the low-, intermediate-, and high-ionization gas, respectively. As a result, we measure a direct-method metallicity of .\r\n\r\nUsing the full rest-UV+optical spectra, we present the first robust, consistent measurements of N/O abundance in any galaxy using three ionization stages of nitrogen (N+/O+, N+2/O+2, N+3/O+2). The uniformity of our N/O measurements suggests that the N/O enrichment is spatially extended and well mixed throughout the ionized ISM. Empirical trends suggest C/O should follow a similar trend as N/O, and thus also be enhanced. In contrast, we find C/O to be significantly depleted relative to N/O, suggesting nonuniform elemental enrichment likely driven by WN stars with little to no contribution from WC stars.\r\n\r\nThe CNO abundance pattern is best reproduced by a modified version of the dual-burst chemical evolution model from C. Kobayashi & A. Ferrara (2024) that reduces the contribution from WC stars relative to WN stars, as expected in metal-poor environments. The resulting short-lived WN phase ejects N-rich, C-poor material. We use this chemical evolution model to assess whether the observed N mass can plausibly arise from the recent star formation in RXCJ2248-ID3 and estimate an ionized N mass of 435 M⊙. This value is consistent with the N mass estimated from the observed emission lines of M⊙ if % of the N gas is ionized.\r\n\r\nThese results demonstrate that standard stellar evolution models can reproduce both the CNO pattern and the total nitrogen mass observed without invoking an exotic IMF or enrichment channel. The uniform N/O ratios across multiple ionization zones further suggest that the WN yields were rapidly mixed into a relatively pristine ambient ISM, preserving the global enhancement observed in RXCJ2248-ID3. Although RXCJ2248-ID3 exhibits strong density and temperature stratification, this structural complexity does not necessarily imply chemical inhomogeneity. The consistent N/O ratios across ions tracing vastly different physical conditions indicate that the enriched material was efficiently dispersed throughout the multiphase ISM. In such a compact (Re ≈ 20 pc), high-pressure environment, turbulent and radiative mixing can homogenize the chemical composition on timescales comparable to, or shorter than, the brief WN phase itself, yielding a chemically uniform yet physically clumpy nebula.\r\n\r\nImportantly, the abundance pattern and physical conditions observed in RXCJ2248-ID3 can only be explained if the galaxy is caught during a narrow evolutionary window within a few megayears of a massive, compact starburst when WN stars dominate chemical feedback. At low metallicity, stars require higher initial masses to reach the WR phase, making such enrichment episodes rare and dependent on sufficiently high SFRs to fully populate the upper IMF. Furthermore, the WN phase itself is extremely short-lived (∼0.03–0.3 Myr) and easily masked by subsequent WC winds, CCSNe, or AGB stars contributions. These timing and SFR constraints make WR-driven N/O enhancement a rare phenomenon associated with extreme starburst conditions that are more common in the early Universe, and which are scarce in the local Universe.\r\n\r\nOur results suggest that the WN-driven N/O enrichment we observe is not a peculiar property of a single system, but rather a brief phase that essentially all high-redshift galaxies (z > 5) with sufficiently high SFR surface densities to produce significant numbers of WN stars likely undergo. In particular, the work of M. W. Topping et al. (2025b) can be used to link N/O outliers to the most extreme [O iii]+Hβ EWs. The observed frequency of such EWs combined with the short lifetime of the WN phase implies a burst cycle of order ∼50 Myr, consistent with galaxies repeatedly cycling through short, bursty episodes of enrichment. Thus, the GLIMPSE-D spectrum of RXCJ2248-ID3 provides not only the first direct evidence of WN stars shaping the chemical evolution of z > 5 galaxies but also a timing argument that situates N/O outliers as a natural, fleeting, phase of high-redshift star formation.\r\n\r\nTaken together, our findings are a glimpse into a short-lived phase of chemically selective enrichment from WN stars at cosmic dawn, providing a physically self-consistent solution to the extreme N/O enhancement and relative C/O depletion observed in RXCJ2248-ID3 and galaxies like it. Thus, RXCJ2248-ID3 serves as a benchmark case for interpreting chemically enriched, stratified, multiphase starbursts in the early Universe.\r\n\r\nAcknowledgments\r\nWe thank the referee for their thorough review of our calculations and analysis and for their helpful suggestions, which greatly improved the robustness of our results and the clarity of the text. 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 #9223. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. We acknowledge the support of the Canadian Space Agency (CSA) [25JWGO4A06]. HA acknowledges support from CNES, focused on the JWST mission, and the Programme National Cosmology and Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES and support by the French National Research Agency (ANR) under grant ANR-21-CE31-0838. The JWST data presented in this article from program #9223 were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via DOI: 10.17909/8642-1k68.","article_number":"112","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy","abstract":[{"text":"We present the discovery of extreme nitrogen enrichment by Wolf Rayet nitrogen (WN) stars in the metal-poor (∼10%Z⊙), lensed, compact (Reff ∼ 20 pc) galaxy RXCJ2248 at z = 6.1, revealed by unprecedentedly deep\r\nJWST/NIRSpec medium-resolution spectroscopy from the GLIMPSE-D Survey. The exquisite signal-to-noise\r\nratio reveals multiple high-ionization nebular lines and broad Balmer and [O III] components (FWHM\r\n∼700–3000 km s\r\n−1\r\n). We detect broadened He II λ1640 and λ4687 (FWHM ∼ 530 km s\r\n−1\r\n) and strong N III λ4642\r\nemission consistent with a population of WN stars, making RXCJ2248 the most distant galaxy with confirmed\r\nWolf Rayet (WR) features to date. We measure the multiphase nebular density across five ions, the direct-method\r\nmetallicity (\r\n12 + log(O/H) = 7.753 ± 0.025\r\n), and a nonuniform elemental enrichment pattern of extreme N/O\r\nenhancement (\r\nlog(N/O) = 0.391 ± 0.037\r\nfrom N+, N+2\r\n, and N+3\r\n) but suppressed C/O relative to empirical\r\nC/N trends. We show that this abundance pattern can be explained by enrichment from a dual-burst with a low\r\nWR carbon/WN ratio, as expected at low metallicities. Crucially, these signatures can only arise during a brief,\r\nrare evolutionary window shortly after a burst (∼3–6 Myr), when WN stars dominate chemical feedback but\r\nbefore dilution by later yields (e.g., supernovae). The observed frequency of strong N emitters at high−z implies a\r\n∼50 Myr burst duty cycle, suggesting that N/O outliers may represent a brief but ubiquitous phase in the\r\nevolution of highly star-forming early galaxies. The WN detection in RXCJ2248, therefore, provides the first\r\ndirect evidence of WR-driven nitrogen enrichment in the first billion years of the Universe and a novel timing\r\nargument for the bursty star formation cycles that shaped galaxies at cosmic dawn.","lang":"eng"}],"DOAJ_listed":"1","external_id":{"arxiv":["2511.13591"]},"year":"2026","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"month":"05","type":"journal_article","date_updated":"2026-06-02T08:46:20Z","OA_place":"publisher","intvolume":"      1003","quality_controlled":"1","status":"public","file":[{"date_updated":"2026-06-02T08:46:08Z","success":1,"relation":"main_file","creator":"dernst","file_size":21249354,"content_type":"application/pdf","date_created":"2026-06-02T08:46:08Z","access_level":"open_access","file_id":"21938","file_name":"2026_AstrophysicalJour_Berg.pdf","checksum":"1058555fdede45e10fca25d74e7977bc"}],"author":[{"full_name":"Berg, Danielle A.","first_name":"Danielle A.","last_name":"Berg"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Chisholm","full_name":"Chisholm, John","first_name":"John"},{"last_name":"Atek","full_name":"Atek, Hakim","first_name":"Hakim"},{"last_name":"Fujimoto","full_name":"Fujimoto, Seiji","first_name":"Seiji"},{"last_name":"Kokorev","first_name":"Vasily","full_name":"Kokorev, Vasily"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"first_name":"Chiaki","full_name":"Kobayashi, Chiaki","last_name":"Kobayashi"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"full_name":"Fei, Qinyue","first_name":"Qinyue","last_name":"Fei"},{"first_name":"Damien","full_name":"Korber, Damien","last_name":"Korber"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Marques-Chaves, Rui","first_name":"Rui","last_name":"Marques-Chaves"},{"full_name":"Martinez, Zorayda","first_name":"Zorayda","last_name":"Martinez"},{"last_name":"Mcquinn","first_name":"Kristen B.W.","full_name":"Mcquinn, Kristen B.W."},{"full_name":"Muñoz, Julian B.","first_name":"Julian B.","last_name":"Muñoz"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"last_name":"Saldana-Lopez","full_name":"Saldana-Lopez, Alberto","first_name":"Alberto"},{"full_name":"Stark, Daniel P.","first_name":"Daniel P.","last_name":"Stark"},{"last_name":"Stephenson","first_name":"Mabel G.","full_name":"Stephenson, Mabel G."},{"last_name":"Hsiao","full_name":"Hsiao, Tiger Yu Yang","first_name":"Tiger Yu Yang"}],"oa":1,"publisher":"IOP Publishing","date_created":"2026-05-31T22:02:12Z","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"oa_version":"Published Version","arxiv":1,"PlanS_conform":"1","article_type":"original","has_accepted_license":"1","article_processing_charge":"Yes","citation":{"ieee":"D. A. Berg <i>et al.</i>, “A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy,” <i>The Astrophysical Journal</i>, vol. 1003, no. 2. IOP Publishing, 2026.","apa":"Berg, D. A., Naidu, R. P., Chisholm, J., Atek, H., Fujimoto, S., Kokorev, V., … Hsiao, T. Y. Y. (2026). A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae5e4c\">https://doi.org/10.3847/1538-4357/ae5e4c</a>","chicago":"Berg, Danielle A., Rohan P. Naidu, John Chisholm, Hakim Atek, Seiji Fujimoto, Vasily Kokorev, Lukas J. Furtak, et al. “A Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae5e4c\">https://doi.org/10.3847/1538-4357/ae5e4c</a>.","short":"D.A. Berg, R.P. Naidu, J. Chisholm, H. Atek, S. Fujimoto, V. Kokorev, L.J. Furtak, C. Kobayashi, D. Schaerer, A. Adamo, Q. Fei, D. Korber, J.J. Matthee, R. Marques-Chaves, Z. Martinez, K.B.W. Mcquinn, J.B. Muñoz, P.A. Oesch, A. Saldana-Lopez, D.P. Stark, M.G. Stephenson, T.Y.Y. Hsiao, The Astrophysical Journal 1003 (2026).","ama":"Berg DA, Naidu RP, Chisholm J, et al. A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. <i>The Astrophysical Journal</i>. 2026;1003(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae5e4c\">10.3847/1538-4357/ae5e4c</a>","ista":"Berg DA, Naidu RP, Chisholm J, Atek H, Fujimoto S, Kokorev V, Furtak LJ, Kobayashi C, Schaerer D, Adamo A, Fei Q, Korber D, Matthee JJ, Marques-Chaves R, Martinez Z, Mcquinn KBW, Muñoz JB, Oesch PA, Saldana-Lopez A, Stark DP, Stephenson MG, Hsiao TYY. 2026. A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. The Astrophysical Journal. 1003(2), 112.","mla":"Berg, Danielle A., et al. “A Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy.” <i>The Astrophysical Journal</i>, vol. 1003, no. 2, 112, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae5e4c\">10.3847/1538-4357/ae5e4c</a>."