[{"fulldoi":"https://doi.org/10.1051/0004-6361/202558205","file":[{"relation":"main_file","creator":"dernst","content_type":"application/pdf","file_id":"23101","checksum":"875d217ea15192fa1208f3db34a7fad6","file_size":587642,"date_updated":"2026-10-12T07:31:23Z","file_name":"2026_AstronomyAstrophysics_Matharu.pdf","date_created":"2026-10-12T07:31:23Z","success":1,"access_level":"open_access"}],"oa_version":"Published Version","scopus_import":"1","citation":{"mla":"Matharu, Jasleen, et al. “A First Look at a Complete View of Spatially Resolved Star Formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO Slitless Spectroscopy.” <i>Astronomy and Astrophysics</i>, vol. 708, A33, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202558205\">10.1051/0004-6361/202558205</a>.","apa":"Matharu, J., Shen, L., Shivaei, I., Oesch, P. A., Papovich, C., Brammer, G., … Xiao, M. (2026). A first look at a complete view of spatially resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202558205\">https://doi.org/10.1051/0004-6361/202558205</a>","short":"J. Matharu, L. Shen, I. Shivaei, P.A. Oesch, C. Papovich, G. Brammer, N.A. Reddy, Y. Cheng, P. Van Dokkum, S.L. Finkelstein, N.P. Hathi, J.S. Kartaltepe, A.M. Koekemoer, J.J. Matthee, N. Pirzkal, S.M. Wilkins, M.A. Wozniak, M. Xiao, Astronomy and Astrophysics 708 (2026).","ama":"Matharu J, Shen L, Shivaei I, et al. A first look at a complete view of spatially resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy. <i>Astronomy and Astrophysics</i>. 2026;708. doi:<a href=\"https://doi.org/10.1051/0004-6361/202558205\">10.1051/0004-6361/202558205</a>","chicago":"Matharu, Jasleen, Lu Shen, Irene Shivaei, Pascal A. Oesch, Casey Papovich, Gabriel Brammer, Naveen A. Reddy, et al. “A First Look at a Complete View of Spatially Resolved Star Formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO Slitless Spectroscopy.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202558205\">https://doi.org/10.1051/0004-6361/202558205</a>.","ieee":"J. Matharu <i>et al.</i>, “A first look at a complete view of spatially resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy,” <i>Astronomy and Astrophysics</i>, vol. 708. EDP Sciences, 2026.","ista":"Matharu J, Shen L, Shivaei I, Oesch PA, Papovich C, Brammer G, Reddy NA, Cheng Y, Van Dokkum P, Finkelstein SL, Hathi NP, Kartaltepe JS, Koekemoer AM, Matthee JJ, Pirzkal N, Wilkins SM, Wozniak MA, Xiao M. 2026. A first look at a complete view of spatially resolved star formation at 1  &#60;  z  &#60;  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy. Astronomy and Astrophysics. 708, A33."},"language":[{"iso":"eng"}],"volume":708,"year":"2026","publisher":"EDP Sciences","OA_place":"publisher","DOAJ_listed":"1","publication":"Astronomy and Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_number":"A33","license":"https://creativecommons.org/licenses/by/4.0/","publication_status":"published","das_tickbox":"0","title":"A first look at a complete view of spatially resolved star formation at 1  <  z  <  1.8 with JWST NGDEEP+FRESCO slitless spectroscopy","external_id":{"arxiv":["2511.15792"]},"doi":"10.1051/0004-6361/202558205","ddc":["520"],"has_accepted_license":"1","department":[{"_id":"JoMa"}],"arxiv":1,"status":"public","article_processing_charge":"No","supplementarymaterial":"no","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-10-04T22:01:55Z","_id":"23048","article_type":"original","author":[{"last_name":"Matharu","full_name":"Matharu, Jasleen","first_name":"Jasleen"},{"first_name":"Lu","last_name":"Shen","full_name":"Shen, Lu"},{"first_name":"Irene","last_name":"Shivaei","full_name":"Shivaei, Irene"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"first_name":"Casey","full_name":"Papovich, Casey","last_name":"Papovich"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Naveen A.","last_name":"Reddy","full_name":"Reddy, Naveen A."},{"full_name":"Cheng, Yingjie","last_name":"Cheng","first_name":"Yingjie"},{"full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum","first_name":"Pieter"},{"first_name":"Steven L.","last_name":"Finkelstein","full_name":"Finkelstein, Steven L."},{"first_name":"Nimish P.","last_name":"Hathi","full_name":"Hathi, Nimish P."},{"last_name":"Kartaltepe","full_name":"Kartaltepe, Jeyhan S.","first_name":"Jeyhan S."},{"first_name":"Anton M.","full_name":"Koekemoer, Anton M.","last_name":"Koekemoer"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Pirzkal, Nor","last_name":"Pirzkal","first_name":"Nor"},{"first_name":"Stephen M.","last_name":"Wilkins","full_name":"Wilkins, Stephen M."},{"first_name":"Michael A.","full_name":"Wozniak, Michael A.","last_name":"Wozniak"},{"full_name":"Xiao, Mengyuan","last_name":"Xiao","first_name":"Mengyuan"}],"type":"journal_article","acknowledgement":"JM is grateful to the Max Planck Society for the MPIA Prize Fellowship and to the Cosmic Dawn Center for the DAWN Fellowship. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The raw 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 JWST Cycle 1 GO programs #1895 and #2079. Support for both programs was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant 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. 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.","intvolume":"       708","abstract":[{"text":"The previously inaccessible star formation tracer Paschen-Alpha (Paα) can now be spatially resolved by JWST NIRCam slitless spectroscopy in distant galaxies up to cosmic noon. In the first study of its kind, we combine JWST NGDEEP NIRISS and FRESCO NIRCam slitless spectroscopy to provide the first direct comparison of spatially resolved dust-obscured (traced by Paα) versus unobscured (traced by Hα) star formation across the main sequence. We stacked Paα and Hα emission-line maps, along with stellar continuum images at both wavelengths of 31 galaxies at 1 < z < 1.8 in three bins of stellar mass spanning 7.7 ≤ log(M*/M⊙) < 11. Surface brightness profiles were measured and equivalent width (EW) profiles computed. Increasing Paα and Hα EW profiles with galactocentric radius across all stellar masses probed provides direct evidence for the inside-out growth of galaxies both via dust-obscured and unobscured star formation for the first time. For galaxies predominantly on the main sequence (log(M*/M⊙)≥8.8), a weakly positive (0.1 ± 0.1) Paα/Hα line profile gradient as a function of radius is found at 8.8 ≤ log(M*/M⊙) < 9.9, with a negative (−0.4 ± 0.1) Paα/Hα line profile gradient as a function of radius found at the highest stellar masses of 9.9 ≤ log(M*/M⊙) < 11.0. Low-mass galaxies (7.7 ≤ log(M*/M⊙) < 8.8) with predominantly high specific star formation rates relative to the main sequence are also found to have a negative (−0.5 ± 0.1) Paα/Hα line profile gradient as a function of radius. Our results demonstrate that while inside-out growth via star formation is ubiquitous across the main sequence just after cosmic noon, centrally concentrated dust attenuation is not. Along with other recent work in the literature, our findings now motivate future studies of resolved SFR and dust attenuation profiles in large samples of individual cosmic noon galaxies across the main sequence, aimed at understanding the intrinsic scatter in spatially resolved star formation.","lang":"eng"}],"file_date_updated":"2026-10-12T07:31:23Z","researchdata_availability":"yes","OA_type":"diamond","PlanS_conform":"1","month":"04","date_updated":"2026-10-12T07:44:07Z","date_published":"2026-04-01T00:00:00Z","quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"01","oa":1},{"author":[{"full_name":"Zhang, Yunchong","last_name":"Zhang","first_name":"Yunchong"},{"last_name":"De Graaff","full_name":"De Graaff, Anna","first_name":"Anna"},{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"first_name":"Sedona H.","full_name":"Price, Sedona H.","last_name":"Price"},{"last_name":"Bezanson","full_name":"Bezanson, Rachel","first_name":"Rachel"},{"first_name":"Claudia","full_name":"Del P. Lagos, Claudia","last_name":"Del P. Lagos"},{"first_name":"Sam E.","full_name":"Cutler, Sam E.","last_name":"Cutler"},{"last_name":"Mcconachie","full_name":"Mcconachie, Ian","first_name":"Ian"},{"last_name":"Cleri","full_name":"Cleri, Nikko J.","first_name":"Nikko J."},{"full_name":"Cooper, Olivia R.","last_name":"Cooper","first_name":"Olivia R."},{"first_name":"Rashmi","last_name":"Gottumukkala","full_name":"Gottumukkala, Rashmi"},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"first_name":"Michaela","full_name":"Hirschmann, Michaela","last_name":"Hirschmann"},{"last_name":"Khullar","full_name":"Khullar, Gourav","first_name":"Gourav"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"full_name":"Leja, Joel","last_name":"Leja","first_name":"Joel"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Miller","full_name":"Miller, Tim B.","first_name":"Tim B."},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"first_name":"Bingjie","full_name":"Wang, Bingjie","last_name":"Wang"},{"first_name":"Katherine E.","full_name":"Whitaker, Katherine E.","last_name":"Whitaker"},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}],"article_type":"original","issue":"2","type":"journal_article","article_processing_charge":"Yes","status":"public","_id":"23092","date_created":"2026-10-11T22:02:05Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2026-10-12T11:55:05Z","PlanS_conform":"1","month":"02","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","day":"01","oa":1,"date_published":"2026-02-01T00:00:00Z","acknowledgement":"We thank Alan Pearl for his contribution to estimating the cosmic variance contribution to the number density uncertainties in this work. We thank Hans-Walter Rix for the valuable discussion on the selection function and correcting the spectroscopic incompleteness of massive quiescent galaxies in RUBIES.\r\n\r\nSome of the data products presented herein were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140.\r\n\r\nThe Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant #140.\r\n\r\nSupport for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant.\r\n\r\nR.B. gratefully acknowledges support from the Research Corporation for Scientific Advancement (RCSA) Cottrell Scholar Award ID No: 27587.\r\n\r\nThe work 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\nT.B.M. was supported by a CIERA Postdoctoral Fellowship.\r\n\r\nThis work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program numbers 1180, 1181, 1210, 1211, 1213, 1214, 1215, 1286, 1345, 1433, 1747, 2028, 2073, 2198, 2282, 2561, 2565, 2750, 2756, 2767, 3073, 3215, 4233, 4446, 4557, 6368, 6541, and 6585. The specific observations analyzed can be accessed via DOI: 10.17909/sjsj-8p46.\r\n\r\nSupport 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.\r\n\r\nThe authors acknowledge the CEERS and PRIMER teams for developing their observing program with a zero-exclusive access period.\r\n\r\nFacility: JWST - James Webb Space Telescope.