},"publication_status":"published","ddc":["520"],"day":"20","volume":1003,"OA_type":"gold","date_published":"2026-05-20T00:00:00Z"},{"publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"publisher":"IOP Publishing","date_created":"2026-06-14T22:01:42Z","PlanS_conform":"1","article_type":"original","oa_version":"Published Version","arxiv":1,"intvolume":"      1004","quality_controlled":"1","date_updated":"2026-06-19T09:58:52Z","OA_place":"publisher","file":[{"file_name":"2026_AstrophysicalJour_Li.pdf","checksum":"bb76fbb51f8d2834cb79f19e7932e3bd","file_id":"22099","access_level":"open_access","date_created":"2026-06-19T09:56:29Z","content_type":"application/pdf","file_size":3386217,"creator":"dernst","relation":"main_file","success":1,"date_updated":"2026-06-19T09:56:29Z"}],"oa":1,"author":[{"first_name":"Zhenwei","full_name":"Li, Zhenwei","last_name":"Li"},{"id":"5dd129bd-0601-11ef-b325-833284687b76","first_name":"Dandan","full_name":"Wei, Dandan","last_name":"Wei"},{"last_name":"Jia","full_name":"Jia, Shi","first_name":"Shi"},{"last_name":"Chen","full_name":"Chen, Hailiang","first_name":"Hailiang"},{"last_name":"Ge","full_name":"Ge, Hongwei","first_name":"Hongwei"},{"last_name":"Chen","first_name":"Zhuo","full_name":"Chen, Zhuo"},{"last_name":"Zhang","full_name":"Zhang, Yangyang","first_name":"Yangyang"},{"last_name":"Chen","full_name":"Chen, Xuefei","first_name":"Xuefei"},{"last_name":"Han","full_name":"Han, Zhanwen","first_name":"Zhanwen"}],"status":"public","volume":1004,"OA_type":"gold","citation":{"chicago":"Li, Zhenwei, Dandan Wei, Shi Jia, Hailiang Chen, Hongwei Ge, Zhuo Chen, Yangyang Zhang, Xuefei Chen, and Zhanwen Han. “A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-Ray Binaries.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae66fd\">https://doi.org/10.3847/1538-4357/ae66fd</a>.","ieee":"Z. Li <i>et al.</i>, “A path to constraints on common envelope ejection in massive binaries: Full evolutionary reconstruction of three Black Hole X-ray binaries,” <i>The Astrophysical Journal</i>, vol. 1004, no. 1. IOP Publishing, 2026.","apa":"Li, Z., Wei, D., Jia, S., Chen, H., Ge, H., Chen, Z., … Han, Z. (2026). A path to constraints on common envelope ejection in massive binaries: Full evolutionary reconstruction of three Black Hole X-ray binaries. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae66fd\">https://doi.org/10.3847/1538-4357/ae66fd</a>","short":"Z. Li, D. Wei, S. Jia, H. Chen, H. Ge, Z. Chen, Y. Zhang, X. Chen, Z. Han, The Astrophysical Journal 1004 (2026).","ama":"Li Z, Wei D, Jia S, et al. A path to constraints on common envelope ejection in massive binaries: Full evolutionary reconstruction of three Black Hole X-ray binaries. <i>The Astrophysical Journal</i>. 2026;1004(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae66fd\">10.3847/1538-4357/ae66fd</a>","ista":"Li Z, Wei D, Jia S, Chen H, Ge H, Chen Z, Zhang Y, Chen X, Han Z. 2026. A path to constraints on common envelope ejection in massive binaries: Full evolutionary reconstruction of three Black Hole X-ray binaries. The Astrophysical Journal. 1004(1), 31.","mla":"Li, Zhenwei, et al. “A Path to Constraints on Common Envelope Ejection in Massive Binaries: Full Evolutionary Reconstruction of Three Black Hole X-Ray Binaries.” <i>The Astrophysical Journal</i>, vol. 1004, no. 1, 31, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae66fd\">10.3847/1538-4357/ae66fd</a>."},"article_processing_charge":"Yes","day":"10","publication_status":"published","ddc":["520"],"date_published":"2026-06-10T00:00:00Z","has_accepted_license":"1","file_date_updated":"2026-06-19T09:56:29Z","scopus_import":"1","doi":"10.3847/1538-4357/ae66fd","issue":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"_id":"21997","department":[{"_id":"YlGo"}],"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2604.10440"]},"year":"2026","month":"06","type":"journal_article","article_number":"31","acknowledgement":"We deeply thank the referee for a very careful reading and constructive comments that have led to the improvement of the manuscript. The authors are grateful to Poshak Gandhi for his valuable suggestions and feedback on this work. This work is supported by the Natural Science Foundation of China (grant Nos. 12125303, 12525304, 12288102, 12473034, 12103028, 12333008, 12422305, 12090040/3, 12273105, 11703081, 11422324, 12073070, and 12173081), the CAS Project for Young Scientists in Basic Research (YSBR-148), the Strategic Priority Research Program of the Chinese Academy of Sciences (grant Nos. XDB1160303, XDB1160201, and XDB1160000), the National Key R&D Program of China (grant Nos. 2021YFA1600403 and 2021YFA1600400), the Key Research Program of Frontier Sciences of CAS (No. ZDBS-LY-7005), the “CAS Light of West China”, the Yunnan Revitalization Talent Support Program-Science & Technology Champion Project (No. 202305AB350003) and Young Talent Project, the International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research (Nos. 202302AN360001 and 202201BC070003), Yunnan Fundamental Research Projects (No. 202401AT070139), and the Natural Science Foundation of Henan Province (No. 242300420944). X.C. acknowledges the New Cornerstone Science Foundation through the XPLORER PRIZE. The authors gratefully acknowledge the “PHOENIX Supercomputing Platform” jointly operated by the Binary Population Synthesis Group and the Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences.","DOAJ_listed":"1","abstract":[{"lang":"eng","text":"The massive binary common envelope (CE) phase plays a pivotal role in the formation of close black hole (BH)/neutron star binaries, yet significant uncertainties remain in our understanding of this process. In this study, we aim to constrain the massive binary CE phase by systematically reconstructing three observed BH X-ray binaries (BHXBs): GRO J1655-40, SAX J1819.3-2525, and 4U 1543-47. Through comprehensive binary evolution simulations and parametric supernova modeling, we establish lower limits for the CE efficiency parameters under different energy considerations within the standard energy formalism. Specifically, we derive minimum values for three cases: α0.5U and αU, representing CE efficiencies with half and all of the internal energy contributing to the envelope ejection, respectively, and αH, accounting for the envelope’s enthalpy. Our analysis reveals that the self-consistent formation of these three BHXBs requires CE efficiency parameters satisfying α0.5U ≳ 6.7, αU ≳ 4.2, and αH ≳ 1.7. Notably, we find no viable solutions with CE efficiency values below unity, even when considering the most extreme scenarios, in which the envelope binding energy is significantly reduced through enthalpy inclusion. Our results strongly imply that either additional energy sources are required or the formalism itself must be revised. Furthermore, we quantitatively assess the impact of BH natal kicks on our results. A key finding is that 4U 1543-47’s formation requires substantial natal kicks (≳50 km s−1), as lower kick velocities are incompatible with isolated binary evolution."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"A path to constraints on common envelope ejection in massive binaries: Full evolutionary reconstruction of three Black Hole X-ray binaries"},{"acknowledgement":"We thank the anonymous referee for insightful comments, which significantly improved the manuscript. We acknowledge Kohei Inayoshi for helpful discussions. 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. The specific observations analyzed can be accessed via DOI: 10.17909/4byn-fe55 and 10.17909/v2y7-j922. These observations are associated with programs #3293 and #9223. S.F. and Q.F. acknowledge support from the Dunlap Institute, which is funded through an endowment established by the David Dunlap family and the University of Toronto. A.S.L. acknowledges support from the Knut and Alice Wallenberg Foundation. A.Z. 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.","article_number":"244","title":"A GLIMPSE of intermediate mass Black Holes in the epoch of reionization: Witnessing the descendants of direct collapse?","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"JWST has revealed an abundance of supermassive black holes (BHs) in the early Universe, and yet the lowest mass seed BHs that gave rise to these populations remain elusive. Here, we present a systematic search for broad-line active galactic nuclei (AGNs) in some of the faintest high-z galaxies surveyed yet by combining ultra-deep JWST/NIRSpec G395M spectroscopy with the strong lensing aid in AS1063. By employing the profile of the [O iii]λ5007 emission lines as a template for narrow-line components and carefully cross-validating with mock observations, we identify a sample of 10 broad-line AGNs at 4.5 < z < 7.0 (eight secure, two tentative). The inferred BH masses from the broad Hα line explore the intermediate BH mass regime down to ∼105.5 M⊙. The stellar mass (M*) is estimated with a galaxy+AGN composite model, and we find the BH to stellar mass ratio spans down to MBH/M* ≲ 0.1%, unveiling populations on the empirical MBH–M* relation observed in the local Universe. We also derive the BH mass function and investigate its low-mass end at this epoch. While we confirm the agreement of our results with previous studies at MBH ≳ 106.5M⊙, we find the mass range of ∼105.5 M⊙ features an enhanced abundance with respect to the extrapolated best-fit Schechter function. Comparison with theoretical models suggests that a possible origin for this enhanced abundance is the direct-collapse BH formation, supporting the scenario that the direct collapse of massive gas clouds is a significant pathway for the earliest supermassive BHs.","lang":"eng"}],"DOAJ_listed":"1","year":"2026","external_id":{"arxiv":["2509.20452"]},"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","month":"06","researchdata_availability":"yes","department":[{"_id":"JoMa"}],"_id":"21999","file_date_updated":"2026-06-22T08:03:55Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"doi":"10.3847/1538-4357/ae6248","issue":"2","scopus_import":"1","has_accepted_license":"1","publication_status":"published","day":"01","ddc":["520"],"article_processing_charge":"Yes","supplementarymaterial":"yes","citation":{"apa":"Fei, Q., Fujimoto, S., Naidu, R. P., Chisholm, J., Atek, H., Brammer, G., … Zitrin, A. (2026). A GLIMPSE of intermediate mass Black Holes in the epoch of reionization: Witnessing the descendants of direct collapse? <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae6248\">https://doi.org/10.3847/1538-4357/ae6248</a>","ieee":"Q. Fei <i>et al.</i>, “A GLIMPSE of intermediate mass Black Holes in the epoch of reionization: Witnessing the descendants of direct collapse?,” <i>The Astrophysical Journal</i>, vol. 1003, no. 2. IOP Publishing, 2026.","chicago":"Fei, Qinyue, Seiji Fujimoto, Rohan P. Naidu, John Chisholm, Hakim Atek, Gabriel Brammer, Yoshihisa Asada, et al. “A GLIMPSE of Intermediate Mass Black Holes in the Epoch of Reionization: Witnessing the Descendants of Direct Collapse?” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae6248\">https://doi.org/10.3847/1538-4357/ae6248</a>.","mla":"Fei, Qinyue, et al. “A GLIMPSE of Intermediate Mass Black Holes in the Epoch of Reionization: Witnessing the Descendants of Direct Collapse?” <i>The Astrophysical Journal</i>, vol. 1003, no. 2, 244, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae6248\">10.3847/1538-4357/ae6248</a>.","ista":"Fei Q, Fujimoto S, Naidu RP, Chisholm J, Atek H, Brammer G, Asada Y, Berg DA, Bromm V, Furtak LJ, Greene JE, Hsiao TYY, Jeon J, Kokorev V, Matthee JJ, Natarajan P, Pan R, Richard J, Saldana-Lopez A, Schaerer D, Volonteri M, Zitrin A. 2026. A GLIMPSE of intermediate mass Black Holes in the epoch of reionization: Witnessing the descendants of direct collapse? The Astrophysical Journal. 1003(2), 244.","ama":"Fei Q, Fujimoto S, Naidu RP, et al. A GLIMPSE of intermediate mass Black Holes in the epoch of reionization: Witnessing the descendants of direct collapse? <i>The Astrophysical Journal</i>. 2026;1003(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae6248\">10.3847/1538-4357/ae6248</a>","short":"Q. Fei, S. Fujimoto, R.P. Naidu, J. Chisholm, H. Atek, G. Brammer, Y. Asada, D.A. Berg, V. Bromm, L.J. Furtak, J.E. Greene, T.Y.Y. Hsiao, J. Jeon, V. Kokorev, J.J. Matthee, P. Natarajan, R. Pan, J. Richard, A. Saldana-Lopez, D. Schaerer, M. Volonteri, A. Zitrin, The Astrophysical Journal 1003 (2026)."},"OA_type":"gold","volume":1003,"date_published":"2026-06-01T00:00:00Z","OA_place":"publisher","date_updated":"2026-06-22T11:34:52Z","quality_controlled":"1","intvolume":"      1003","status":"public","author":[{"full_name":"Fei, Qinyue","first_name":"Qinyue","last_name":"Fei"},{"last_name":"Fujimoto","first_name":"Seiji","full_name":"Fujimoto, Seiji"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"last_name":"Atek","full_name":"Atek, Hakim","first_name":"Hakim"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"first_name":"Yoshihisa","full_name":"Asada, Yoshihisa","last_name":"Asada"},{"full_name":"Berg, Danielle A.","first_name":"Danielle A.","last_name":"Berg"},{"full_name":"Bromm, Volker","first_name":"Volker","last_name":"Bromm"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"Hsiao","first_name":"Tiger Yu Yang","full_name":"Hsiao, Tiger Yu Yang"},{"last_name":"Jeon","full_name":"Jeon, Junehyoung","first_name":"Junehyoung"},{"last_name":"Kokorev","first_name":"Vasily","full_name":"Kokorev, Vasily"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"Priyamvada","full_name":"Natarajan, Priyamvada","last_name":"Natarajan"},{"last_name":"Pan","first_name":"Richard","full_name":"Pan, Richard"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"full_name":"Saldana-Lopez, Alberto","first_name":"Alberto","last_name":"Saldana-Lopez"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"first_name":"Marta","full_name":"Volonteri, Marta","last_name":"Volonteri"},{"last_name":"Zitrin","full_name":"Zitrin, Adi","first_name":"Adi"}],"oa":1,"file":[{"file_name":"2026_AstrophysicalJour_Fei.pdf","checksum":"b04247996b8dcd0eb5387581706d1106","file_id":"22112","access_level":"open_access","date_created":"2026-06-22T08:03:55Z","content_type":"application/pdf","file_size":19681834,"relation":"main_file","creator":"dernst","date_updated":"2026-06-22T08:03:55Z","success":1}],"date_created":"2026-06-14T22:01:43Z","publisher":"IOP Publishing","language":[{"iso":"eng"}],"dataavailabilitystatement":"10.17909/4byn-fe55 and 10.17909/v2y7-j922 used with Software: LMFIT (M. Newville et al. 2014) msafit (A. de Graaff et al. 2024). - Text extracted from Acknowledgements, no separate DAS","publication":"The Astrophysical Journal","arxiv":1,"oa_version":"Published Version","das_tickbox":"0","article_type":"original","PlanS_conform":"1"},{"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"year":"2025","external_id":{"arxiv":["2504.12460"]},"type":"journal_article","month":"12","article_number":"36","acknowledgement":"We thank Fulvio Ferlito, Ana Maria Delgado, and Ken Osato for helpful conversations during this work. M.E.L. is supported by NSF grant DGE-2036197. Z.H. acknowledges financial support from NASA ATP grant 80NSSC24K1093. The Flatiron Institute is supported by the Simons Foundation.","abstract":[{"text":"The next generation of weak-gravitational-lensing surveys has the potential to place stringent constraints on cosmological parameters. However, their analysis is limited by systematics such as the intrinsic alignments of galaxies, which alter weak-lensing convergence and can lead to biases in cosmological parameter estimations. For the first time, in this work, we investigate the impact of intrinsic alignments on non-Gaussian statistics of the weak-lensing field using galaxy shapes derived from the IllustrisTNG hydrodynamical simulation. We create two catalogs of ray-traced convergence maps: one that includes the measured intrinsic shape of each galaxy and another where all galaxies are randomly rotated to eliminate intrinsic alignments. We compare a range of weak-lensing statistics between the two catalogs, including the shear–shear correlation function, the map-level angular power spectrum, one-point, peak count, and minimum distribution functions, and Minkowski functionals. For each statistic, we assess the level of statistical distinguishability between catalogs for a set of future survey angular areas. Our results reveal strong small-scale correlation in the alignment of galaxies and statistically significant boosts in weak-lensing convergence in both positive and negative directions for high-significance peaks and minima, respectively. We note that our analysis is at a fixed number density of  ˜ 5 arcmin^-2, drawn from a single realization of initial conditions, and does not include observational uncertainties or supersample covariance contributions. Weak-lensing analyses utilizing non-Gaussian statistics must account for intrinsic alignments to avoid significantly compromised cosmological inferences.","lang":"eng"}],"DOAJ_listed":"1","title":"The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file_date_updated":"2026-04-13T08:20:16Z","scopus_import":"1","doi":"10.3847/1538-4357/ae1ca7","issue":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"_id":"21724","department":[{"_id":"ZoHa"}],"OA_type":"gold","volume":996,"ddc":["520"],"publication_status":"published","day":"23","citation":{"ama":"Lee ME, Haiman Z, Pandey S, Genel S. The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. <i>The Astrophysical Journal</i>. 2025;996(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1ca7\">10.3847/1538-4357/ae1ca7</a>","ista":"Lee ME, Haiman Z, Pandey S, Genel S. 2025. The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. The Astrophysical Journal. 996(1), 36.","mla":"Lee, Max E., et al. “The Effect of Intrinsic Alignments on Weak-Lensing Statistics in Hydrodynamical Simulations.” <i>The Astrophysical Journal</i>, vol. 996, no. 1, 36, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1ca7\">10.3847/1538-4357/ae1ca7</a>.","short":"M.E. Lee, Z. Haiman, S. Pandey, S. Genel, The Astrophysical Journal 996 (2025).","apa":"Lee, M. E., Haiman, Z., Pandey, S., &#38; Genel, S. (2025). The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae1ca7\">https://doi.org/10.3847/1538-4357/ae1ca7</a>","ieee":"M. E. Lee, Z. Haiman, S. Pandey, and S. Genel, “The effect of intrinsic alignments on weak-lensing statistics in hydrodynamical simulations,” <i>The Astrophysical Journal</i>, vol. 996, no. 1. IOP Publishing, 2025.","chicago":"Lee, Max E., Zoltán Haiman, Shivam Pandey, and Shy Genel. “The Effect of Intrinsic Alignments on Weak-Lensing Statistics in Hydrodynamical Simulations.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ae1ca7\">https://doi.org/10.3847/1538-4357/ae1ca7</a>."},"article_processing_charge":"Yes","date_published":"2025-12-23T00:00:00Z","has_accepted_license":"1","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","publisher":"IOP Publishing","date_created":"2026-04-12T22:01:52Z","article_type":"original","PlanS_conform":"1","arxiv":1,"oa_version":"Published Version","quality_controlled":"1","intvolume":"       996","OA_place":"publisher","date_updated":"2026-04-13T08:30:52Z","author":[{"first_name":"Max E.","full_name":"Lee, Max E.","last_name":"Lee"},{"last_name":"Haiman","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"last_name":"Pandey","first_name":"Shivam","full_name":"Pandey, Shivam"},{"first_name":"Shy","full_name":"Genel, Shy","last_name":"Genel"}],"oa":1,"file":[{"success":1,"date_updated":"2026-04-13T08:20:16Z","relation":"main_file","creator":"dernst","content_type":"application/pdf","file_size":4122087,"date_created":"2026-04-13T08:20:16Z","access_level":"open_access","file_id":"21732","checksum":"0d8fa05617420230eac39944b36839e9","file_name":"2025_AstrophysicalJournal_Lee.pdf"}],"status":"public"},{"publication_status":"published","day":"20","ddc":["520"],"article_processing_charge":"Yes","citation":{"ama":"Rinaldi P, Pérez-González PG, Rieke GH, et al. Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. <i>The Astrophysical Journal</i>. 2025;994(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae089c\">10.3847/1538-4357/ae089c</a>","ista":"Rinaldi P, Pérez-González PG, Rieke GH, Lyu J, D’Eugenio F, Wu Z, Carniani S, Looser TJ, Shivaei I, Boogaard LA, Diaz-Santos T, Colina L, Östlin G, Alberts S, Álvarez-Márquez J, Annuziatella M, Aravena M, Bhatawdekar R, Bunker AJ, Caputi KI, Charlot S, Crespo Gómez A, Curti M, Eckart A, Gillman S, Hainline K, Kumari N, Hjorth J, Iani E, Inami H, Ji Z, Johnson BD, Jones GC, Labiano Á, Maiolino R, Melinder J, Moutard T, Peissker F, Rieke M, Robertson B, Scholtz J, Tacchella S, Van Der Werf PP, Walter F, Williams CC, Willott C, Witstok J, Übler H, Zhu Y. 2025. Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. The Astrophysical Journal. 994(1), 86.","mla":"Rinaldi, Pierluigi, et al. “Deciphering the Nature of Virgil: An Obscured Active Galactic Nucleus Lurking within an Apparently Normal Lyα Emitter during Cosmic Reionization.” <i>The Astrophysical Journal</i>, vol. 994, no. 1, 86, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae089c\">10.3847/1538-4357/ae089c</a>.","short":"P. Rinaldi, P.G. Pérez-González, G.H. Rieke, J. Lyu, F. D’Eugenio, Z. Wu, S. Carniani, T.J. Looser, I. Shivaei, L.A. Boogaard, T. Diaz-Santos, L. Colina, G. Östlin, S. Alberts, J. Álvarez-Márquez, M. Annuziatella, M. Aravena, R. Bhatawdekar, A.J. Bunker, K.I. Caputi, S. Charlot, A. Crespo Gómez, M. Curti, A. Eckart, S. Gillman, K. Hainline, N. Kumari, J. Hjorth, E. Iani, H. Inami, Z. Ji, B.D. Johnson, G.C. Jones, Á. Labiano, R. Maiolino, J. Melinder, T. Moutard, F. Peissker, M. Rieke, B. Robertson, J. Scholtz, S. Tacchella, P.P. Van Der Werf, F. Walter, C.C. Williams, C. Willott, J. Witstok, H. Übler, Y. Zhu, The Astrophysical Journal 994 (2025).","apa":"Rinaldi, P., Pérez-González, P. G., Rieke, G. H., Lyu, J., D’Eugenio, F., Wu, Z., … Zhu, Y. (2025). Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae089c\">https://doi.org/10.3847/1538-4357/ae089c</a>","ieee":"P. Rinaldi <i>et al.</i>, “Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization,” <i>The Astrophysical Journal</i>, vol. 994, no. 1. IOP Publishing, 2025.","chicago":"Rinaldi, Pierluigi, Pablo G. Pérez-González, George H. Rieke, Jianwei Lyu, Francesco D’Eugenio, Zihao Wu, Stefano Carniani, et al. “Deciphering the Nature of Virgil: An Obscured Active Galactic Nucleus Lurking within an Apparently Normal Lyα Emitter during Cosmic Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ae089c\">https://doi.org/10.3847/1538-4357/ae089c</a>."},"OA_type":"gold","volume":994,"date_published":"2025-11-20T00:00:00Z","has_accepted_license":"1","publisher":"IOP Publishing","date_created":"2026-04-12T22:01:53Z","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","oa_version":"Published Version","article_type":"original","PlanS_conform":"1","OA_place":"publisher","date_updated":"2026-04-13T07:54:11Z","intvolume":"       994","quality_controlled":"1","status":"public","author":[{"last_name":"Rinaldi","full_name":"Rinaldi, Pierluigi","first_name":"Pierluigi"},{"last_name":"Pérez-González","full_name":"Pérez-González, Pablo G.","first_name":"Pablo G."},{"full_name":"Rieke, George H.","first_name":"George H.","last_name":"Rieke"},{"full_name":"Lyu, Jianwei","first_name":"Jianwei","last_name":"Lyu"},{"last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco","first_name":"Francesco"},{"last_name":"Wu","full_name":"Wu, Zihao","first_name":"Zihao"},{"last_name":"Carniani","full_name":"Carniani, Stefano","first_name":"Stefano"},{"last_name":"Looser","first_name":"Tobias J.","full_name":"Looser, Tobias J."},{"last_name":"Shivaei","first_name":"Irene","full_name":"Shivaei, Irene"},{"first_name":"Leindert A.","full_name":"Boogaard, Leindert A.","last_name":"Boogaard"},{"last_name":"Diaz-Santos","first_name":"Tanio","full_name":"Diaz-Santos, Tanio"},{"last_name":"Colina","first_name":"Luis","full_name":"Colina, Luis"},{"first_name":"Göran","full_name":"Östlin, Göran","last_name":"Östlin"},{"full_name":"Alberts, Stacey","first_name":"Stacey","last_name":"Alberts"},{"full_name":"Álvarez-Márquez, Javier","first_name":"Javier","last_name":"Álvarez-Márquez"},{"last_name":"Annuziatella","first_name":"Marianna","full_name":"Annuziatella, Marianna"},{"full_name":"Aravena, Manuel","first_name":"Manuel","last_name":"Aravena"},{"last_name":"Bhatawdekar","first_name":"Rachana","full_name":"Bhatawdekar, Rachana"},{"last_name":"Bunker","full_name":"Bunker, Andrew J.","first_name":"Andrew J."