\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), Scipy (P. Virtanen et al. 2020), Photutils (L. Bradley 2023), SpectRes (A. C. Carnall 2017), Scikit-learn (F. Pedregosa et al. 2011), Prospector (B. Johnson & J. Leja 2017; J. Leja et al. 2017; B. Johnson et al. 2021).","intvolume":"       997","file_date_updated":"2026-10-12T11:51:24Z","abstract":[{"lang":"eng","text":"We present the number density of massive (log(M*/Mo)> 10.3) quiescent galaxies at 2 < z < 5 using JWST NIRSpec PRISM spectra. This work relies on spectra from RUBIES, which provides excellent data quality and an unparalleled, well-defined targeting strategy to robustly infer physical properties and number densities. We identify quiescent galaxy candidates within RUBIES through principal component analysis and construct a final sample using star formation histories derived from spectrophotometric fitting of the NIRSpec PRISM spectra and NIRCam photometry. By inverting the RUBIES selection function, we correct for survey incompleteness and calculate the number density of massive quiescent galaxies at these redshifts, providing the most complete spectroscopic estimates prior to cosmic noon to date. We find that early massive quiescent galaxies are surprisingly common (≳10−5 Mpc−3 by 4 < z < 5), which is consistent with previous studies based on JWST photometry alone and/or in smaller survey areas. We compare our number densities with predictions from six state-of-the-art cosmological galaxy formation simulations. At z > 3, most simulations fail to produce enough massive quiescent galaxies, suggesting the treatment of feedback and/or the channels for early efficient formation are incomplete in most galaxy evolution models."}],"OA_type":"gold","year":"2026","publisher":"IOP Publishing","DOAJ_listed":"1","OA_place":"publisher","oa_version":"Published Version","scopus_import":"1","citation":{"short":"Y. Zhang, A. De Graaff, D.J. Setton, S.H. Price, R. Bezanson, C. Del P. Lagos, S.E. Cutler, I. Mcconachie, N.J. Cleri, O.R. Cooper, R. Gottumukkala, J.E. Greene, M. Hirschmann, G. Khullar, I. Labbe, J. Leja, M.V. Maseda, J.J. Matthee, T.B. Miller, T. Nanayakkara, K.A. Suess, B. Wang, K.E. Whitaker, C.C. Williams, The Astrophysical Journal 997 (2026).","mla":"Zhang, Yunchong, et al. “RUBIES Spectroscopically Confirms the High Number Density of Quiescent Galaxies From2&#60;z&#60;5.” <i>The Astrophysical Journal</i>, vol. 997, no. 2, 252, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae24e1\">10.3847/1538-4357/ae24e1</a>.","apa":"Zhang, Y., De Graaff, A., Setton, D. J., Price, S. H., Bezanson, R., Del P. Lagos, C., … Williams, C. C. (2026). RUBIES spectroscopically confirms the high number density of quiescent galaxies from2&#60;z&#60;5. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae24e1\">https://doi.org/10.3847/1538-4357/ae24e1</a>","chicago":"Zhang, Yunchong, Anna De Graaff, David J. Setton, Sedona H. Price, Rachel Bezanson, Claudia Del P. Lagos, Sam E. Cutler, et al. “RUBIES Spectroscopically Confirms the High Number Density of Quiescent Galaxies From2&#60;z&#60;5.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae24e1\">https://doi.org/10.3847/1538-4357/ae24e1</a>.","ama":"Zhang Y, De Graaff A, Setton DJ, et al. RUBIES spectroscopically confirms the high number density of quiescent galaxies from2&#60;z&#60;5. <i>The Astrophysical Journal</i>. 2026;997(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae24e1\">10.3847/1538-4357/ae24e1</a>","ista":"Zhang Y, De Graaff A, Setton DJ, Price SH, Bezanson R, Del P. Lagos C, Cutler SE, Mcconachie I, Cleri NJ, Cooper OR, Gottumukkala R, Greene JE, Hirschmann M, Khullar G, Labbe I, Leja J, Maseda MV, Matthee JJ, Miller TB, Nanayakkara T, Suess KA, Wang B, Whitaker KE, Williams CC. 2026. RUBIES spectroscopically confirms the high number density of quiescent galaxies from2&#60;z&#60;5. The Astrophysical Journal. 997(2), 252.","ieee":"Y. Zhang <i>et al.</i>, “RUBIES spectroscopically confirms the high number density of quiescent galaxies from2&#60;z&#60;5,” <i>The Astrophysical Journal</i>, vol. 997, no. 2. IOP Publishing, 2026."},"fulldoi":"https://doi.org/10.3847/1538-4357/ae24e1","file":[{"checksum":"547c63f9265be5d41efdc555a25423cc","file_size":5995619,"file_name":"2026_AstrophysicalJour_Zhang.pdf","date_updated":"2026-10-12T11:51:24Z","creator":"dernst","relation":"main_file","content_type":"application/pdf","file_id":"23110","access_level":"open_access","date_created":"2026-10-12T11:51:24Z","success":1}],"volume":997,"language":[{"iso":"eng"}],"has_accepted_license":"1","doi":"10.3847/1538-4357/ae24e1","ddc":["520"],"arxiv":1,"department":[{"_id":"JoMa"}],"publication":"The Astrophysical Journal","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_number":"252","external_id":{"arxiv":["2508.08577"]},"publication_status":"published","title":"RUBIES spectroscopically confirms the high number density of quiescent galaxies from2<z<5"},{"date_published":"2026-02-24T00:00:00Z","oa":1,"day":"24","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","PlanS_conform":"1","month":"02","date_updated":"2026-10-14T07:58:57Z","OA_type":"gold","file_date_updated":"2026-10-14T07:50:51Z","abstract":[{"lang":"eng","text":"We investigate the association between galaxies and neutral O I absorption systems at z ∼ 6, which trace metalenriched gas during the epoch of reionization. We identify 40 galaxies across six quasar fields, residing in 15\r\noverdensities within 300 kpc of the background sight lines. Five O I absorption systems are associated with five of\r\nthese overdensities, yielding a covering fraction of\r\n0.27 0.10\r\n+0.13\r\nwithin 300 kpc. The absorption occurs beyond typical\r\nvirial radii, indicating that the gas traces extended overdensity environments rather than individual galaxy halos,\r\nunlike the z ∼ 0 circumgalactic medium (CGM), which is largely bound to halos. These galaxy-associated\r\nabsorbers account for ∼35% of all O I systems seen in blind quasar surveys, implying the remainder arise in\r\nlower-mass galaxies below our detection threshold or in dense neutral intergalactic medium pockets. The CGM\r\naround these galaxies contains ≳ 2 × 106 M⊙ of oxygen, comparable to the interstellar medium oxygen mass of\r\nthe galaxies themselves, suggesting that the surrounding environment holds as much metal mass as the galaxies.\r\nAll five galaxy-associated systems show significantly higher\r\nlog NCII NOI ( / )\r\nratios than absorbers lacking galaxy\r\nassociations. Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal that four of the five exhibit\r\nenrichment patterns consistent with Population III nucleosynthesis at the outskirts of galaxy overdensities. These\r\nrare systems offer a unique window into the role of first-generation stars in shaping the early metal enrichment of\r\ngalaxies and their environments."}],"intvolume":"       999","acknowledgement":"IOP Science home\r\nAccessibility Help\r\n\r\nJournals\r\nBooks\r\nPublishing Support\r\nLogin\r\nThe Astrophysical Journal\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nEIGER. VIII. First Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch of Reionization\r\nJack Higginson, Rongmon Bordoloi, Robert A. Simcoe, Jorryt Matthee, Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, Simon J. Lilly, Anna-Christina Eilers, Rohan P. NaiduShow full author list\r\n\r\nPublished 2026 February 24 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal, Volume 999, Number 1\r\nCitation Jack Higginson et al 2026 ApJ 999 49\r\nDOI 10.3847/1538-4357/ae3e81\r\n\r\nPDFOpens in a new tab.\r\nePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens in a new tab.\r\nePub\r\nArticle metrics\r\n626 Total downloads\r\n\r\n22 total citations on Dimensions.\r\nShare this article\r\nArticle information\r\nAbstract\r\nWe investigate the association between galaxies and neutral O i absorption systems at z ∼ 6, which trace metal-enriched gas during the epoch of reionization. We identify 40 galaxies across six quasar fields, residing in 15 overdensities within 300 kpc of the background sight lines. Five O i absorption systems are associated with five of these overdensities, yielding a covering fraction of \r\n within 300 kpc. The absorption occurs beyond typical virial radii, indicating that the gas traces extended overdensity environments rather than individual galaxy halos, unlike the z ∼ 0 circumgalactic medium (CGM), which is largely bound to halos. These galaxy-associated absorbers account for ∼35% of all O i systems seen in blind quasar surveys, implying the remainder arise in lower-mass galaxies below our detection threshold or in dense neutral intergalactic medium pockets. The CGM around these galaxies contains  ≳  2 × 106 M⊙ of oxygen, comparable to the interstellar medium oxygen mass of the galaxies themselves, suggesting that the surrounding environment holds as much metal mass as the galaxies. All five galaxy-associated systems show significantly higher \r\n ratios than absorbers lacking galaxy associations. Furthermore, relative abundance ratios ([Si/O], [C/O]) reveal that four of the five exhibit enrichment patterns consistent with Population III nucleosynthesis at the outskirts of galaxy overdensities. These rare systems offer a unique window into the role of first-generation stars in shaping the early metal enrichment of galaxies and their environments.\r\n\r\nExport citation and abstract\r\nBibTeX\r\nRIS\r\n\r\nPrevious article in issue\r\nNext article in issue\r\nRelated links\r\n\r\nOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nThe first generations of stars formed shortly after the Epoch of Recombination within dark matter overdensities, producing the first significant quantities of metals and enriching the intergalactic medium (IGM) while reionizing hydrogen and helium (e.g., R. S. Klessen & S. C. O. Glover 2023). These metals and gas eventually coalesced into the first galaxies, which over cosmic time evolved into Milky Way–like systems today. Studying these young galaxies and their environments provides critical insight into galaxy formation and evolution, constraining models of stellar feedback, gas accretion, and chemical enrichment (C.-A. Faucher-Giguère & S. P. Oh 2023; C. Peroux & D. Nelson 2024).\r\n\r\nAt low redshift, decades of observations using deep ground-based spectroscopy and Hubble Space Telescope (HST) data of background quasars and foreground galaxies have built a rich understanding of the circumgalactic medium (CGM) and its interplay with galaxies (e.g., J. Tumlinson et al. 2017). The CGM plays a crucial role in gas recycling, star formation regulation, and quenching; understanding its structure and composition informs galaxy growth models (Y. Peng et al. 2015; E. Zinger et al. 2020).\r\n\r\nHigh-redshift studies, leveraging ground- and space-based near-infrared (NIR) spectroscopy of quasars, reveal that the early Universe was already chemically enriched by the epoch of reionization (e.g., T. J. Cooper et al. 2019; L. Christensen et al. 2023; R. L. Davies et al. 2023a). Among tracers of neutral and low-ionization gas, O i has emerged as a key probe: surveys report an increase in O i number density at z  ≳  5–6 (G. D. Becker et al. 2019; L. Christensen et al. 2023; A. M. Sebastian et al. 2024; A. Sodini et al. 2024), while higher-ionization species like C iv and Si iv decline, consistent with a softer and evolving UV background at the end of reionization (T. J. Cooper et al. 2019; V. D’Odorico et al. 2022; R. L. Davies et al. 2023a, 2023b).\r\n\r\nHistorically, connecting absorption systems with their host galaxies was challenging due to the difficulty of obtaining deep, high-redshift galaxy spectroscopy. This has changed with the advent of JWST, providing unprecedented views of early galaxies and their impact on surrounding gas through surveys such as EIGER (D. Kashino et al. 2023) and ASPIRE (F. Wang et al. 2023). First systematic studies of cool, low-ionization CGM traced by Mg ii around z ∼ 6 galaxies suggest that high-redshift CGM differs significantly from its low-redshift counterpart: these galaxies typically have low masses, and strong stellar feedback can eject metals far beyond the halo’s gravitational potential (R. Bordoloi et al. 2024). Such pioneering studies now allow systematic investigations of the CGM in the early Universe.\r\n\r\nThe UV background during reionization was inhomogeneous and rapidly evolving (e.g., S. R. Furlanetto & S. P. Oh 2005; B. D. Oppenheimer et al. 2009; K. Finlator et al. 2013; G. D. Becker et al. 2015; S. E. I. Bosman et al. 2022), initially dominated by Population III stars (K. Nakajima & R. Maiolino 2022; K. Nakajima et al. 2025), then by early star-forming galaxies (L. Jiang et al. 2022; J. Matthee et al. 2022), with active galactic nuclei (AGN) contributing significantly by z ∼ 5 (A. D’Aloisio et al. 2017; G. Kulkarni et al. 2019; C.-A. Faucher-Giguère 2020). Modeling indicates that pockets of Population III star formation may persist throughout the Epoch of Reionization (L. Tornatore et al. 2007; R. H. Mebane et al. 2018; J. L. Johnson & A. Aykutalp 2019; A. Venditti et al. 2023; O. Zier et al. 2025).\r\n\r\nThe large reservoir of neutral O i observed in quasar absorption lines at high redshift is typically self-shielded, providing robust estimates of chemical abundances. Studying the association of these absorbers with galaxies offers unique insight into the CGM of early galaxies, and into potential contributions from Population III stars to early chemical enrichment.\r\n\r\nIn this work, we study the cool, neutral CGM around galaxies at z ∼ 6, traced by O i absorption from the EIGER survey (D. Kashino et al. 2023). We focus on O i absorbers associated with [O iii]5008-emitting galaxies at 5.875 <z < 6.378 within 300 kpc of six background quasars. We quantify absorber incidence, column densities, and mass estimates, and analyze ionic abundances to probe chemical enrichment, including potential contributions from Population III stars.\r\n\r\nThis paper is organized as follows. Section 2 describes the observations; Section 3 details our methods for galaxy selection, redshift estimation, galaxy properties, defining galaxy overdensities, absorber measurements, and completeness; Section 4 presents the results, including the association of O i absorption with galaxies, the incidence of galaxy-associated O i absorbers, their chemical abundances, and physical interpretations; Section 5 summarizes our conclusions. Throughout, we adopt a ΛCDM cosmology with H0 = 67.66 km s−1 Mpc−1 (Planck Collaboration et al. 2020).\r\n\r\n2. Observations\r\nEIGER (Program ID 1243; PI: S. J. Lilly) is a large JWST Wide Field Slitless Spectroscopy (WFSS) program totaling 126.5 hr, conducting deep WFSS observations in six extragalactic fields, each centered on an ultraluminous quasar at z ≥ 6. These quasars have also been observed with deep optical and NIR medium- and high-resolution spectroscopy with Magellan/FIRE, Very Large Telescope/X-shooter, and Keck High Resolution Echelle Spectrometer (HIRES)/MOSFIRE, providing over 100 hr of complementary NIR spectroscopy across the six sight lines. We refer the reader to A.-C. Eilers et al. (2023) and A.-C. Ďurovčíková et al. (2025) for data reduction and details of the ground-based quasar spectroscopy. In addition, all fields are covered by deep JWST/NIRCam and HST imaging. A detailed description of the survey design, methodology, and spectroscopic and photometric observation details is provided in D. Kashino et al. (2023), J. Matthee et al. (2023), and R. Bordoloi et al. (2024). In this work, we make use of the complete EIGER survey of z ≥ 5.9 galaxies spanning all six extragalactic fields (D. Kashino et al. 2026).\r\n\r\nWe note that all six quasars were chosen with prior knowledge of metal absorption systems along their lines of sight, which could in principle bias any attempt to associate galaxies with those absorbers. In contrast, a galaxy-centric approach starts with quasar–galaxy pairs without prior knowledge of absorption and then builds statistics systematically (see e.g., R. Bordoloi et al. 2011; J. K. Werk et al. 2013; R. Bordoloi et al. 2014). However, once a blind, well-characterized galaxy survey is in place, the two approaches converge. This is conceptually similar to a program that combines quasar spectroscopy performed without prior absorber selection with a complete galaxy survey. This work employs deep blind galaxy searches in each of the EIGER fields, yielding an emission-line complete sample of spectroscopic galaxies (J. Matthee et al. 2022; R. Bordoloi et al. 2024) and a complete census of absorption lines along these sight lines (Section 3.5). By combining these two elements—a galaxy survey with quantified completeness and an absorption survey with well-defined sensitivity—we establish a robust framework for conducting a census of CGM absorption around galaxies. This combined approach has been successfully demonstrated at low redshifts (J. N. Burchett et al. 2019).\r\n\r\n3. Methods\r\nIn this section, we describe how galaxy redshifts and properties are measured and how absorption lines are identified and measured.\r\n\r\n3.1. Galaxy Redshifts\r\nSince our focus is on galaxies at z ∼ 6 near the quasar sight lines, we begin with the full EIGER catalog of [O iii] emitters (D. Kashino et al. 2026), which contains 948 galaxies detected via [O iii] emission within 5.33 ≤ z ≤ 6.97. From this catalog, we select galaxies that (1) lie at least 10,000 km s−1 in the foreground of each quasar , (2) are within a projected impact parameter of 300 pkpc, and (3) have O i λ1302 coverage in the quasar NIR spectra outside of the Gunn–Peterson trough. This yields a sample of 40 galaxies. Of these, 33 fall within the central of the EIGER spectroscopic footprint (R. Bordoloi et al. 2024), observed with both JWST/NIRCam reverse grism modules (A and B). Because the two modules disperse light in opposite directions, they provide independent moderate-resolution (R ∼ 1500) spectra of the same target, enabling us to assess redshift measurement uncertainties.\r\n\r\nFollowing the procedure in R. Bordoloi et al. (2024), we visually inspect each NIRCam 2D spectrum using the custom Python application programming interface (API) zgui(R. Bordoloi et al. 2025), extract 1D spectra from each module, and fit Gaussians to the emission line to determine redshifts. Redshifts from the two modules are consistent with a mean velocity offset of Δv = 9.3 km s−1 with a standard deviation of 24 km s−1 (Figure 1). We therefore adopt an average redshift uncertainty of ≈24 km s−1 for the [O iii] emitters, sufficient for associating metal absorption systems with their host galaxies. Hereafter, we focus on this sample of 40 galaxies.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. Redshift uncertainty distribution of the [O iii] emitter EIGER galaxies. The histogram shows the difference in redshift between emission-line measurements from NIRCam Grism Module A and Module B spectra, expressed in km s−1. Individual redshifts were derived from Gaussian fits to the [O iii] and Hβ lines. The two modules yield consistent results with a mean offset and standard deviation of Δz = 0.0028 ± 0.0073 (Δv = 9.3 ± 24 km s−1).\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\n3.2. Galaxy Stellar Mass, Star formation Rate, Halo Mass\r\nTo estimate galaxy stellar masses and star formation rates (SFRs), we follow the procedure of J. Matthee et al. (2022). We first measure the [O iii] and Hβ emission-line fluxes of each galaxy, and combine these with JWST/NIRCam broadband photometry (F115W, F200W, and F356W) to perform spectral energy distribution fitting at the galaxy redshift using the Prospector code (B. D. Johnson et al. 2021). We assume a G. Chabrier (2003) initial mass function (IMF), adopt MIST isochrones (J. Choi et al. 2016; A. Dotter 2016), a nonparametric star formation history model (R. P. Naidu et al. 2024), and the dust attenuation curve of D. Calzetti et al. (2000). Galaxy SFRs are derived by averaging over the most recent 50 Myr of star formation history from the Prospector posteriors.\r\n\r\nFigure 2 (left) shows the impact parameter distribution of the 40 EIGER galaxies relative to the background quasars (black star symbols). The galaxies are randomly distributed with respect to the quasar sight lines. The right panel shows their stellar masses and SFRs, with symbols color coded by galaxy redshift. Following R. Bordoloi et al. (2024), we estimate halo masses and virial radii (Rvir) using abundance matching from P. Behroozi et al. (2019). Uncertainties in Rvir are propagated from the 16th and 84th percentile stellar mass errors, giving a mean uncertainty of ΔRvir = 1.8 kpc. The galaxies span stellar masses of and SFRs of , with all systems being star-forming by selection.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 2. Properties of 40 spectroscopically confirmed galaxies at 5.9 ≤ z ≤ 6.4 within 300 kpc of background quasars in the EIGER survey. Each square denotes a galaxy and is color coded by redshift. Left: angular positions and impact parameters relative to the background quasar (black star), with dashed concentric rings marking 100, 200, and 300 kpc at z = 6. Right: stellar mass vs. SFR, averaged over the last 50 Myr. Error bars show the 16th–84th percentile uncertainties in stellar mass and SFR.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nOne galaxy (z = 5.910384, galaxyID = 15362, qsoID = J159) has an exceptionally high stellar mass of , beyond the calibrated range of the P. Behroozi et al. (2019) relation. This object exhibits a compact, pointlike morphology and likely hosts an obscured AGN, placing it among the recently identified population of little red dots (LRDs; e.g., J. Matthee et al. 2024). We do not detect broad Hβ for this object. However, this is not unexpected, as LRDs can have Hα/Hβ values as high as ∼10 (M. Brooks et al. (2025; A. Torralba et al. 2026, in preparation). As robust AGN modeling at these redshifts is not yet established, we estimated its halo mass by linearly extrapolating the P. Behroozi et al. (2019) relation from the stable stellar mass regime. We explicitly note where this assumption may affect our results in the following sections. Additionally, this galaxy has not been plotted in the right panel of 2.\r\n\r\n3.3. Galaxy Overdensities\r\nA significant fraction of z ≥ 6 galaxies in the EIGER survey are not isolated but are found in overdense environments, either as mergers or members of “protogroups” (see, e.g., D. Kashino et al. 2026). The EIGER [O iii] galaxy catalog already merges individual [O iii] emission clumps within 2″ into a single system, even when they exhibit complex morphologies or merger signatures. To identify larger-scale overdensities, we therefore search for galaxies that lie at similar redshifts but are widely separated on the sky.\r\n\r\nWithin 300 kpc from the QSO sight lines, we identify overdensities around the 40 selected EIGER galaxies using a friends-of-friends algorithm (R. Bordoloi et al. 2025). Galaxies are grouped as an overdensity if they lie within 1 pMpc in projected separation and within ±1000 km s−1 in redshift space. A galaxy is considered part of an overdensity only if all members are “fully” connected, i.e., each galaxy in the overdensity satisfies these conditions with all other members. Around each detected O i absorption system, we further search for overdensities within ±1500 km s−1 of the absorber redshift, and merge these associations to ensure all clustered galaxies are treated as a single overdensity. This conservative approach ensures that we capture the full galaxy environment of O i absorbers. The 40 galaxies studied in this work are part of 15 distinct overdensities, with each grouping containing 1–5 members. The number of galaxies in each grouping is reported in Table 1. The typical velocity dispersion of these overdensities is 449.2 km s−1.