},{"full_name":"Caputi, Karina I.","first_name":"Karina I.","last_name":"Caputi"},{"last_name":"Charlot","full_name":"Charlot, Stéphane","first_name":"Stéphane"},{"last_name":"Crespo Gómez","full_name":"Crespo Gómez, Alejandro","first_name":"Alejandro"},{"first_name":"Mirko","full_name":"Curti, Mirko","last_name":"Curti"},{"first_name":"Andreas","full_name":"Eckart, Andreas","last_name":"Eckart"},{"first_name":"Steven","full_name":"Gillman, Steven","last_name":"Gillman"},{"first_name":"Kevin","full_name":"Hainline, Kevin","last_name":"Hainline"},{"last_name":"Kumari","full_name":"Kumari, Nimisha","first_name":"Nimisha"},{"full_name":"Hjorth, Jens","first_name":"Jens","last_name":"Hjorth"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","first_name":"Edoardo","last_name":"Iani","orcid":"0000-0001-8386-3546"},{"last_name":"Inami","full_name":"Inami, Hanae","first_name":"Hanae"},{"full_name":"Ji, Zhiyuan","first_name":"Zhiyuan","last_name":"Ji"},{"last_name":"Johnson","full_name":"Johnson, Benjamin D.","first_name":"Benjamin D."},{"last_name":"Jones","first_name":"Gareth C.","full_name":"Jones, Gareth C."},{"last_name":"Labiano","first_name":"Álvaro","full_name":"Labiano, Álvaro"},{"last_name":"Maiolino","full_name":"Maiolino, Roberto","first_name":"Roberto"},{"full_name":"Melinder, Jens","first_name":"Jens","last_name":"Melinder"},{"last_name":"Moutard","first_name":"Thibaud","full_name":"Moutard, Thibaud"},{"full_name":"Peissker, Florian","first_name":"Florian","last_name":"Peissker"},{"full_name":"Rieke, Marcia","first_name":"Marcia","last_name":"Rieke"},{"last_name":"Robertson","full_name":"Robertson, Brant","first_name":"Brant"},{"last_name":"Scholtz","first_name":"Jan","full_name":"Scholtz, Jan"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"first_name":"Paul P.","full_name":"Van Der Werf, Paul P.","last_name":"Van Der Werf"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"},{"first_name":"Chris","full_name":"Willott, Chris","last_name":"Willott"},{"last_name":"Witstok","full_name":"Witstok, Joris","first_name":"Joris"},{"last_name":"Übler","first_name":"Hannah","full_name":"Übler, Hannah"},{"last_name":"Zhu","first_name":"Yongda","full_name":"Zhu, Yongda"}],"oa":1,"file":[{"file_size":10298729,"content_type":"application/pdf","success":1,"date_updated":"2026-04-13T07:53:00Z","creator":"dernst","relation":"main_file","file_id":"21731","checksum":"5d13b0ad3e9f56cbe29c5de0ba5757c8","file_name":"2025_AstrophysicalJournal_Rinaldi.pdf","date_created":"2026-04-13T07:53:00Z","access_level":"open_access"}],"year":"2025","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","month":"11","acknowledgement":"The authors are deeply grateful to Antonello Calabrò for valuable insights on CLOUDY and pyCloudy, and for publicly sharing their SFG and AGN models, which were used as a reference to verify the consistency of our photoionization models. The authors also thank Adam Carnall for insightful input on bagpipes and for assistance with the implementation of the two-population model adopted in this work. Finally, they also thank Camilla Pacifici, Vasily Kokorev, and Cristian Vignali for their insightful discussions.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST programs GTO #1180, GO #1210, GTO#1283, GO #1963, GO #1895, GO# 3215, and GO#6511.\r\n\r\nThe authors acknowledge the FRESCO, JEMS, and #3215 teams led by co-PIs P. Oesch, C. C. Williams, M. Maseda, D. Eisenstein, and R. Maiolino for developing their observing program with a zero-exclusive-access period. Processing for the JADES NIRCam data release was performed on the lux cluster at the University of California, Santa Cruz, funded by NSF MRI grant AST 1828315. Also based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 526555. The data presented in this article were obtained from MAST at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi: 10.17909/1rq3-8048 P. Oesch & D. Magee (2023), C. Williams et al. (2023), G. Illingworth (2015), and M. Rieke et al. (2023).\r\n\r\nA.J.B. acknowledges funding from the “FirstGalaxies” Advanced Grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 789056).\r\n\r\nP.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by the Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER, UE.\r\n\r\nB.E.R. acknowledges support from the NIRCam Science Team contract to the University of Arizona, NAS5-02015, and JWST Program 3215.\r\n\r\nS.T. acknowledges support by the Royal Society Research Grant G125142.\r\n\r\nThe research of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.\r\n\r\nJ.W. gratefully acknowledges support from the Cosmic Dawn Center through the DAWN Fellowship. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140.\r\n\r\nY.Z., Z.J., and P.L. gratefully acknowledge the JWST/NIRCam contract to the University of Arizona NAS5-02015.\r\n\r\nThe work of G.H.R. and P.L. was also supported by grant 80NSSC18K0555, from the NASA Goddard Space Flight Center to the University of Arizona.\r\n\r\nH.Ü. acknowledges funding by the European Union (ERC APEX, 101164796). 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 Executive Agency. Neither the European Union nor the granting authority can be held responsible for them.\r\n\r\nG.C.J. acknowledges support by the Science and Technology Facilities Council (STFC), ERC Advanced grant 695671 “QUENCH.”\r\n\r\nA.C.G. acknowledges support by JWST contract B0215/JWST-GO-02926.\r\n\r\nG.O. acknowledges support from the Swedish National Space Agency (SNSA).\r\n\r\nH.I. acknowledges support from JSPS KAKENHI grant No. JP21H01129.\r\n\r\nM.A. gratefully acknowledges support from ANID Basal Project FB210003 and ANID MILENIO NCN2024_112.\r\n\r\nT.D.S. acknowledges the research project was supported by the Hellenic Foundation for Research and Innovation (HFRI) under the “2nd Call for HFRI Research Projects to Support Faculty Members and Researchers” (project No.: 03382).\r\n\r\nR.M. 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. R.M. also acknowledges funding from a research professorship from the Royal Society.\r\n\r\nI.S. acknowledges funding from the Atraccíon de Talento grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain, and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant No. 101117541, DistantDust).\r\n\r\nK.I.C. acknowledges funding from the Dutch Research Council (NWO) through the award of the Vici grant VI.C.212.036.\r\n\r\nFacilities: HST - Hubble Space Telescope satellite, JWST. -\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2022), Bagpipes (A. C. Carnall et al. 2019), MSAEXP (G. Brammer 2023) NumPy (C. R. Harris et al. 2020), pandas (The pandas development team 2024) Photutils (L. Bradley et al. 2016), TOPCAT (M. Taylor 2022).","article_number":"86","title":"Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"We present a comprehensive analysis of the MIRI Extremely Red Object Virgil, a Lyα emitter at zspec = 6.6379 ± 0.0035 with the photometric properties of a Little Red Dot. Leveraging new JWST/MIRI imaging from the MIDIS and PAHSPECS programs, we confirm Virgil’s extraordinary nature among galaxies in JADES/GOODS-South, exhibiting a strikingly red NIRCam-to-MIRI color (F444W–F1500W = 2.84 ± 0.04 mag). Deep NIRSpec/PRISM spectroscopy from the OASIS program offers key insights into the host galaxy, revealing properties of an average star-forming galaxy during Cosmic Reionization, such as a subsolar metallicity, low-to-moderate dust content, and a relatively high ionization parameter and electron temperature. By estimating the star formation rate of Virgil from UV and Hα, we find evidence that the galaxy is either entering or fading out of a bursty episode. Although line-ratio diagnostics employed at high z would classify Virgil as an active galactic nucleus (AGN), this classification becomes ambiguous once redshift evolution is considered. Nonetheless, Virgil occupies the same parameter space as recently confirmed AGNs at similar redshifts. The new deep MIRI data at 15 μm reinforce the AGN nature of Virgil, as inferred from multiple spectral energy distribution (SED) fitting codes. Virgil’s rising infrared SED and UV excess resemble those of Dust-Obscured Galaxies (DOGs) studied with Spitzer at Cosmic Noon, particularly blue-excess HotDOGs. Our results highlight the need for a multiwavelength approach incorporating MIRI to uncover such extreme sources at z ≳ 6 and to shed light on the interplay between galaxy evolution and early black hole growth during Cosmic Reionization.","lang":"eng"}],"DOAJ_listed":"1","file_date_updated":"2026-04-13T07:53:00Z","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae089c","scopus_import":"1","department":[{"_id":"JoMa"}],"_id":"21727"},{"article_processing_charge":"Yes","citation":{"ieee":"E. Banerjee <i>et al.</i>, “MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3,” <i>The Astrophysical Journal</i>, vol. 980, no. 2. IOP Publishing, 2025.","chicago":"Banerjee, Eshita, Sowgat Muzahid, Joop Schaye, Jérémy Blaizot, Nicolas Bouché, Sebastiano Cantalupo, Sean D. Johnson, Jorryt J Matthee, and Anne Verhamme. “MUSEQuBES: Connecting H i Absorption with Lyα Emitters at z ≈ 3.3.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ada7e9\">https://doi.org/10.3847/1538-4357/ada7e9</a>.","apa":"Banerjee, E., Muzahid, S., Schaye, J., Blaizot, J., Bouché, N., Cantalupo, S., … Verhamme, A. (2025). MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ada7e9\">https://doi.org/10.3847/1538-4357/ada7e9</a>","short":"E. Banerjee, S. Muzahid, J. Schaye, J. Blaizot, N. Bouché, S. Cantalupo, S.D. Johnson, J.J. Matthee, A. Verhamme, The Astrophysical Journal 980 (2025).","mla":"Banerjee, Eshita, et al. “MUSEQuBES: Connecting H i Absorption with Lyα Emitters at z ≈ 3.3.” <i>The Astrophysical Journal</i>, vol. 980, no. 2, 171, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ada7e9\">10.3847/1538-4357/ada7e9</a>.","ama":"Banerjee E, Muzahid S, Schaye J, et al. MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3. <i>The Astrophysical Journal</i>. 2025;980(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ada7e9\">10.3847/1538-4357/ada7e9</a>","ista":"Banerjee E, Muzahid S, Schaye J, Blaizot J, Bouché N, Cantalupo S, Johnson SD, Matthee JJ, Verhamme A. 2025. MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3. The Astrophysical Journal. 980(2), 171."},"day":"20","ddc":["520"],"publication_status":"published","volume":980,"OA_type":"gold","date_published":"2025-02-20T00:00:00Z","has_accepted_license":"1","publisher":"IOP Publishing","date_created":"2025-03-09T23:01:26Z","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"oa_version":"Published Version","article_type":"original","date_updated":"2026-02-16T12:42:00Z","OA_place":"publisher","intvolume":"       980","quality_controlled":"1","status":"public","isi":1,"file":[{"relation":"main_file","creator":"dernst","date_updated":"2025-03-10T11:54:52Z","success":1,"file_size":1194131,"content_type":"application/pdf","access_level":"open_access","date_created":"2025-03-10T11:54:52Z","checksum":"1d33a8eb59f42a0c7a943c8859e9b883","file_name":"2025_AstrophysicalJour_Banerjee.pdf","file_id":"19379"}],"oa":1,"author":[{"last_name":"Banerjee","first_name":"Eshita","full_name":"Banerjee, Eshita"},{"first_name":"Sowgat","full_name":"Muzahid, Sowgat","last_name":"Muzahid"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Blaizot","first_name":"Jérémy","full_name":"Blaizot, Jérémy"},{"first_name":"Nicolas","full_name":"Bouché, Nicolas","last_name":"Bouché"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"last_name":"Johnson","full_name":"Johnson, Sean D.","first_name":"Sean D."