\r\n\r\nTable 1. O i Absorption Lines and Associated Galaxy Properties\r\n\r\nLabel\tQuasar\tzgala\tR\t〈v〉b\t#c\tzO I\t\t\t\t\t\r\n \t \t \t(kpc)\t(km s−1)\tGalaxies\t \t(cm−2)\t(cm−2)\t(cm−2)\t(cm−2)\t(cm−2)\r\n(1)\t(2)\t(3)\t(4)\t(5)\t(6)\t(7)\t(8)\t(9)\t(10)\t(11)\t(12)\r\na\tJ0100\t5.941\t119.6\t157\t5\t5.945\t\t\t\t\t\r\nb\tJ1148\t6.008\t157.5\t130\t3\t6.011\t\td\t\t\t\r\nc\tJ159\t5.934\t25.2\t−920\t5\t5.913\t\t\t\t⋯\t⋯\r\nd\tJ159\t6.049\t40.8\t230\t2\t6.054\t\t<13.12\t\t⋯\t⋯\r\ne\tJ1030\t6.075\t147.9\t−131\t2\t6.076\te\t\t\t⋯\t⋯\r\nNotes. The galaxies listed are the primary members of groups with detections at the lowest impact parameter from the host quasar. aRedshift of the primary member of the overdensity. bVelocity offset of O i relative to the primary member galaxy of the overdensity. cNumber of galaxy members in the overdensity. dFor this system, Si II λ1304 was not present, so the value given here is derived from fitting Si II λ1526. eThis system is blended; see discussion in Section 3.4.\r\n\r\nDownload table as: \r\nASCII\r\nTypeset image\r\n\r\nThroughout this work, we define the galaxy with the smallest impact parameter to the background quasar sight line within each galaxy overdensity as the primary member. This convention is adopted solely to simplify the presentation and does not imply a unique physical association between the intervening absorption system and this galaxy. In fact, the concept of a unique absorber–galaxy association at high redshift is significantly less robust than in the low-redshift Universe (e.g., R. Bordoloi et al. 2024). As discussed in Section 4.1, none of the O i absorption systems lie within the virial radius of any individual halo. Even at low redshift, the galaxy with the smallest impact parameter is not necessarily the one with the smallest velocity offset from the absorber, and therefore does not constitute evidence for a unique absorber–galaxy pair (A. Hamanowicz et al. 2020). This behavior is also observed for galaxies residing in groups (R. Bordoloi et al. 2011). Our analysis, therefore, focuses on the broader environment, which we argue is most appropriately characterized by galaxy overdensities, and our choice of a primary galaxy does not affect our main conclusions.\r\n\r\n3.4. Absorption-line Detection and Measurements\r\nWe follow the procedures outlined in R. Bordoloi et al. (2024) to identify and measure the strength of O i absorption systems around EIGER galaxies, and provide a brief summary here. We first use a custom Python-based 1D spectrum viewer to identify and tabulate all intervening absorption lines in the EIGER quasar spectra. A semiautomated CGM absorption-line analysis pipeline is then used to perform the measurements. For each galaxy, we extract a ±1500 km s−1 spectral window centered on its systemic redshift, for all transitions of interest. In this work, we analyze slices around O i λ1302, Si ii λ1260, Si ii λ1304, Si ii λ1527, C ii λ1334, Si iv λ1393, Si iv λ1402, C iv λ1548, and C iv λ1550. Each slice is locally continuum-normalized using an automated Legendre polynomial fit, with the polynomial order chosen via the Bayesian Information Criterion. The continuum fits and absorption features are visually inspected, and both rest-frame equivalent widths (Wr) and apparent optical depth (AOD) column densities are measured. We define a detection as any absorption system with Wr ≥ 3σw, where σw is the 1σ uncertainty in Wr. We note that this uncertainty contains both the statistical uncertainty due to the signal-to-noise ratio of the data and the continuum-fitting uncertainty. Nondetections are reported as 2σw upper limits measured within ±100 km s−1 of the systemic redshift of the galaxy. For column density, we report the 2σ uncertainty on AOD column density as an upper limit on nondetections. When a transition is detected in multiple instruments, each spectrum is analyzed independently, and the inverse-variance-weighted mean is adopted as the final Wr. The details of this automated approach and full documentation of the APIs used can be found in R. Bordoloi et al. (2025).\r\n\r\nFor all detections, we perform Voigt profile fitting using the rbvfit package, which employs Markov Chain Monte Carlo (MCMC) sampling to simultaneously fit multiple absorption systems across different instruments (R. Bordoloi & J. Higginson 2025). This approach yields robust column densities, resolves the kinematic structure, and enables accurate modeling of blended lines. Additionally, since we obtain a marginalized posterior distribution for the fitted parameters, the results yield accurate column density estimates even if the Doppler b parameter or velocity centroids are not well constrained in moderate-resolution spectra (see discussion in R. Bordoloi et al. 2024). In our case, most of the O i Si ii C ii transitions are all covered by higher-resolution HIRES spectroscopy and thus their properties are well constrained. rbvfit supports two MCMC samplers, emcee (D. Foreman-Mackey et al. 2013) and zeus (M. Karamanis et al. 2021; M. Karamanis & F. Beutler 2020), both of which are used in this work depending on the complexity of the fit. We typically adopt 50 walkers with initial perturbations of either 10−3 or 10−6, and default chain lengths of 8000–20,000 steps, ensuring the total number of steps exceeds 50 times the autocorrelation time. Additional steps are run as needed to achieve convergence. In each case, a flat prior is assumed with reasonable physical bounds.\r\n\r\nFigure 3 shows an example of Voigt profile fits to O i λ1302 and Si ii λ1304 lines simultaneously modeled across FIRE, X-shooter, and HIRES. We fit a two-component Voigt profile with a mean velocity offset from the host galaxy of voffset =  157 km s−1 . This joint fitting maximizes information from all instruments while preserving the kinematic detail provided by higher-resolution data. Galaxy overdensities associated with this system are marked with green vertical ticks. This system has a total O i column density 13.46. All other O i fits are presented in Figure 8. All absorption-line measurements are presented in Table 1.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Voigt profile fits to O i and Si ii absorption profiles at z = 5.945 toward the quasar SDSS J0100+2802. Shown are the flux (black), error spectrum (red), best-fit Voigt model (orange/black), and individual Voigt components (thin blue), using data from FIRE, X-shooter, and HIRES. Vertical green lines mark galaxy members of the associated overdensity. Spectra from all instruments and all transitions are simultaneously fit using the rbvfit Bayesian absorption-line fitter.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nWe note that an O i and Si ii absorption system is detected along the J1030 quasar sight line at z ∼ 6.075, blended with an intervening C iv absorber at z ∼ 4.948 (Figure 8, top left panels; see also C. G. Díaz et al. 2021). The z ∼ 6.076 system is confirmed by the independent detection of Si ii, Mg ii, C ii, and Fe ii absorption in FIRE and X-shooter data, and we simultaneously fit the C iv, O i, and Si ii systems across three instruments. Although the proximity of the C iv doublet in wavelength space introduces an inherent degeneracy with the O i and Si ii pair, high-resolution HIRES data reveal sufficient kinematic substructure to warrant an additional component at a mean velocity offset of voffset = –85.4 km s−1. We interpret this component as O i, supported by the aforementioned coincident detections. To constrain the system, we use the secondary lines to fix the velocity centroid of the O i component and perform simultaneous Voigt profile fitting across all three instruments, including both C iv transitions and single-component O i and Si ii models. The column density reported in this work corresponds to this singular O i component, and the system is marked with an asterisk in Table 1.\r\n\r\n3.5. O i Absorption Detection Completeness\r\nWe quantify the completeness of O i absorption detection around each galaxy as follows. For each galaxy overdensity, we compute the detection sensitivity on a pixel-by-pixel basis following the general framework of, e.g., K. M. Lanzetta et al. (1987), M. L. Bernet et al. (2010), and N. L. Mathes et al. (2017). In particular, we use a continuum-normalized spectral slice of ±1500 km s−1 centered on the expected O i absorption at the redshift of each galaxy overdensity.\r\n\r\nWe define the completeness in O i absorption detection in a single instrument as\r\n\r\nwhere H is the Heaviside step function, and is the equivalent-width cutoff at which completeness is defined. We adopt Å to facilitate comparison with the literature (see Section 4.2). Nσ is the detection threshold, which we set to Nσ = 3 by convention. The equivalent-width error, σEW(z), is given by\r\n\r\nwhere Δλj is the wavelength spacing between adjacent pixels (set by the spectrograph), and npix is the number of pixels over which the equivalent width is computed. We adopt the typical width of an O i absorber as npix for our analysis, yielding npix, X-shooter = 10, npix, HIRES = 50, and npix, FIRE = 11, respectively. This is a conservative approach to calculating completeness, as the typical width of the absorbers is larger than the resolving power of the instruments. We neglect continuum-fitting errors, so σEW(z) reflects only statistical uncertainties from the spectra. Any chip gaps or sky lines are masked. σI and Ic are the flux uncertainty and continuum levels of the spectrum.\r\n\r\nFor galaxy overdensities observed with multiple spectrographs, we define the combined completeness as requiring detection in at least one instrument across the relevant wavelength range. For example, with three or more instruments available,\r\n\r\nwhere the logical OR (∨) runs over all instruments i ∈ X-shooter, FIRE, HIRES. We then compute the mean completeness for each overdensity, and obtain the overall mean completeness, , by averaging over all overdensities weighted by their wavelength coverage. This yields a mean completeness of 91.4% for O i absorption around galaxy overdensities in the EIGER survey for 0.05 Å.\r\n\r\n4. Results\r\nIn this section, we present the variation of O i absorption around z ∼ 6 galaxies, the incidence of O i absorption per comoving path length that is due to O i absorption around galaxies, and the chemical abundance of these systems.\r\n\r\n4.1. Variation of O i Absorption around Galaxies\r\nSince all 40 galaxies in our sample reside within 15 identified overdensities (Section 3.3), we investigate whether O i absorption is preferentially detected in these environments. For clarity, we show the primary galaxy in each overdensity (as defined in Section 3.3) when presenting the radial distribution of O i absorption. Out of the 15 overdensities, 5 show associated O i absorption.\r\n\r\nFigure 4 shows the 2D spatial distribution of galaxies around these five detected systems, with the size depicting the virial radii of the galaxies. The galaxies are randomly distributed around the absorbers, and we do not find correlations with stellar mass, star formation, or other galaxy properties. In all five cases where we have O i detection, the galaxy member with the minimum impact parameter is also the member with the lowest R/Rvir.