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"}],"external_id":{"isi":["001421001500001"]},"year":"2025","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"month":"02","type":"journal_article","acknowledgement":"We would like to thank the anonymous referee for useful comments. We thank Marijke Segers, Lorrie Straka, and Monica Turner for their early contributions to the MUSEQuBES project. We thank Raghunathan Srianand for useful suggestions. E.B. thanks Labanya Kumar Guha and Yucheng Guo for helpful discussions. S.C. gratefully acknowledges the fund support from the European Research Council (ERC).\r\n\r\nSoftware: NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), Matplotlib (J. D. Hunter 2007), and AstroPy (Astropy Collaboration et al. 2013, 2018).","article_number":"171","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3","abstract":[{"text":"We present a comprehensive analysis of H i absorption around 96 Lyα emitters (LAEs) at z ≈ 3.3 (median Lyα luminosity ≈1042 erg s−1). These LAEs were identified within eight MUSE fields, each (math. formular) on the sky and centered on a bright background quasar, as part of the MUSEQuBES survey. Using Voigt profile fitting for all H i absorbers detected within ±​​​​​​500 km s−1 of these LAEs, we compiled a catalog of 800 H i absorption components. Our analysis shows that H i absorption is enhanced near the LAEs compared to the intergalactic medium. However, no trend is found between the column densities of H i absorbers and their impact parameters from the LAEs (spanning ​​​​​​≈54–260 pkpc). Additionally, all galaxies associated with Lyman-limit systems have impact parameters >50 pkpc from the quasar sightlines, suggesting that true absorber hosts may be too faint to detect. The LAEs show an overall H i covering fraction (fc(H i)) of ≈88% for a threshold (math. formular) (H i) = 15. Notably, at the same threshold, the LAEs in pairs/groups exhibit a 100% H i covering fraction out to ≈250 pkpc. In contrast, isolated LAEs consistently show a lower fc(H i) of ≈80%. This environmental influence on fc(H i) is also evident up to ≈300 km s−1 in differential bins of line-of-sight velocity. We find an anticorrelation between fc(H i) and the equivalent width of rest-frame Lyα emission (EW0). Based on the Lyα shell model, this could imply that gas-rich galaxies tend to reside in gas-rich environments or that the LAEs with higher EW0 are more efficient at ionizing their surrounding medium.","lang":"eng"}],"DOAJ_listed":"1","file_date_updated":"2025-03-10T11:54:52Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"doi":"10.3847/1538-4357/ada7e9","issue":"2","scopus_import":"1","department":[{"_id":"JoMa"}],"_id":"19365"},{"article_number":"11","acknowledgement":"We thank the PRIMER team 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 program #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. 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 (DNRF140). 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 was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. Support for this work for R.P.N. 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. T.B.M. was supported by a CIERA fellowship.\r\nAll software packages used in this work are publicly available on Github: grizli, msafit, msaexp, Prospector, and sedpy. We acknowledge: astropy (Astropy Collaboration et al. 2013, 2018, 2022), matplotlib (J. D. Hunter 2007), numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), lmfit (M. Newville et al. 2024), eMPT (N. Bonaventura et al. 2023), the jwst pipeline (H. Bushouse et al. 2024), msaexp (G. Brammer 2024a), and grizli (G. Brammer 2024b),.","abstract":[{"lang":"eng","text":"We report the spectroscopic discovery of a massive quiescent galaxy at zspec = 7.29 ± 0.01, just ∼700 Myr after the big bang. RUBIES-UDS-QG-z7 was selected from public JWST/NIRCam and MIRI imaging from the PRIMER survey and observed with JWST/NIRSpec as part of RUBIES. The NIRSpec/PRISM spectrum reveals one of the strongest Balmer breaks observed thus far at z > 6, with no emission lines but tentative Balmer and Ca absorption features, as well as a Lyman break. Simultaneous modeling of the NIRSpec/PRISM spectrum and NIRCam and MIRI photometry (spanning 0.9–18 μm) shows that the galaxy formed a stellar mass of\r\n(math. formular) before z ∼ 8 and ceased forming stars 50–100 Myr prior to the time of observation, resulting in log (sSFR/Gyr- 1) < -1 . We measure a small physical size of (math formular) , which implies a high stellarmass surface density within the effective radius of (math formular) comparable to the highest densities measured in quiescent galaxies at z ∼ 2–5. The 3D stellar-mass density profile of RUBIES-UDS-QG-z7 is remarkably similar to the central densities of local massive ellipticals, suggesting that at least some of their cores may have already been in place at z > 7. The discovery of RUBIES-UDS-QG-z7 has strong implications for galaxy formation models: the estimated number density of quiescent galaxies at z ∼ 7 is >100 × larger than predicted from any model to date, indicating that quiescent galaxies have formed earlier than previously expected. "}],"DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"RUBIES reveals a massive quiescent galaxy at z = 7.3","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"isi":["001457334900001"],"arxiv":["2409.03829"]},"year":"2025","month":"04","type":"journal_article","_id":"19596","department":[{"_id":"JoMa"}],"file_date_updated":"2025-04-22T09:08:17Z","scopus_import":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/adab7a","issue":"1","has_accepted_license":"1","volume":983,"OA_type":"gold","citation":{"mla":"Weibel, Andrea, et al. “RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3.” <i>The Astrophysical Journal</i>, vol. 983, no. 1, 11, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/adab7a\">10.3847/1538-4357/adab7a</a>.","ista":"Weibel A, De Graaff A, Setton DJ, Miller TB, Oesch PA, Brammer G, Lagos CDP, Whitaker KE, Williams CC, Baggen JFW, Bezanson R, Boogaard LA, Cleri NJ, Greene JE, Hirschmann M, Hviding RE, Kuruvanthodi A, Labbé I, Leja J, Maseda MV, Matthee JJ, Mcconachie I, Naidu RP, Roberts-Borsani G, Schaerer D, Suess KA, Valentino F, Van Dokkum P, Wang B. 2025. RUBIES reveals a massive quiescent galaxy at z = 7.3. The Astrophysical Journal. 983(1), 11.","ama":"Weibel A, De Graaff A, Setton DJ, et al. RUBIES reveals a massive quiescent galaxy at z = 7.3. <i>The Astrophysical Journal</i>. 2025;983(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/adab7a\">10.3847/1538-4357/adab7a</a>","short":"A. Weibel, A. De Graaff, D.J. Setton, T.B. Miller, P.A. Oesch, G. Brammer, C.D.P. Lagos, K.E. Whitaker, C.C. Williams, J.F.W. Baggen, R. Bezanson, L.A. Boogaard, N.J. Cleri, J.E. Greene, M. Hirschmann, R.E. Hviding, A. Kuruvanthodi, I. Labbé, J. Leja, M.V. Maseda, J.J. Matthee, I. Mcconachie, R.P. Naidu, G. Roberts-Borsani, D. Schaerer, K.A. Suess, F. Valentino, P. Van Dokkum, B. Wang, The Astrophysical Journal 983 (2025).","chicago":"Weibel, Andrea, Anna De Graaff, David J. Setton, Tim B. Miller, Pascal A. Oesch, Gabriel Brammer, Claudia D.P. Lagos, et al. “RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/adab7a\">https://doi.org/10.3847/1538-4357/adab7a</a>.","ieee":"A. Weibel <i>et al.</i>, “RUBIES reveals a massive quiescent galaxy at z = 7.3,” <i>The Astrophysical Journal</i>, vol. 983, no. 1. IOP Publishing, 2025.","apa":"Weibel, A., De Graaff, A., Setton, D. J., Miller, T. B., Oesch, P. A., Brammer, G., … Wang, B. (2025). RUBIES reveals a massive quiescent galaxy at z = 7.3. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/adab7a\">https://doi.org/10.3847/1538-4357/adab7a</a>"},"article_processing_charge":"Yes","day":"10","ddc":["520"],"publication_status":"published","date_published":"2025-04-10T00:00:00Z","quality_controlled":"1","intvolume":"       983","date_updated":"2026-02-16T12:42:28Z","OA_place":"publisher","isi":1,"file":[{"success":1,"date_updated":"2025-04-22T09:08:17Z","relation":"main_file","creator":"dernst","content_type":"application/pdf","file_size":1964589,"date_created":"2025-04-22T09:08:17Z","access_level":"open_access","file_id":"19605","checksum":"a1132e0b18bb643f9a32674c6694375a","file_name":"2025_AstrophysicalJour_Weibel.pdf"}],"author":[{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"first_name":"Anna","full_name":"De Graaff, Anna","last_name":"De Graaff"},{"full_name":"Setton, David J.","first_name":"David J.","last_name":"Setton"},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"last_name":"Lagos","first_name":"Claudia D.P.","full_name":"Lagos, Claudia D.P."},{"first_name":"Katherine E.","full_name":"Whitaker, Katherine E.","last_name":"Whitaker"},{"last_name":"Williams","full_name":"Williams, Christina C.","first_name":"Christina C."},{"full_name":"Baggen, Josephine F.W.","first_name":"Josephine F.W.","last_name":"Baggen"},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"last_name":"Kuruvanthodi","full_name":"Kuruvanthodi, Adarsh","first_name":"Adarsh"},{"last_name":"Labbé","full_name":"Labbé, Ivo","first_name":"Ivo"},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Mcconachie","first_name":"Ian","full_name":"Mcconachie, Ian"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Guido","full_name":"Roberts-Borsani, Guido","last_name":"Roberts-Borsani"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"first_name":"Katherine A.","full_name":"Suess, Katherine A.","last_name":"Suess"},{"first_name":"Francesco","full_name":"Valentino, Francesco","last_name":"Valentino"},{"last_name":"Van Dokkum","first_name":"Pieter","full_name":"Van Dokkum, Pieter"},{"first_name":"Bingjie","full_name":"Wang, Bingjie","last_name":"Wang"}],"oa":1,"status":"public","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"publisher":"IOP Publishing","date_created":"2025-04-20T22:01:28Z","article_type":"original","oa_version":"Published Version","arxiv":1},{"intvolume":"       984","quality_controlled":"1","date_updated":"2026-02-16T12:42:56Z","OA_place":"publisher","isi":1,"file":[{"file_id":"19708","file_name":"2025_AstrophysicalJour_Tiede.pdf","checksum":"0d4c57ee944599c0789f3db467c5ca2f","date_created":"2025-05-19T07:20:30Z","access_level":"open_access","content_type":"application/pdf","file_size":1058601,"date_updated":"2025-05-19T07:20:30Z","success":1,"relation":"main_file","creator":"dernst"}],"author":[{"first_name":"Christopher","full_name":"Tiede, Christopher","last_name":"Tiede"},{"full_name":"Zrake, Jonathan","first_name":"Jonathan","last_name":"Zrake"},{"full_name":"Macfadyen, Andrew","first_name":"Andrew","last_name":"Macfadyen"},{"orcid":"0000-0003-3633-5403","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"oa":1,"status":"public","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"date_created":"2025-05-18T22:02:49Z","publisher":"IOP Publishing","article_type":"original","oa_version":"Published Version","arxiv":1,"has_accepted_license":"1","volume":984,"OA_type":"gold","article_processing_charge":"Yes","citation":{"chicago":"Tiede, Christopher, Jonathan Zrake, Andrew Macfadyen, and Zoltán Haiman. “Suppressed Accretion onto Massive Black Hole Binaries Surrounded by Thin Disks.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/adc727\">https://doi.org/10.3847/1538-4357/adc727</a>.","apa":"Tiede, C., Zrake, J., Macfadyen, A., &#38; Haiman, Z. (2025). Suppressed accretion onto massive black hole binaries surrounded by thin disks. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/adc727\">https://doi.org/10.3847/1538-4357/adc727</a>","ieee":"C. Tiede, J. Zrake, A. Macfadyen, and Z. Haiman, “Suppressed accretion onto massive black hole binaries surrounded by thin disks,” <i>The Astrophysical Journal</i>, vol. 984, no. 2. IOP Publishing, 2025.","ista":"Tiede C, Zrake J, Macfadyen A, Haiman Z. 2025. Suppressed accretion onto massive black hole binaries surrounded by thin disks. The Astrophysical Journal. 984(2), 144.","ama":"Tiede C, Zrake J, Macfadyen A, Haiman Z. Suppressed accretion onto massive black hole binaries surrounded by thin disks. <i>The Astrophysical Journal</i>. 