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. Galaxy overdensities around z ∼ 6 O i absorbers in the EIGER survey. Each panel shows the background quasar (red star) at the center, with foreground galaxies associated with O i absorption marked as circles. Circles are color coded by the velocity offset between the galaxy and the O i absorber, and circle sizes are scaled to their virial radii. Only galaxies within 300 kpc of the quasar are shown, highlighting the overdensities nearest the absorbers. Dashed circles denote projected impact parameters of 50, 100, 200, and 300 pkpc from the quasar.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nFigure 5 presents 1D the radial profiles around the primary galaxies in these systems. The marker size indicates the number of member galaxies in each overdensity, while the color encodes the velocity offset from the corresponding O i absorption. Panels (a) and (c) show impact parameter (R), and panels (b) and (d) show the same distribution normalized by the halo virial radius (R/Rvir).\r\n\r\nZoom InZoom OutReset image size\r\nFigure 5. Radial absorption profiles of O i absorption at z ∼ 6. Each point marks the impact parameter to the nearest galaxy in a galaxy overdensity, with all detected O i absorption arising in such environments. Overdensities with O i absorption are shown as circles, while nondetections (2σ limits) are indicated by downward arrows. Points are color coded by the velocity offset between the galaxy redshift and the O i absorber, and their size scales with the number of members in the overdensity. The mean uncertainty on the virial radius is ΔRvir = 1.81 kpc. Top panels: rest-frame equivalent width vs. impact parameter (R, left) and normalized impact parameter (R/Rvir, right). Bottom panels: same as above, but for O i column densities.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nMost of the O i detections occur within R ≲ 175 kpc of the primary galaxy, corresponding to an incidence rate of , estimated using 68% Wilson score confidence intervals. Within 100 kpc, the incidence is , increasing to for R ≤ 50 kpc. Conversely, at R  >  150 kpc, an incidence of is measured. Within 300 kpc of the primary galaxy, the overall incidence is , with values of for 50 ≤ R ≤ 300 kpc and for 100 ≤ R ≤ 300 kpc. These rates are substantially weaker than the incidence of strong Mg ii absorption at z ∼ 6 (R. Bordoloi et al. 2024), indicating that neutral oxygen preferentially traces a different phase of the circumgalactic environment.\r\n\r\nPanels (b) and (d) reveal that O i absorbers are typically located at much larger R/Rvir than strong low-ionization tracers such as Mg ii. This distinction suggests that O i absorption at z ∼ 6 is not confined to the CGM of an individual galaxy but instead reflects the larger-scale gaseous environment of galaxy overdensities—what might be described as “cosmic ecosystems” rather than isolated halos.\r\n\r\nComparing the stellar mass distributions of overdensities with and without O i absorption, we find no statistically significant differences. The mean stellar mass of galaxies in overdensities with absorption is , compared to for those without.\r\n\r\nWe emphasize that at z ∼ 6, the large R/Rvir values of these halos imply that O i absorption typically arises at scales well beyond the typical CGM [R/Rvir ≲ 1] (J. Tumlinson et al. 2017) probed by low-ionization lines at lower redshift. Unlike the low-z CGM, where metal absorbers are closely tied to the halo of a single massive galaxy, the O i absorbers studied here appear to be linked to extended networks of low-mass, young galaxies embedded in shared overdensities. Over cosmic time, these small systems and their diffuse gaseous environments are expected to merge and evolve into more massive systems, eventually forming Milky Way–like galaxies by z = 0. Thus, neutral O i at reionization is best understood not as a tracer of isolated galactic halos, but as a probe of the extended environments that connect galaxies, gas, and structure growth in the early Universe.\r\n\r\nBecause O i absorption traces dense, neutral gas and requires only minimal ionization corrections, we can place a conservative lower limit on the total oxygen mass associated with the EIGER galaxies. These estimates are intended as simple, order-of-magnitude calculations to provide intuition about the amount of neutral oxygen relative to the observed galaxy properties. Following the formalism of R. Bordoloi et al. (2014), the oxygen mass contained in an annulus bounded by Rin and Rout is\r\n\r\nwhere Rin and Rout are the inner and outer radii of the annulus, fc is the covering fraction (the incidence of O i detections in that bin), 〈NOI〉 is the mean O i column density in the annulus, and mO = 16 mp is the mass of an oxygen atom, with mp being the mass of a proton. For a conservative lower limit, we adopt fion = 1, where fion is the ionization fraction (i.e., we assume that all of the oxygen mass is in the neutral phase). We justify this assumption as follows: O i is tightly coupled to H i through charge exchange, and in dense gas, the required ionization correction is minor, even under strong radiation fields such as the Fermi Bubbles (R. Bordoloi et al. 2017; T. Ashley et al. 2022). Under a typical metagalactic UV background, it is generally less than 10% and does not significantly alter the inferred oxygen abundance. In addition, oxygen does not deplete onto dust grains, unlike Si or C. For these reasons, we consider the approximation NO,total ≈ NOI to be valid for our analysis.\r\n\r\nWe compute masses in two radial bins: 0–100 kpc and 100–300 kpc, respectively. The total oxygen mass within radius is obtained by summing the masses of the constituent annuli. This yields a strict lower limit of  ≳  2 ×106M⊙ on the total oxygen mass within = 300 kpc.\r\n\r\nWe compare the inferred oxygen mass in the extended environment of our sample with the total oxygen content in the interstellar medium (ISM) of a typical z ∼ 6 galaxy. In computing this quantity, we make the following assumptions. First, we assume that all galaxies in this work lie on the typical z ∼ 6 mass–metallicity relation, derived by stacking [O iii] emitter galaxies (J. Matthee et al. 2022), and we adopt the gas-phase metallicity from this relation for each galaxy.\r\n\r\nBecause direct measurements of the total H2 and H i gas content are not available at these redshifts, we extrapolate the molecular gas fraction from L. J. Tacconi et al. (2018) to z ∼ 6 and adopt a conservative H i gas fraction based on local observations (S. Huang et al. 2012). We note that high-z galaxies are likely more gas-rich than their local counterparts; therefore, the inferred ISM gas masses should be considered lower limits.\r\n\r\nWith these caveats in mind, we estimate the total ISM oxygen mass as\r\n\r\nwhere we define . Here, XO is the gas-phase oxygen abundance derived from the mass–metallicity relation, and and MHI are the molecular and atomic gas masses derived as described above. For our galaxy sample, the mean stellar mass is , corresponding to an ISM oxygen mass of MO,ISM  ≳  6.8 × 105 M⊙. Remarkably, this indicates that the typical ISM oxygen content is comparable to the oxygen mass in the extended environment around these galaxies, implying that the circumgalactic or intergalactic medium at z ∼ 6 contains a substantial reservoir of oxygen. While these estimates depend on several specific assumptions, the inferred ISM and CGM oxygen masses appear to be of similar magnitude.\r\n\r\nAt low redshift, both L* and sub-L* galaxies similarly exhibit substantial metal content in their circumgalactic medium (CGM), with the CGM containing at least as much metal as the ISM of their host galaxies (J. Tumlinson et al. 2011; R. Bordoloi et al. 2014). A key difference is that, whereas the low-z CGM is typically gravitationally bound to its host galaxy, at high redshift much of the gas exists in the extended environment of galaxy overdensities rather than being bound to individual galaxies (see also R. Bordoloi et al. 2024).\r\n\r\n4.2. Expected Incidence of O i Absorbers\r\nIn this section, we report the expected redshift-path incidence of O i absorbers around [O iii] emitting galaxies detected in the EIGER survey. We define the number of O i absorbers associated with each galaxy overdensity per unit absorption distance above a detection threshold (WOI ≥ 0.05Å ) as\r\n\r\n\r\nHere, Rmax = 300 kpc is the survey radius adopted in this work, and is the mean O i absorber detection completeness (see Section 3.5; 91.4% for WOI ≥ 0.05 Å). nOD is defined as\r\n\r\n\r\nngal is the number density of [O iii] emitting galaxies per unit comoving volume, estimated from the [O iii] luminosity function at z ∼ 6. And 〈overdensity size〉 is simply the mean number of galaxies in each galaxy overdensity empirically measured to be 〈overdensity size〉 = 2.67. fc is the O i absorption covering fraction within 300 kpc for WOI ≥ 0.05 Å (). (The covering fraction within 300 kpc is independent of the definition of the primary member.)\r\n\r\nTo estimate the number density of galaxies per unit comoving volume (ngal), we integrate the z ∼ 6 [O iii] luminosity function derived from the EIGER survey, with a minimum luminosity of Lmin = 1042.2 ergs−1 (J. Matthee et al. 2022):\r\n\r\n\r\nwhere Φ(L) is the [O iii] luminosity function defined as\r\n\r\n\r\nHere, Φ* is the characteristic number density, L* is the characteristic luminosity, and α is the faint-end slope. We adopt Φ* = 10−4.02 Mpc−3, L* = 1043.33 ergs−1, and α = −1.92, values derived from detailed completeness calculations of the EIGER [O iii]-emitting galaxies (R. Mackenzie et al. 2026, in preparation). This results in ngal = 8.586 × 10−04 Mpc−3. Using these values in Equation (6) yields , for O i absorption around galaxies at a mean galaxy redshift of 6.001.\r\n\r\nAll calculations in this section are performed with a detection threshold of WOI > 0.05Å, since the survey is highly complete down to this equivalent-width limit and because most of the literature surveys we compare against adopt the same threshold.\r\n\r\nWe emphasize that this approach differs from blind QSO absorption-line surveys (e.g., G. D. Becker et al. 2006; L. Christensen et al. 2023; A. M. Sebastian et al. 2024; A. Sodini et al. 2024), where all O i absorption-line systems along the full quasar redshift path are counted to compute dN/dX directly, under the assumption that the absorber cross section is contributed by all galaxies. In contrast, our method begins by defining the absorber cross section around galaxy overdensities and then estimating the corresponding contribution to dN/dX from the galaxy overdensities under study. Comparing these two approaches constrains the fraction of O i (or other metal) absorption systems that arise in the extended halos of these galaxies. Figure 6 shows these literature measurements as colored circles, while the contribution to dN/dX around z ∼ 6 galaxy overdensities is indicated by an orange square. To quantify the relative contribution of galaxy overdensities, we fit a single power law to all literature values at z  >  4 (blue dashed line with shaded region). Comparing the dN/dX inferred from quasar absorption-line surveys at z ∼ 6 to our measured value, we find that O i dN/dX around z ∼ 6 EIGER galaxy environments account for 35% ± 16% of all O i absorption-line systems detected in blind quasar surveys. This implies that [O iii] emitting galaxy environments at z ∼ 6 contribute roughly one-third of the O i absorption systems at that epoch. Although the EIGER QSOs were selected to have known absorption systems along their sight lines, the EIGER galaxy survey around these sight lines is highly complete and independent of this selection. Therefore, we can create an unbiased measurement of the absorption cross section (dN/dX) around these galaxy overdensities. We justify this comparison to blind absorption surveys in Section 2.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Incidence of O i absorbers per comoving path length, dN/dX. Values are derived from all O i absorption lines along high-z quasar sight lines. Literature measurements are shown from G. D. Becker et al. (2019; blue circles), L. Christensen et al. (2023; purple circles), and A. M. Sebastian et al. (2024; red circles). The blue dashed line shows a power-law fit to the z  > 4 literature data, with the shaded region marking the 1σ uncertainty. The orange square gives the inferred dN/dX when including only O i absorption associated with host galaxies (see Section 4.2), indicating that only ∼35% of O i absorbers at z ∼ 6 arise in galaxy environments.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nThis in turn suggests that ∼65% of the O i absorption systems detected along quasar sight lines at the epoch of reionization are not associated with [O iii] emitter galaxy overdensities. Either the bulk of O i absorption resides in isolated pockets of neutral IGM gas outside extended galaxy halos, or it is contributed by even lower-luminosity, less massive galaxies () that fall below the EIGER detection limits. Such systems may also be detected in galaxy halos that are oxygen-poor or lack strong [O iii] emission features, since our galaxy identifications primarily rely on [O iii] and Hβ emission lines.\r\n\r\nSimulations suggest that O i absorption should primarily arise in galactic halos rather than in the diffuse IGM, since metals are not widely distributed and ionization fronts propagate more quickly than metals (B. D. Oppenheimer et al. 2009; K. Finlator et al. 2013). Very low-mass protogalaxies forming their first stars may blur the boundary between IGM and CGM, enriching their surroundings with metals, especially if their star formation is bursty and prolific. If sufficiently numerous, such systems could contribute a nonnegligible fraction of oxygen in the early Universe.\r\n\r\nRecent observations support this possibility. K. Nakajima et al. (2025) reported a strongly lensed (μ = 98) galaxy at z ≈ 6.6 with a stellar mass upper limit of only ∼2700 M⊙ and a dynamical mass ∼100 times larger. The source shows emission and may be dominated by Population III stars. This provides direct evidence of oxygen production in extremely low-mass systems. A population of such ultralow-mass dwarf galaxies could plausibly account for the ∼65% of O i absorbers detected along quasar sight lines that are not associated with galaxies in our survey. Our sensitivity limit of (J. Matthee et al. 2022) means such dwarfs remain undetected. However, these galaxies may lack a dense enough CGM to shield neutral O i from the UV background; thus, even if they produce oxygen, neutral O i may not survive (K. Finlator et al. 2013). Interestingly, simulations by S. Kušmić et al. (2024) showed that the contribution of metal ions, including O i, is only weakly correlated with the stellar mass of the galaxy, and the contribution is indistinguishable when comparing across galaxy luminosities. Additionally, they argue that due to the steep slope of the stellar mass function, lower-mass, lower-luminosity galaxies contribute the majority of absorbing metal ions in the CGM and IGM.\r\n\r\nLater simulation works by C. Doughty et al. (2018); C. Doughty & K. Finlator (2019) suggest that as the Epoch of Reionization continues, O i will reduce overall but be preferentially found in higher column density regions close to halos, as they have a better ability to self-shield from ionizing photons. In fact, C. Doughty & K. Finlator (2019) found that at z = 6 the majority of O i mass was located in the ISM of galaxies and only ∼30% of O i mass was found in the CGM and IGM. In contrast, in this work, we find that a substantial (comparable to ISM mass) oxygen mass exists outside galaxies; however, we stress that our mass measurements are order-of-magnitude estimates. A more direct comparison between these simulations and this work is the covering fraction. They report ∼5%–25% covering fraction at z = 6 for O i with out to 102 pkpc. In the EIGER survey, we report a covering fraction using a minimum threshold of WOI ≥ 0.05 Å (or approximately logNOI > 13.7 cm−2) out to 300 kpc. Given the large measurement uncertainties and different definitions of associated galaxies, the covering fractions are qualitatively consistent between the two works.\r\n\r\nThe simulations of K. Finlator et al. (2013) suggest that O i absorbers with are most likely associated with halos of mass ∼109 M⊙, where self-shielding is efficient. They further predict that only ∼13% of all O i absorption systems should reside in halos of 1010–1011.5 M⊙, the mass range of galaxies probed in this work. By contrast, we measure a higher dN/dX of ∼35%, but qualitatively our results remain consistent with the idea that roughly two-thirds of O i absorbers are associated with undetected ∼109 M⊙ halos. Future observations targeting lower-luminosity galaxies and higher redshifts will be essential to test these predictions.\r\n\r\nAfter the initial posting of this manuscript, G. Pruto et al. (2026) presented a simulation-based study that adopts the observational compilation shown in Figure 6 as a reference and explores the corresponding behavior in numerical models. Our minimum Wr threshold corresponds to ; therefore, the most appropriate comparison is with their sample. Qualitatively, the two sets of results are in agreement. A key distinction lies in the definition of galactic environment. We characterize environments in terms of galaxy overdensities, which we argue is the most appropriate description of where O i absorbers reside at z ≈ 6, whereas G. Pruto et al. (2026) define the CGM based on the virial radii of halos with . As a result, a direct quantitative comparison is not straightforward. Nevertheless, their inferred dN/dX corresponds to an incidence rate of O i absorbers of ∼58% ± 11%, which is consistent with our measurements within the uncertainties. This agreement may depend on their tighter constraints on absorber location and on the adopted minimum Wr or threshold. G. Pruto et al. (2026) further report that ∼80% of O i absorbers with are predicted to lie outside the CGM, also in qualitative agreement with our findings.\r\n\r\n4.3. Metal Abundances in O i absorber population\r\nIn this section, we examine the relative abundances and metal column density ratios of O i absorbers associated with galaxy overdensities, and compare them to O i absorbers without any associated galaxies. To enable a fair comparison, we restrict our analysis to the six quasar sight lines from the EIGER survey and identify all O i absorption systems in the redshift range where an [O iii]-emitting galaxy could be detected (5.9 ≤ zOI ≤ zQSO). We detect 10 O i absorption systems in total, 5 of which have associated galaxy overdensities (Table 1) and 5 are without any identified galaxy association.\r\n\r\nWe first compare the ionic column density ratios in these two populations. Figure 7 (top panels) shows the ratios of NSiII/NOI and NCII/NOI as functions of NOI. Systems located near galaxy overdensities (blue squares) systematically show higher Si ii/O i and C ii/O i ratios compared to systems without associated overdensities (green crosses). This offset could reflect differences in metallicity, or alternatively, the effects of ionization. However, since the majority of these O i systems lack detectable high-ionization transitions, it is reasonable to assume that neutral oxygen and singly ionized silicon and carbon dominate the elemental reservoirs (see also L. Christensen et al. 2023). In those cases, the observed ionic ratios provide direct tracers of relative abundances. Two exceptions are found along the J0100 and J1148 sight lines, which do exhibit Si iv and C iv absorption; for these systems, the degeneracy between chemical composition and ionization corrections cannot be resolved. It is plausible that, on average, O i absorption found near galaxy overdensities has higher elemental abundance ratios as the non-galaxy-associated absorbers either have significantly lower-luminosity and less massive galaxies, which would be expected to produce less metal, or there are truly no galaxies associated with this population.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 7. Top panels: ion column density ratios of Si ii to O i (left) and C ii to O i (right) as a function of the detected O i column densities, shown in logarithmic units. Absorbers associated with galaxy overdensities (blue squares) and those not associated with galaxy overdensities (green crosses) exhibit clear variations in their column density ratios. One sight line with no detected Si ii absorption is indicated with a downward arrow, where a 2σ upper limit on the column density is assumed. Bottom panel: relative abundance ratios [Si/O] vs. [C/O] with respect to solar abundance. The background contours show the IMF-weighted abundance distributions from Population II and Population III SN models. Orange and pink circles indicate abundance ratios predicted by low-metallicity Population II SN models. The abundance ratios of several O i absorbers associated with galaxy overdensities are consistent with a significant contribution from Population III SNe.\r\n\r\nDownload figure:\r\n\r\nStandard image\r\nHigh-resolution image\r\nWe next compute the relative abundances [Si/O] and [C/O], presented in the bottom panel of Figure 7. These abundances are defined as\r\n\r\n\r\nwhere NSi,tot and NC,tot represent the summed ionic column densities. For systems with detected high-ionization absorption (C iv or Si iv), we include both low- and high-ionization states (NSiII + NSiIV and NCII + NCIV), marking these measurements as lower limits (blue upward arrows in the figure) since additional undetected ionization states may be present. We note that in the two systems (a and b) exhibiting high-ionization absorption (see Table 1), the low- and high-ionization absorption components are offset in velocity by Δv = –66 km s−1 and –69 km s−1, respectively. These offsets are within ≲1.5 resolution elements of the instrument, and therefore we cannot statistically distinguish whether the low- and high-ionization components are kinematically distinct. This is suggestive of a complex, potentially multiphase gaseous environment in the outskirts of these galaxies. For systems without detected high-ionization transitions, we adopt NSiII and NCII as the dominant contributions. We assume NO,tot ≈ NOI, as ionization corrections for O i are typically very small at high O i column densities (see Section 4.1 for discussion). We adopt solar reference abundances of = −1.18 ± 0.05 and (M. Asplund et al. 2021).\r\n\r\nFigure 7 (bottom panel) reveals a striking separation between O i absorbers associated with galaxy overdensities (blue squares) and those without galaxy associations (green crosses). Systems near galaxies are found in the upper left of the [Si/O]–[C/O] diagram, with two cases exhibiting high-ionization absorption (lower abundance limits, blue arrows), which will offset them even farther from the locus of nongalaxy absorbers.\r\n\r\nWe place these abundance patterns in the context of chemical enrichment models from different stellar populations (see also L. Christensen et al. 2023). The contours and colored circles in Figure 7 highlight predicted [C/O] and [Si/O] yields from representative Population II and Population III supernova (SN) models, weighted by a Salpeter IMF. The weighting by number of stars predicted by an IMF is done to represent the typical observational relative abundance distribution in these models. These are not exhaustive but span the dominant theoretical expectations.