2025;984(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/adc727\">10.3847/1538-4357/adc727</a>","mla":"Tiede, Christopher, et al. “Suppressed Accretion onto Massive Black Hole Binaries Surrounded by Thin Disks.” <i>The Astrophysical Journal</i>, vol. 984, no. 2, 144, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/adc727\">10.3847/1538-4357/adc727</a>.","short":"C. Tiede, J. Zrake, A. Macfadyen, Z. Haiman, The Astrophysical Journal 984 (2025)."},"publication_status":"published","day":"09","ddc":["520"],"date_published":"2025-05-09T00:00:00Z","_id":"19699","department":[{"_id":"ZoHa"}],"file_date_updated":"2025-05-19T07:20:30Z","scopus_import":"1","issue":"2","doi":"10.3847/1538-4357/adc727","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_number":"144","acknowledgement":"C.T. sincerely thanks Daniel J. D'Orazio for useful and illuminating discussions. This work was supported by the European Union's Horizon 2023 research and innovation program under Marie Sklodowska-Curie grant agreement No. 101148364, by Sapere Aude Starting grant No. 121587 through the Danish Independent Research Fund, by the LISA Preparatory Science Program (LPS) through NASA grant 80NSSC24K0440, and by NASA Astrophysics Theory Program (ATP) grant 80NSSC22K0822. Computation time for this work was supported through the NYU IT High Performance Computing resources as well as the Tycho supercomputer hosted at the SCIENCE HPC center at the University of Copenhagen.","DOAJ_listed":"1","abstract":[{"text":"We demonstrate that gas disks around binary systems might deliver gas to the binary components only when the circumbinary disk is relatively warm. We present new grid-based hydrodynamics simulations, performed with the binary on the grid and a locally isothermal equation of state, in which the binary is seen to functionally \"stop accreting\" if the orbital Mach number in the disk exceeds a threshold value of about 40. Above this threshold, the disk continues to extract angular momentum from the binary orbit, but it delivers very little mass to the black holes and instead piles up mass in a ring surrounding the binary. This ring will eventually become viscously relaxed and deliver mass to the binary at the large-scale inflow rate. However, we show that the timescale for such relaxation can far exceed the implied binary lifetime. We demonstrate that the ability of a binary–disk system to equilibrate is dependent on the efficiency at which accretion streams deposit mass onto the binary, which, in turn is highly sensitive to the thermodynamic conditions of the inner disk. If disks around massive black hole binaries do operate in such nonaccreting regimes, it suggests these systems may be dimmer than their single black hole counterparts but could exhibit dramatic rebrightening after the black holes inspiral and merge. This dimming begins in the UV/optical and could completely choke high-energy emission, such that these systems would likely be intrinsically X-ray weak with reddened continua, potentially resembling the spectra of \"little red dots\" recently identified in JWST observations.","lang":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Suppressed accretion onto massive black hole binaries surrounded by thin disks","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2410.03830"],"isi":["001483889000001"]},"year":"2025","month":"05","type":"journal_article"},{"file_date_updated":"2025-05-19T07:08:39Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"issue":"2","doi":"10.3847/1538-4357/adc1ca","scopus_import":"1","department":[{"_id":"JoMa"}],"_id":"19700","year":"2025","external_id":{"arxiv":["2403.02304"],"isi":["001481589300001"]},"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","month":"05","acknowledgement":"B.W. and J.L. acknowledge support from JWST-GO-04233.009-A. R.L.D. is supported by the Australian Research Council through the Discovery Early Career Researcher Award (DECRA) Fellowship DE240100136 funded by the Australian Government. T.B.M. was supported by a CIERA postdoctoral fellowship. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant #140. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #562 (First Light at Cosmic Dawn: Exploiting the James Webb Space Telescope Revolution). 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 here can be accessed via DOI:10.17909/c3t4-9p39. Computations for this research were performed on the Pennsylvania State University's Institute for Computational and Data Sciences' Roar supercomputer. This publication made use of the NASA Astrophysical Data System for bibliographic information.","article_number":"121","title":"RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"lang":"eng","text":"The JWST discovery of \"little red dots\" (LRDs) is reshaping our picture of the early Universe, yet the physical mechanisms driving their compact size and UV-optical colors remain elusive. Here, we report an unusually bright LRD (zspec = 3.1) observed as part of the RUBIES program. This LRD exhibits broad emission lines (FWHM ∼ 4000 km s−1), a blue UV continuum, a clear Balmer break, and a red continuum sampled out to rest-frame 4 μm with MIRI. We develop a new joint galaxy and active galactic nucleus (AGN) model within the Prospector Bayesian inference framework and perform spectrophotometric modeling using NIRCam, MIRI, and NIRSpec/Prism observations. Our fiducial model reveals a M* ∼ 109 M⊙ galaxy alongside a dust-reddened AGN driving the optical emission. Explaining the rest-frame optical color as a reddened AGN requires AV ≳ 3, suggesting that a great majority of the accretion disk energy is reradiated as dust emission. Yet, despite clear AGN signatures, we find a surprising lack of hot torus emission, which implies that either the dust emission in this object must be cold, or the red continuum must instead be driven by a massive, evolved stellar population of the host galaxy—seemingly inconsistent with the high-EW broad lines (Hα rest-frame EW ∼ 800 Å). The widths and luminosities of Pa-β, Pa-δ, Pa-γ, and Hα imply a modest black hole mass of MBH ∼ 108 M⊙. Additionally, we identify a narrow blueshifted He i λ 1.083 μm absorption feature in NIRSpec/G395M spectra, signaling an ionized outflow with kinetic energy up to ∼1% the luminosity of the AGN. The low redshift of RUBIES-BLAGN-1, combined with the depth and richness of the JWST imaging and spectroscopic observations, provides a unique opportunity to build a physical model for these so-far mysterious LRDs, which may prove to be a crucial phase in the early formation of massive galaxies and their supermassive black holes."}],"DOAJ_listed":"1","date_created":"2025-05-18T22:02:49Z","publisher":"IOP Publishing","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","arxiv":1,"oa_version":"Published Version","article_type":"original","OA_place":"publisher","date_updated":"2026-02-16T12:42:43Z","intvolume":"       984","quality_controlled":"1","status":"public","oa":1,"author":[{"last_name":"Wang","first_name":"Bingjie","full_name":"Wang, Bingjie"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"last_name":"Davies","full_name":"Davies, Rebecca L.","first_name":"Rebecca L."},{"last_name":"Greene","first_name":"Jenny E.","full_name":"Greene, Jenny E."},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"first_name":"Gabriel B.","full_name":"Brammer, Gabriel B.","last_name":"Brammer"},{"full_name":"Goulding, Andy D.","first_name":"Andy D.","last_name":"Goulding"},{"first_name":"Tim B.","full_name":"Miller, Tim B.","last_name":"Miller"},{"first_name":"Katherine A.","full_name":"Suess, Katherine A.","last_name":"Suess"},{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"last_name":"Boogaard","first_name":"Leindert A.","full_name":"Boogaard, Leindert A."},{"last_name":"Cleri","first_name":"Nikko J.","full_name":"Cleri, Nikko J."},{"first_name":"Michaela","full_name":"Hirschmann, Michaela","last_name":"Hirschmann"},{"first_name":"Harley","full_name":"Katz, Harley","last_name":"Katz"},{"last_name":"Labbé","full_name":"Labbé, Ivo","first_name":"Ivo"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"full_name":"Rix, Hans Walter","first_name":"Hans Walter","last_name":"Rix"},{"first_name":"David J.","full_name":"Setton, David J.","last_name":"Setton"},{"first_name":"Katherine E.","full_name":"Whitaker, Katherine E.","last_name":"Whitaker"}],"file":[{"access_level":"open_access","date_created":"2025-05-19T07:08:39Z","checksum":"1a9ff4516d11808bc6947744473c9fc2","file_name":"2025_AstrophysicalJour_Wang.pdf","file_id":"19707","relation":"main_file","creator":"dernst","success":1,"date_updated":"2025-05-19T07:08:39Z","content_type":"application/pdf","file_size":3522072}],"isi":1,"day":"09","publication_status":"published","ddc":["520"],"citation":{"ista":"Wang B, De Graaff A, Davies RL, Greene JE, Leja J, Brammer GB, Goulding AD, Miller TB, Suess KA, Weibel A, Williams CC, Bezanson R, Boogaard LA, Cleri NJ, Hirschmann M, Katz H, Labbé I, Maseda MV, Matthee JJ, Mcconachie I, Naidu RP, Oesch PA, Rix HW, Setton DJ, Whitaker KE. 2025. RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. The Astrophysical Journal. 984(2), 121.","ama":"Wang B, De Graaff A, Davies RL, et al. RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. <i>The Astrophysical Journal</i>. 2025;984(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/adc1ca\">10.3847/1538-4357/adc1ca</a>","mla":"Wang, Bingjie, et al. “RUBIES: JWST/NIRSpec Confirmation of an Infrared-Luminous, Broad-Line Little Red Dot with an Ionized Outflow.” <i>The Astrophysical Journal</i>, vol. 984, no. 2, 121, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/adc1ca\">10.3847/1538-4357/adc1ca</a>.","short":"B. Wang, A. De Graaff, R.L. Davies, J.E. Greene, J. Leja, G.B. Brammer, A.D. Goulding, T.B. Miller, K.A. Suess, A. Weibel, C.C. Williams, R. Bezanson, L.A. Boogaard, N.J. Cleri, M. Hirschmann, H. Katz, I. Labbé, M.V. Maseda, J.J. Matthee, I. Mcconachie, R.P. Naidu, P.A. Oesch, H.W. Rix, D.J. Setton, K.E. Whitaker, The Astrophysical Journal 984 (2025).","ieee":"B. Wang <i>et al.</i>, “RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow,” <i>The Astrophysical Journal</i>, vol. 984, no. 2. IOP Publishing, 2025.","chicago":"Wang, Bingjie, Anna De Graaff, Rebecca L. Davies, Jenny E. Greene, Joel Leja, Gabriel B. Brammer, Andy D. Goulding, et al. “RUBIES: JWST/NIRSpec Confirmation of an Infrared-Luminous, Broad-Line Little Red Dot with an Ionized Outflow.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/adc1ca\">https://doi.org/10.3847/1538-4357/adc1ca</a>.","apa":"Wang, B., De Graaff, A., Davies, R. L., Greene, J. E., Leja, J., Brammer, G. B., … Whitaker, K. E. (2025). RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/adc1ca\">https://doi.org/10.3847/1538-4357/adc1ca</a>"},"article_processing_charge":"Yes","OA_type":"gold","volume":984,"date_published":"2025-05-09T00:00:00Z","has_accepted_license":"1"},{"isi":1,"file":[{"content_type":"application/pdf","file_size":5474992,"success":1,"date_updated":"2025-09-02T06:40:23Z","relation":"main_file","creator":"dernst","file_id":"20268","file_name":"2025_AstrophysicalJour_Iani.pdf","checksum":"92196e8352dddb1f305c253da1996ab6","date_created":"2025-09-02T06:40:23Z","access_level":"open_access"}],"oa":1,"author":[{"full_name":"Iani, Edoardo","first_name":"Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","orcid":"0000-0001-8386-3546","last_name":"Iani"},{"last_name":"Rinaldi","first_name":"Pierluigi","full_name":"Rinaldi, Pierluigi"},{"first_name":"Karina I.","full_name":"Caputi, Karina I.","last_name":"Caputi"},{"last_name":"Annunziatella","first_name":"Marianna","full_name":"Annunziatella, Marianna"},{"first_name":"Danial","full_name":"Langeroodi, Danial","last_name":"Langeroodi"},{"first_name":"Jens","full_name":"Melinder, Jens","last_name":"Melinder"},{"last_name":"Pérez-González","first_name":"Pablo G.","full_name":"Pérez-González, Pablo G."