\r\n\r\nPopulation III pair-instability SNe (PISNe; 140–260M⊙; light green contours) predict narrow [C/O] ≃ –0.7 and high [Si/O] values, inconsistent with any of our observed systems. Such PISNe are also expected to produce substantial amounts of iron-peak elements, leading to elevated Fe/O ratios (J. Tumlinson et al. 2004). We will investigate Mg ii and Fe ii absorption associated with z ∼ 6 galaxies in an upcoming work (J. Higginson et al. 2026, in preparation). Models of massive Population III stars (10–100 M⊙) produce both hypernovae (gray contours; E > 1052 erg) and standard core-collapse SNe (light blue contours; A. Heger & S. E. Woosley 2010), spanning a broader region overlapping some of our measurements. We also consider Population II models: low-metallicity core-collapse SNe from M. Limongi & A. Chieffi (2018; orange contours, Population II SNe (L18)) occupy −0.25 ≲ [C/O] ≲ 0.5 and −0.4 ≲ [Si/O] ≲ 0.4, overlapping parts of the Population III range, while the C. Kobayashi et al. (2006) yields (pink and orange circles for hypernovae and SNe, respectively) tend toward lower [Si/O] and [C/O].\r\n\r\nAgainst these predictions, the contrast between the two absorber populations is clear. All nongalaxy O i systems (green crosses) fall at the lower left of the diagram, consistent with enrichment from both Population II and/or Population III SNe models. This regime also overlaps with ultra-metal-poor damped Lyman-α absorbers (DLAs) at z ∼ 3 (−0.5 ≲ [Si/O] ≲ 0, −0.5 ≲ [C/O] ≲ 0; R. Cooke et al. 2011; R. J. Cooke et al. 2017). By contrast, three of the five galaxy-associated absorbers lie well outside both the locus of Population II predictions and the locus of ultra-metal-poor DLA relative abundances. These systems are best explained if Population III enrichment played a major role, suggesting that they may represent a distinct population from ultra-metal-poor DLA host galaxies (see also A. Sodini et al. 2024).\r\n\r\nSimilarly, A. Sodini et al. (2024) found that the [C/O] and [Si/O] abundance ratios for high-redshift O i absorber systems are consistent with significant enrichment from Population III, with the majority explained by ≥ 30% contributions. They also find a large spread in the implied Population III contribution; several systems require ≥ 60% contributions, while others fall significantly below the average. This is a strong indication of heterogeneous chemical enrichment by Population III stars during the epoch of reionization.\r\n\r\nThe absorber toward J159 at z = 5.91 shows [C/O] = 0.20, [Si/O] = 0.55 (labeled c), and no evidence of high-ionization absorption. These abundance ratios are best explained by contributions from Population III SNe or hypernovae. The absorber toward J1030 at z = 6.07 ([C/O] = −0.38, [Si/O] = 0.65, labeled e) also shows no high-ionization absorption. The relative abundances in these two predominantly neutral systems are therefore quite robust. Interestingly, the J1030 system is not reproduced by any single Population II or Population III model, suggesting that it may have experienced multiple enrichment episodes, producing unusually high [Si/O] coupled with low [C/O].\r\n\r\nTwo cases require special mention. The absorber toward J0100 at z = 5.94 shows [C/O] ≥ 0.42 and [Si/O] ≥ 0.67 (labeled a), with strong C iv and Si iv absorption. Since these are lower limits, ionization corrections (for carbon and silicon) would push this system further upward, strengthening the case for Population III contributions. This observation is best explained by contributions from Population III hypernovae models. The J1148 absorber at z = 6.01 shows [C/O] ≥ 0.02 and [Si/O] ≥ 0.20 (labeled b), again with high-ionization lines; correcting for ionization would shift it diagonally upward in the diagram. Taken together, four of the five galaxy-associated absorbers show relative abundances that cannot be explained by Population II models alone, pointing instead to significant enrichment from Population III SNe or hypernovae.\r\n\r\nThus, most galaxy-associated O i systems carry signatures of Population III enrichment. These results suggest that O i systems tracing galaxy overdensities at z ∼ 6 carry chemical signatures of Population III enrichment, likely from multiple SNe events rather than a single explosion. The elevated [Si/O] and [C/O] ratios in these environments imply that [O iii]—emitting galaxies at this epoch may retain significant Population III contributions, and that metal-line absorbers around such overdensities provide a powerful probe of the first generations of stars.\r\n\r\n4.4. Comparison to the z ≈ 0 Universe\r\nAt z ∼ 6, we cannot directly detect the local environments where O i absorption systems arise. However, at z ∼ 0, there are instances where the environments giving rise to O i absorption are well understood. Here, we discuss several such instances and compare them with z ∼ 6 observations. Such comparisons can provide useful insights regarding the nature of local environments within which O i systems exist at high z. We focus on O i absorption associated with local blue compact dwarf (BCD) galaxies and the Magellanic Stream (MS), owing to their low metallicities and well-characterized local environments.\r\n\r\nThere is evidence that O i is found preferentially in the H ii regions of local BCDs, with their H i regions being pristine or showing very low levels of enrichment (D. Kunth et al. 1994; M. Pettini & K. Lipman 1995; T. X. Thuan & Y. I. Izotov 1997). In particular, T. X. Thuan & Y. I. Izotov (1997) report that, to varying degrees, low-ionization metal lines (e.g., O i and Si ii) reside in the ionized hydrogen regions of BCDs rather than the neutral hydrogen regions. They report . Compared to the z ∼ 6 measurements in panel (b) of Figure 7, the O i column density of the BCD is comparable, but the Si ii-to-O i ratio is inconsistent with the z ∼ 6 values. On the other hand, V. Lebouteiller et al. (2004) find that the H ii region of the BCD I Zw 36 has significantly higher metallicity than its H i region. However, inferred from velocity offsets, O i in that system is associated with the H i region. The reported O i column density of that BCD () is approximately 2 orders of magnitude higher than the z ∼ 6 sample. Given the available evidence, we conclude that the observed z ∼ 6 O i absorption systems are not similar to local BCD systems and are unlikely to originate in H ii regions.\r\n\r\nThe MS is a filamentary trail of gas in the Local Group. Multiphase absorption-line observations from A. J. Fox et al. (2013) and P. Richter et al. (2013) support the argument that the MS was tidally stripped from the Magellanic Clouds approximately 2 Gyr ago. Inferences from the abundance ratios of alpha elements in the MS are best explained by contributions from massive stars via Type II SNe when the MS was still part of the Magellanic Clouds, although the presence of significant dust depletion makes further inferences into enrichment history difficult. An additional study of the MS (N. Kumari et al. 2015) reports abundance ratios in a compact high-velocity cloud (CHVC) that is believed to be associated with the MS. They find [Si/O] = −0.04 ± 0.25 and [C/O] = −0.09 ± 0.23. When comparing these with the z ∼ 6 observations presented in panel (c) of Figure 7, we see that the CHVC abundance ratios occupy a different region of parameter space than the z ≈ 6 O i absorbers within identified galactic overdensities showing Population III enrichment signatures (points a, c, e). This discrepancy provides evidence that these z ∼ 6 O i absorbers with Population III enrichment signatures are unlikely to arise in environments similar to the MS. However, the ionic ratios of O i absorption systems not associated with galaxy overdensities (green crosses) are consistent with this measurement. With the caveat that MS measurements do contain dust depletion effects, it is plausible that such O i systems may trace IGM structures with densities comparable to those of the MS at high z.\r\n\r\n5. Conclusion\r\nWe have conducted a survey of neutral O i absorption systems associated with galaxies during the Epoch of Reionization in the EIGER survey, using six high-redshift quasars as background sight lines. Our study focuses on the distribution of neutral oxygen around -emitting galaxies within 300 kpc and their connection to galaxy overdensities. The main results are as follows:\r\n\r\n1.  \r\nFive O i absorbers are detected among 15 galaxy overdensities, spanning z = 5.91–6.16 with a mean redshift 〈z〉 = 6.001.\r\n2.  \r\nThe O i covering fraction within 300 kpc of the closest galaxy is , with for R ≤ 50 kpc and for 50 ≤ R ≤ 300 kpc, where the covering fraction is calculated using the galaxy in an overdensity with the lowest impact parameter.\r\n3.  \r\nWe find  ≳ 2 × 106 M⊙ of oxygen within 300 kpc, a mass comparable to the ISM oxygen content of z ∼ 6 galaxies—assuming minimal ionization correction (see Section 4.1 for justification)—suggesting that the circumgalactic environment already holds metal reservoirs rivaling those inside galaxies.\r\n4.  \r\nO i absorbers are detected as far as ∼8 R/Rvir from galaxies, in sharp contrast to low-ionization tracers such as Mg ii, which are typically confined within ≲R/Rvir.\r\n5.  \r\nThe incidence of galaxy-associated O i absorbers is \r\n \r\n. Comparison with blind quasar absorption-line surveys indicates that these systems represent only ∼35% of all O i absorbers at z ∼ 6, implying that the majority likely arise in lower-mass galaxies below current detection limits or in dense neutral IGM pockets that survived reionization.\r\n6.  \r\nRelative abundance and ionization ratios ([Si/O], [C/O]) show that galaxy-associated O i systems are chemically enriched, with signatures in several systems consistent with contributions from Population III stars. In particular, we identify four galaxy overdensities whose outskirts exhibit absorption-line abundance ratios consistent with contributions from Population III nucleosynthesis.\r\n\r\nOverall, these results indicate that neutral O i at z ∼ 6 primarily traces extended overdensity environments rather than the CGM of individual halos. Moreover, the chemical abundance patterns of galaxy-associated O i systems suggest contributions from Population III stars, likely arising from multiple SNe events rather than a single explosion. The elevated [Si/O] and [C/O] ratios imply that [O iii]-emitting galaxies at this epoch may retain significant Population III enrichment. Consequently, metal-line absorbers around such overdensities offer a powerful probe of the first generations of stars, providing insight into early chemical enrichment and the role of primordial stellar populations in shaping galaxy evolution during the Epoch of Reionization.\r\n\r\nAcknowledgments\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 #1243. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration (NASA) through the agency’s scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The JWST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via DOI: 10.17909/y94q-h212. This work was partially supported by the National Science Foundation under grant No. AST-2108931. Jorryt Matthee and Ivan Kramarenko acknowledge funding from the European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities: JWST - James Webb Space Telescope (NIRCam), Magellan: Baade - (FIRE), VLT: Kueyen - (X-shooter), and Keck: I - (HIRES, MOSFIRE).