},{"last_name":"Álvarez-Márquez","first_name":"Javier","full_name":"Álvarez-Márquez, Javier"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I.","last_name":"Bosman"},{"last_name":"Costantin","full_name":"Costantin, Luca","first_name":"Luca"},{"last_name":"Moutard","full_name":"Moutard, Thibaud","first_name":"Thibaud"},{"last_name":"Colina","first_name":"Luis","full_name":"Colina, Luis"},{"last_name":"Östlin","first_name":"Göran","full_name":"Östlin, Göran"},{"first_name":"Thomas R.","full_name":"Greve, Thomas R.","last_name":"Greve"},{"last_name":"Wright","full_name":"Wright, Gillian","first_name":"Gillian"},{"first_name":"Almudena","full_name":"Alonso-Herrero, Almudena","last_name":"Alonso-Herrero"},{"last_name":"Bik","full_name":"Bik, Arjan","first_name":"Arjan"},{"first_name":"Steven","full_name":"Gillman, Steven","last_name":"Gillman"},{"first_name":"Alejandro","full_name":"Crespo Gómez, Alejandro","last_name":"Crespo Gómez"},{"last_name":"Hjorth","first_name":"Jens","full_name":"Hjorth, Jens"},{"first_name":"Sarah","full_name":"Kendrew, Sarah","last_name":"Kendrew"},{"full_name":"Labiano, Alvaro","first_name":"Alvaro","last_name":"Labiano"},{"first_name":"John P.","full_name":"Pye, John P.","last_name":"Pye"},{"full_name":"Tikkanen, Tuomo V.","first_name":"Tuomo V.","last_name":"Tikkanen"},{"last_name":"Walter","full_name":"Walter, Fabian","first_name":"Fabian"},{"first_name":"Manuel","full_name":"Güdel, Manuel","last_name":"Güdel"},{"last_name":"Henning","first_name":"Thomas","full_name":"Henning, Thomas"},{"last_name":"Van Der Werf","full_name":"Van Der Werf, Paul P.","first_name":"Paul P."}],"status":"public","intvolume":"       989","quality_controlled":"1","date_updated":"2026-02-16T12:43:12Z","OA_place":"publisher","PlanS_conform":"1","article_type":"original","oa_version":"Published Version","arxiv":1,"publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"publisher":"IOP Publishing","date_created":"2025-08-24T22:01:29Z","has_accepted_license":"1","date_published":"2025-08-20T00:00:00Z","volume":989,"OA_type":"gold","citation":{"chicago":"Iani, Edoardo, Pierluigi Rinaldi, Karina I. Caputi, Marianna Annunziatella, Danial Langeroodi, Jens Melinder, Pablo G. Pérez-González, et al. “MIDIS: MIRI Uncovers Virgil, the First Little Red Dot with Clear Detection of Its Host Galaxy at z ≃ 6.6.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">https://doi.org/10.3847/1538-4357/ade5a6</a>.","apa":"Iani, E., Rinaldi, P., Caputi, K. I., Annunziatella, M., Langeroodi, D., Melinder, J., … Van Der Werf, P. P. (2025). MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">https://doi.org/10.3847/1538-4357/ade5a6</a>","ieee":"E. Iani <i>et al.</i>, “MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6,” <i>The Astrophysical Journal</i>, vol. 989, no. 2. IOP Publishing, 2025.","ama":"Iani E, Rinaldi P, Caputi KI, et al. MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. <i>The Astrophysical Journal</i>. 2025;989(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">10.3847/1538-4357/ade5a6</a>","ista":"Iani E, Rinaldi P, Caputi KI, Annunziatella M, Langeroodi D, Melinder J, Pérez-González PG, Álvarez-Márquez J, Boogaard LA, Bosman SEI, Costantin L, Moutard T, Colina L, Östlin G, Greve TR, Wright G, Alonso-Herrero A, Bik A, Gillman S, Crespo Gómez A, Hjorth J, Kendrew S, Labiano A, Pye JP, Tikkanen TV, Walter F, Güdel M, Henning T, Van Der Werf PP. 2025. MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6. The Astrophysical Journal. 989(2), 160.","mla":"Iani, Edoardo, et al. “MIDIS: MIRI Uncovers Virgil, the First Little Red Dot with Clear Detection of Its Host Galaxy at z ≃ 6.6.” <i>The Astrophysical Journal</i>, vol. 989, no. 2, 160, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade5a6\">10.3847/1538-4357/ade5a6</a>.","short":"E. Iani, P. Rinaldi, K.I. Caputi, M. Annunziatella, D. Langeroodi, J. Melinder, P.G. Pérez-González, J. Álvarez-Márquez, L.A. Boogaard, S.E.I. Bosman, L. Costantin, T. Moutard, L. Colina, G. Östlin, T.R. Greve, G. Wright, A. Alonso-Herrero, A. Bik, S. Gillman, A. Crespo Gómez, J. Hjorth, S. Kendrew, A. Labiano, J.P. Pye, T.V. Tikkanen, F. Walter, M. Güdel, T. Henning, P.P. Van Der Werf, The Astrophysical Journal 989 (2025)."},"article_processing_charge":"Yes","publication_status":"published","ddc":["520"],"day":"20","_id":"20217","department":[{"_id":"JoMa"}],"scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"doi":"10.3847/1538-4357/ade5a6","issue":"2","file_date_updated":"2025-09-02T06:40:23Z","abstract":[{"lang":"eng","text":"We present Virgil, a Mid-Infrared Instrument (MIRI) extremely red object detected with the F1000W filter as part of the MIRI Deep Imaging Survey observations of the Hubble Ultra Deep Field. Virgil is an Lyα emitter (LAE) at zspec = 6.6312 ± 0.0019 (from the Very Large Telescope/MUSE) with a rest-frame UV-to-optical spectral energy distribution (SED) typical of LAEs at similar redshifts. However, MIRI observations reveal an unexpected extremely red color at rest-frame near-infrared (NIR) wavelengths, F444W − F1000W = 2.33 ± 0.06. Such a steep\r\nrise in the NIR, completely missed without MIRI imaging, is poorly reproduced by models including only stellar populations and hints toward the presence of an active galactic nucleus, although alternative explanations such as extreme dust obscuration and strong nebular continuum and emission lines contribution due to young stellar ages cannot be completely ruled out. According to the shape of its overall SED, Virgil belongs to the recently discovered\r\npopulation of little red dots but displays an extended rest-frame UV-optical wavelength morphology following a 2DSérsic profile with an average index of n = 0.93+0.85_0.31 and re = 0.49+0.05_0.11  pkpc. Only at MIRI wavelengths, Virgil is unresolved due to the coarser point-spread function. This discovery demonstrates the crucial importance of deep MIRI surveys to reveal the true nature and properties of high-z galaxies that otherwise would be misinterpreted and raises the question of how common Virgil-like objects could be in the early Universe."}],"DOAJ_listed":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"MIDIS: MIRI uncovers Virgil, the first Little Red Dot with clear detection of its host galaxy at z ≃ 6.6","article_number":"160","acknowledgement":"The authors thank R. Cooper, G. Yang, V. Kokorev, D. Wen, C. Williams, and H. Übler for useful discussions and comments.\r\nE.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. A.A.-H. acknowledges support from grant PID2021-124665NB-I00 funded by MCIN/AEI/10.13039/ 501100011033 and by “ERDF A way of making Europe.” P.G.P.-G. acknowledges support from grant PID2022-139567NB-I00 funded by the Spanish Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. J.A.-M., A.C.-G., and L.C. 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.” L.C. thanks the support from the Cosmic Dawn Center received during visits to DAWN as an international associate. L.C. acknowledges support by grants PIB2021-127718NB-100 and PID2022-139567NB-I00 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.” T.R.G. acknowledges support from the Carlsberg Foundation (grant No. CF20-0534). S.G. acknowledges financial support from the Cosmic Dawn Center (DAWN), funded by the Danish National Research Foundation (DNRF) under grant No. 140. This work was supported by research grants (VIL16599, VIL54489) from VILLUM FONDEN. J.P.P. and T.V.T. acknowledge financial support from the UK Science and Technology Facilities Council and the UK Space Agency.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the MAST at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GO #1963, GO #1895, and GTO #1283. The authors acknowledge the team led by co-PIs: C. Williams, M. Maseda, and S. Tacchella, and PI P. Oesch, for developing their respective observing programs with a zero-exclusive-access period. Also based on observations made with the NASA/ESA HST obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work presented here is the effort of the entire MIRI team, and the enthusiasm within the MIRI partnership is a significant factor in its success. MIRI draws on the scientific and technical expertise of the following organizations: Ames Research Center, USA; Airbus Defence and Space, UK; CEA-Irfu, Saclay, France; Centre Spatial de Liège, Belgium; Consejo Superior de Investigaciones Científicas, 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 für 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; Toegepast-Natuurwetenschappelijk Onderzoek (TNO-TPD), 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; University of Stockholm, Sweden; Utah State University, USA.\r\nFor the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) licence to the Author Accepted Manuscript version arising from this submission.","month":"08","type":"journal_article","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2406.18207"],"isi":["001548132000001"]},"year":"2025"},{"department":[{"_id":"IlCa"}],"_id":"20586","doi":"10.3847/1538-4357/adfecb","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"issue":"2","scopus_import":"1","file_date_updated":"2025-11-04T12:33:51Z","title":"Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"We present the discovery of deep, irregular, periodic transits toward the white dwarf ZTF J1944+4557 using follow-up time-series photometry and spectroscopy from Palomar, Keck, McDonald, Perkins, and Lowell observatories. We find a predominant period of 4.9704 hr, consistent with an orbit near the Roche limit of the white dwarf, with individual dips over 30% deep and lasting between 15 and 40 minutes. Similar to the first known white dwarf with transiting debris, WD 1145+017, the transit events are well-defined with prominent out-of-transit phases where the white dwarf appears unobscured. Spectroscopy concurrent with transit photometry reveals that the average Ca K equivalent width remains constant in and out of transit. The broadening observed in several absorption features cannot be reproduced by synthetic photospheric models, suggesting the presence of circumstellar gas. Simultaneous g + r- and g + i-band light curves from the CHIMERA instrument reveal no color dependence to the transit depths, requiring transiting dust grains to have sizes s ≳  0.2 μm. The transit morphologies appear to be constantly changing at a rate faster than the orbital period. Overall transit activity varies in the system, with transit features completely disappearing during the seven months between our 2023 and 2024 observing seasons and then reappearing in 2025 March, still repeating at 4.9704 hr. Our observations of the complete cessation and resumption of transit activity provide a novel laboratory for constraining the evolution of disrupted debris and processes like disk exhaustion and replenishment timescales at white dwarfs.","lang":"eng"}],"DOAJ_listed":"1","acknowledgement":"We first extend our gratitude to our anonymous referee, whose careful review and recommendations enhanced this manuscript. In fruitful conversations and correspondence with Tim Cunningham, Jay Farihi, Jim Fuller, Philip Muirhead, Saul Rappaport, Siyi Xu (许偲艺), and Nadia Zakamska, we found guidance that improved our interpretation of these results. We are deeply grateful for the observing support by John Kuehne at McDonald Observatory and Colt Pauley at the Perkins Telescope Observatory. This material is based upon work supported by the National Aeronautics and Space Administration under grant No. 80NSSC23K1068 issued through the Science Mission Directorate. J.A.G. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 2234657.\r\n\r\nThis worked is based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grants No. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University, Cornell University, Northwestern University and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\r\n\r\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.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.\r\n\r\nThis publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.\r\n\r\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.\r\n\r\nThis research relied upon the SIMBAD and VizieR databases operated by CDS (Strasbourg, France) and the bibliographic resources of The SAO Astrophysics Data System.\r\n\r\nFacilities: PO:1.2m - Palomar Observatory's 1.2 meter Samuel Oschin Telescope (Zwicky Transient Facility) - , Hale (CHIMERA, DBSP), Struve - McDonald Observatory's 2.1m Otto Struve Telescope(ProEM), Perkins - Lowell Observatory's 72in Perkins Telescope (PRISM), LDT - (LMI), Keck:I - KECK I Telescope (LRIS), Gaia - , PS1 - Panoramic Survey Telescope and Rapid Response System Telescope #1 (Pan-STARRS), Spitzer (IRAC) - , WISE - Wide-field Infrared Survey Explorer.\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), astroquery (A. Ginsburg et al. 2019), ccdproc (M. Craig et al. 2017), cuvarbase (J. Hoffman 2022), extinction (K. Barbary 2016), hipercam (V. S. Dhillon et al. 2021), lmfit (M. Newville et al. 2014), matplotlib (J. D. Hunter 2007), numpy (C. R. Harris et al. 2020), pandas (The pandas Development Team 2025), phot2lc (Z. Vanderbosch 2023), photutils (L. Bradley et al. 2024), Pyriod (K. Bell 2022), scipy (P. Virtanen et al. 2020).","article_number":"167","type":"journal_article","month":"10","year":"2025","external_id":{"arxiv":["2508.18348"],"isi":["001592080300001"]},"tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","oa":1,"author":[{"full_name":"Guidry, Joseph A.","first_name":"Joseph A.","last_name":"Guidry"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P."},{"first_name":"J. J.","full_name":"Hermes, J. J.","last_name":"Hermes"},{"full_name":"Veras, Dimitri","first_name":"Dimitri","last_name":"Veras"},{"first_name":"Mark A.","full_name":"Hollands, Mark A.","last_name":"Hollands"},{"last_name":"Bhattacharjee","first_name":"Soumyadeep","full_name":"Bhattacharjee, Soumyadeep"},{"last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","full_name":"Caiazzo, Ilaria"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"last_name":"Kao","full_name":"Kao, Malia L.","first_name":"Malia L."},{"first_name":"Lou Baya","full_name":"Ould Rouis, Lou Baya","last_name":"Ould Rouis"},{"first_name":"Antonio C.","full_name":"Rodriguez, Antonio C.","last_name":"Rodriguez"},{"first_name":"Jan","full_name":"Van Roestel, Jan","last_name":"Van Roestel"}],"file":[{"content_type":"application/pdf","file_size":5323398,"date_updated":"2025-11-04T12:33:51Z","success":1,"creator":"dernst","relation":"main_file","file_id":"20601","checksum":"24892d1b5bfa1867eb0a353f10c31b82","file_name":"2025_AstrophysicalJour_Guidry.pdf","date_created":"2025-11-04T12:33:51Z","access_level":"open_access"}],"isi":1,"OA_place":"publisher","date_updated":"2026-02-16T12:43:29Z","intvolume":"       992","quality_controlled":"1","arxiv":1,"oa_version":"Published Version","article_type":"original","PlanS_conform":"1","date_created":"2025-11-02T23:01:33Z","publisher":"IOP Publishing","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","has_accepted_license":"1","date_published":"2025-10-20T00:00:00Z","publication_status":"published","ddc":["520"],"day":"20","citation":{"ieee":"J. A. Guidry <i>et al.</i>, “Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing,” <i>The Astrophysical Journal</i>, vol. 992, no. 2. IOP Publishing, 2025.","apa":"Guidry, J. A., Vanderbosch, Z. P., Hermes, J. J., Veras, D., Hollands, M. A., Bhattacharjee, S., … Van Roestel, J. (2025). Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/adfecb\">https://doi.org/10.3847/1538-4357/adfecb</a>","chicago":"Guidry, Joseph A., Zachary P. Vanderbosch, J. J. Hermes, Dimitri Veras, Mark A. Hollands, Soumyadeep Bhattacharjee, Ilaria Caiazzo, et al. “Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 Hr Orbit—and Its Vanishing.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/adfecb\">https://doi.org/10.3847/1538-4357/adfecb</a>.","short":"J.A. Guidry, Z.P. Vanderbosch, J.J. Hermes, D. Veras, M.A. Hollands, S. Bhattacharjee, I. Caiazzo, K. El-Badry, M.L. Kao, L.B. Ould Rouis, A.C. Rodriguez, J. Van Roestel, The Astrophysical Journal 992 (2025).","ista":"Guidry JA, Vanderbosch ZP, Hermes JJ, Veras D, Hollands MA, Bhattacharjee S, Caiazzo I, El-Badry K, Kao ML, Ould Rouis LB, Rodriguez AC, Van Roestel J. 2025. Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. The Astrophysical Journal. 992(2), 167.","ama":"Guidry JA, Vanderbosch ZP, Hermes JJ, et al. Transiting planetary debris near the Roche limit of a white dwarf on a 4.97 hr orbit—and its vanishing. <i>The Astrophysical Journal</i>. 2025;992(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/adfecb\">10.3847/1538-4357/adfecb</a>","mla":"Guidry, Joseph A., et al. “Transiting Planetary Debris near the Roche Limit of a White Dwarf on a 4.97 Hr Orbit—and Its Vanishing.” <i>The Astrophysical Journal</i>, vol. 992, no. 2, 167, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/adfecb\">10.3847/1538-4357/adfecb</a>."},"article_processing_charge":"Yes","OA_type":"gold","volume":992},{"oa":1,"author":[{"last_name":"Setton","first_name":"David J.","full_name":"Setton, David J."},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"de Graaff","first_name":"Anna","full_name":"de Graaff, Anna"},{"last_name":"Ma","first_name":"Yilun 逸伦","full_name":"Ma, Yilun 逸伦"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Bezanson","full_name":"Bezanson, Rachel","first_name":"Rachel"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"last_name":"Katz","first_name":"Harley","full_name":"Katz, Harley"},{"full_name":"Labbe, Ivo","first_name":"Ivo","last_name":"Labbe"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"last_name":"McConachie","first_name":"Ian","full_name":"McConachie, Ian"},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"last_name":"Price","first_name":"Sedona H.","full_name":"Price, Sedona H."},{"first_name":"Katherine A.","full_name":"Suess, Katherine A.","last_name":"Suess"},{"first_name":"Pieter","full_name":"van Dokkum, Pieter","last_name":"van Dokkum"},{"first_name":"Bingjie 冰洁","full_name":"Wang 王, Bingjie 冰洁","last_name":"Wang 王"},{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"first_name":"Katherine E.","full_name":"Whitaker, Katherine E.","last_name":"Whitaker"},{"last_name":"Williams","first_name":"Christina C.","full_name":"Williams, Christina C."}],"file":[{"content_type":"application/pdf","file_size":1989640,"creator":"dernst","relation":"main_file","success":1,"date_updated":"2026-02-09T06:39:23Z","file_name":"2025_AstrophysicalJournal_Setton.pdf","checksum":"2a424eb43748a6370ff058c98adb15c6","file_id":"21163","access_level":"open_access","date_created":"2026-02-09T06:39:23Z"}],"status":"public","intvolume":"       995","quality_controlled":"1","OA_place":"publisher","date_updated":"2026-02-09T06:41:48Z","article_type":"original","PlanS_conform":"1","arxiv":1,"oa_version":"Published Version","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","publisher":"IOP Publishing","date_created":"2026-01-28T15:21:47Z","has_accepted_license":"1","date_published":"2025-12-09T00:00:00Z","OA_type":"gold","volume":995,"ddc":["520"],"day":"09","publication_status":"published","article_processing_charge":"Yes","citation":{"mla":"Setton, David J., et al. “Little Red Dots at an Inflection Point: Ubiquitous v-Shaped Turnover Consistently Occurs at the Balmer Limit.” <i>The Astrophysical Journal</i>, vol. 995, no. 1, 118, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1500\">10.3847/1538-4357/ae1500</a>.","ista":"Setton DJ, Greene JE, de Graaff A, Ma Y逸伦, Leja J, Matthee JJ, Bezanson R, Boogaard LA, Cleri NJ, Katz H, Labbe I, Maseda MV, McConachie I, Miller TB, Price SH, Suess KA, van Dokkum P, Wang 王 B冰洁, Weibel A, Whitaker KE, Williams CC. 2025. Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit. The Astrophysical Journal. 995(1), 118.","ama":"Setton DJ, Greene JE, de Graaff A, et al. Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit. <i>The Astrophysical Journal</i>. 2025;995(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1500\">10.3847/1538-4357/ae1500</a>","short":"D.J. Setton, J.E. Greene, A. de Graaff, Y.逸伦 Ma, J. Leja, J.J. Matthee, R. Bezanson, L.A. Boogaard, N.J. Cleri, H. Katz, I. Labbe, M.V. Maseda, I. McConachie, T.B. Miller, S.H. Price, K.A. Suess, P. van Dokkum, B.冰洁 Wang 王, A. Weibel, K.E. Whitaker, C.C. Williams, The Astrophysical Journal 995 (2025).","apa":"Setton, D. J., Greene, J. E., de Graaff, A., Ma, Y. 逸伦, Leja, J., Matthee, J. J., … Williams, C. C. (2025). Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae1500\">https://doi.org/10.3847/1538-4357/ae1500</a>","ieee":"D. J. Setton <i>et al.</i>, “Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit,” <i>The Astrophysical Journal</i>, vol. 995, no. 1. IOP Publishing, 2025.","chicago":"Setton, David J., Jenny E. Greene, Anna de Graaff, Yilun 逸伦 Ma, Joel Leja, Jorryt J Matthee, Rachel Bezanson, et al. “Little Red Dots at an Inflection Point: Ubiquitous v-Shaped Turnover Consistently Occurs at the Balmer Limit.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ae1500\">https://doi.org/10.3847/1538-4357/ae1500</a>."},"_id":"21057","department":[{"_id":"JoMa"}],"scopus_import":"1","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"doi":"10.3847/1538-4357/ae1500","file_date_updated":"2026-02-09T06:39:23Z","DOAJ_listed":"1","abstract":[{"lang":"eng","text":"Among the most puzzling early discoveries of JWST are “little red dots” (LRDs), compact red sources that host broad Balmer emission lines, and in many cases exhibit a “V-shaped” change in slope in the rest-optical. The physical properties of LRDs currently have order-of-magnitude uncertainties, because models to explain the continuum of these sources differ immensely. Here, we leverage the complete selection of red sources in the RUBIES program, supplemented with public PRISM spectra, to study the origin of this V shape. By fitting a broken power law with a flexible inflection point, we find that a large fraction of red Hα emitters at 2 < z < 6 exhibit a strong change in slope, and that all strong inflections appear associated with the Balmer limit (0.3645 μm). Using a simple model of a reddened active galactic nucleus (AGN) with an unobscured scattered-light component, we demonstrate that the observed V shape in LRDs is unlikely to occur at any specific wavelength if the entire continuum is dominated by light from a power-law AGN continuum. In contrast, models with an intrinsic feature at the Balmer limit, such as those that are dominated by an evolved stellar population, can produce the observed spectral shapes, provided that a reddened component picks up sufficiently redward of the break. While no model can comfortably explain the full LRD spectral energy distribution, the common inflection location suggests that a single component consistently dominates the rest-frame UV optical in LRDs, and that this component is associated with T ∼ 10^4 K hydrogen."}],"title":"Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"118","acknowledgement":"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. The specific observations analyzed can be accessed via DOI: 10.17909/0esg-h949. All of the data products presented herein were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center, which is funded by the Danish National Research Foundation under grant No. 140. We express gratitude toward the members of the GTO, GO, and DDT teams, whose public data we utilized in this work.\r\n\r\nSupport for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. Support for program No. 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. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project No. 562. D.S. acknowledges helpful conversations with Xiaohui Fan and Jared Siegel that contributed to the quality of this work, in addition to aesthetic sign-off from Stephanie Permut on the colors of figures. T.B.M. was supported by a CIERA fellowship. The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.","type":"journal_article","month":"12","tmp":{"short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"year":"2025","external_id":{"arxiv":["2411.03424"]}}]