\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018, 2022), rbcodes (R. Bordoloi et al. 2025), rbvfit (R. Bordoloi & J. Higginson 2025).","type":"journal_article","issue":"1","article_type":"original","author":[{"first_name":"Jack","full_name":"Higginson, Jack","last_name":"Higginson"},{"first_name":"Rongmon","full_name":"Bordoloi, Rongmon","last_name":"Bordoloi"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","last_name":"Kramarenko"},{"last_name":"Lilly","full_name":"Lilly, Simon J.","first_name":"Simon J."},{"full_name":"Eilers, Anna-Christina","last_name":"Eilers","first_name":"Anna-Christina"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"full_name":"Yue, Minghao","last_name":"Yue","first_name":"Minghao"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-10-12T12:15:27Z","_id":"23115","status":"public","article_processing_charge":"Yes","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"arxiv":1,"ddc":["520"],"doi":"10.3847/1538-4357/ae3e81","has_accepted_license":"1","title":"EIGER. VIII. First stars signatures in the connection between O I absorption and galaxies in the epoch of reionization","publication_status":"published","external_id":{"arxiv":["2510.05220"]},"article_number":"49","publication":"The Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"OA_place":"publisher","DOAJ_listed":"1","publisher":"IOP Publishing","year":"2026","language":[{"iso":"eng"}],"volume":999,"file":[{"access_level":"open_access","success":1,"date_created":"2026-10-14T07:50:51Z","file_size":2808503,"checksum":"1b8caf640c32d0d27a078bfb27ffcf8a","date_updated":"2026-10-14T07:50:51Z","file_name":"2026_AstrophysicalJour_Higginson.pdf","content_type":"application/pdf","file_id":"23136","relation":"main_file","creator":"dernst"}],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"fulldoi":"https://doi.org/10.3847/1538-4357/ae3e81","oa_version":"Published Version","citation":{"short":"J. Higginson, R. Bordoloi, R.A. Simcoe, J.J. Matthee, D. Kashino, R. Mackenzie, I. Kramarenko, S.J. Lilly, A.-C. Eilers, R.P. Naidu, M. Yue, The Astrophysical Journal 999 (2026).","mla":"Higginson, Jack, et al. “EIGER. VIII. First Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch of Reionization.” <i>The Astrophysical Journal</i>, vol. 999, no. 1, 49, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae3e81\">10.3847/1538-4357/ae3e81</a>.","apa":"Higginson, J., Bordoloi, R., Simcoe, R. A., Matthee, J. J., Kashino, D., Mackenzie, R., … Yue, M. (2026). EIGER. VIII. First stars signatures in the connection between O I absorption and galaxies in the epoch of reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae3e81\">https://doi.org/10.3847/1538-4357/ae3e81</a>","chicago":"Higginson, Jack, Rongmon Bordoloi, Robert A. Simcoe, Jorryt J Matthee, Daichi Kashino, Ruari Mackenzie, Ivan Kramarenko, et al. “EIGER. VIII. First Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch of Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae3e81\">https://doi.org/10.3847/1538-4357/ae3e81</a>.","ama":"Higginson J, Bordoloi R, Simcoe RA, et al. EIGER. VIII. First stars signatures in the connection between O I absorption and galaxies in the epoch of reionization. <i>The Astrophysical Journal</i>. 2026;999(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae3e81\">10.3847/1538-4357/ae3e81</a>","ista":"Higginson J, Bordoloi R, Simcoe RA, Matthee JJ, Kashino D, Mackenzie R, Kramarenko I, Lilly SJ, Eilers A-C, Naidu RP, Yue M. 2026. EIGER. VIII. First stars signatures in the connection between O I absorption and galaxies in the epoch of reionization. The Astrophysical Journal. 999(1), 49.","ieee":"J. Higginson <i>et al.</i>, “EIGER. VIII. First stars signatures in the connection between O I absorption and galaxies in the epoch of reionization,” <i>The Astrophysical Journal</i>, vol. 999, no. 1. IOP Publishing, 2026."},"scopus_import":"1"},{"status":"public","article_processing_charge":"Yes","supplementarymaterial":"yes","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-10-12T12:17:25Z","_id":"23117","article_type":"original","author":[{"first_name":"Daichi","full_name":"Kashino, Daichi","last_name":"Kashino"},{"first_name":"Simon J.","last_name":"Lilly","full_name":"Lilly, Simon J."},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"full_name":"Eilers, Anna-Christina","last_name":"Eilers","first_name":"Anna-Christina"},{"first_name":"Rongmon","full_name":"Bordoloi, Rongmon","last_name":"Bordoloi"},{"last_name":"Simcoe","full_name":"Simcoe, Robert A.","first_name":"Robert A."},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Minghao","last_name":"Yue","full_name":"Yue, Minghao"},{"last_name":"Liu","full_name":"Liu, Bin","first_name":"Bin"}],"type":"journal_article","issue":"2","acknowledgement":"We thank Enrico Garaldi, Rahul Kannan, Aaron Smith, and the THESAN team for providing us with their simulation data, and Norbert Pirzkal for helpful advice on our NIRCam observing program.\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 were taken under GTO program No. 1243. The specific observations analyzed can be accessed via doi:10.17909/6grb-j154.\r\n\r\nThe participation of S.J.L. as an Interdisciplinary Scientist in the JWST Flight Science Working Group 2002-2022 has been supported by the European Space Agency. His earlier involvement in the development of the JWST 1996–2001 was supported by the Canadian Space Agency.\r\n\r\nThis work is partially based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 084.A-0360(A), 084.A-0390(A), 086.A-0162(A), 086.A-0574(A), 087.A-0607(A), 089.A-0814(A), 093.A-0707(A), 098.B-0537(A), and 286.A-5025(A). Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit 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. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.\r\n\r\nThis work has been supported by JSPS KAKENHI grant No. JP21K13956 (D.K.). J.M. is supported by the European Union (ERC, AGENTS, 101076224).\r\n\r\nFacilities: JWST - James Webb Space Telescope (NIRCam), VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), Magellan:Baade - Magellan I Walter Baade Telescope (FIRE), Keck:I - KECK I Telescope (MOSFIRE), Keck:II - KECK II Telescope (ESI).\r\n\r\nSoftware: Python, numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), Astropy (Astropy Collaboration et al. 2013), Matplotlib (J. D. Hunter 2007), PypeIt (J. X. Prochaska et al. 2019).","intvolume":"       997","abstract":[{"lang":"eng","text":"We present a comprehensive analysis of the relationship between galaxies and the intergalactic medium (IGM) during the late stages of cosmic reionization, based on the complete JWST EIGER dataset. Using deep NIRCam 3.5 μm slitless spectroscopy, we construct a sample of 948 [O iii]λ5008-emitting galaxies with −21.4 ≲ MUV ≲ −17.2 spanning 5.33 < z < 6.97 along six quasar sight lines. We correlate these galaxies with Lyα and Lyβ transmission measured from high-resolution quasar spectra across multiple redshift intervals. We find clear redshift evolution in the correlation between galaxy density and transmission: it is suppressed in overdense regions at z < 5.50, while enhanced at 5.70 < z < 6.15. The intermediate range exhibits a transitional behavior. Cross-correlation measurements further reveal excess absorption within ∼8 cMpc of galaxies at low redshifts, and enhanced transmission at intermediate scales (∼5–20 cMpc) at z > 5.70. Statistical tests using mock catalogs with realistic galaxy clustering but no correlation with the transmission field confirm that the observed correlations are unlikely to arise by chance. The evolving signals can be explained by stronger absorption in overdense regions, combined with the competing influences of local radiation fields and the rising background radiation. While local radiation dominates ionization of the surrounding IGM at earlier times, the background becomes increasingly important, eventually surpassing the impact of nearby galaxies. These results support an inside-out progression of reionization, with ionized regions originating around clustered, star-forming galaxies and gradually extending into underdense regions."}],"file_date_updated":"2026-10-14T08:09:31Z","researchdata_availability":"no","OA_type":"gold","PlanS_conform":"1","month":"01","date_updated":"2026-10-14T08:12:05Z","date_published":"2026-01-28T00:00:00Z","quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"28","oa":1,"fulldoi":"https://doi.org/10.3847/1538-4357/ae2799","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"file":[{"access_level":"open_access","date_created":"2026-10-14T08:09:31Z","success":1,"file_name":"2026_AstrophysicalJour_Kashino.pdf","date_updated":"2026-10-14T08:09:31Z","file_size":11393255,"checksum":"c33405da323cac352c0d751f0fe6f021","creator":"dernst","relation":"main_file","file_id":"23138","content_type":"application/pdf"}],"scopus_import":"1","citation":{"chicago":"Kashino, Daichi, Simon J. Lilly, Jorryt J Matthee, Ruari Mackenzie, Anna-Christina Eilers, Rongmon Bordoloi, Robert A. Simcoe, Rohan P. Naidu, Minghao Yue, and Bin Liu. “EIGER. VII. The Evolving Relationship between Galaxies and the Intergalactic Medium in the Final Stages of Reionization.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae2799\">https://doi.org/10.3847/1538-4357/ae2799</a>.","ama":"Kashino D, Lilly SJ, Matthee JJ, et al. EIGER. VII. The evolving relationship between galaxies and the intergalactic medium in the final stages of reionization. <i>The Astrophysical Journal</i>. 2026;997(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae2799\">10.3847/1538-4357/ae2799</a>","ista":"Kashino D, Lilly SJ, Matthee JJ, Mackenzie R, Eilers A-C, Bordoloi R, Simcoe RA, Naidu RP, Yue M, Liu B. 2026. EIGER. VII. The evolving relationship between galaxies and the intergalactic medium in the final stages of reionization. The Astrophysical Journal. 997(2), 280.","ieee":"D. Kashino <i>et al.</i>, “EIGER. VII. The evolving relationship between galaxies and the intergalactic medium in the final stages of reionization,” <i>The Astrophysical Journal</i>, vol. 997, no. 2. IOP Publishing, 2026.","mla":"Kashino, Daichi, et al. “EIGER. VII. The Evolving Relationship between Galaxies and the Intergalactic Medium in the Final Stages of Reionization.” <i>The Astrophysical Journal</i>, vol. 997, no. 2, 280, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae2799\">10.3847/1538-4357/ae2799</a>.","apa":"Kashino, D., Lilly, S. J., Matthee, J. J., Mackenzie, R., Eilers, A.-C., Bordoloi, R., … Liu, B. (2026). EIGER. VII. The evolving relationship between galaxies and the intergalactic medium in the final stages of reionization. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae2799\">https://doi.org/10.3847/1538-4357/ae2799</a>","short":"D. Kashino, S.J. Lilly, J.J. Matthee, R. Mackenzie, A.-C. Eilers, R. Bordoloi, R.A. Simcoe, R.P. Naidu, M. Yue, B. Liu, The Astrophysical Journal 997 (2026)."},"oa_version":"Published Version","language":[{"iso":"eng"}],"volume":997,"year":"2026","publisher":"IOP Publishing","OA_place":"publisher","DOAJ_listed":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication":"The Astrophysical Journal","article_number":"280","publication_status":"published","das_tickbox":"0","title":"EIGER. VII. The evolving relationship between galaxies and the intergalactic medium in the final stages of reionization","external_id":{"arxiv":["2506.03121"]},"doi":"10.3847/1538-4357/ae2799","ddc":["520"],"has_accepted_license":"1","department":[{"_id":"JoMa"}],"arxiv":1},{"fulldoi":"https://doi.org/10.1038/s41550-026-02993-5","oa_version":"None","scopus_import":"1","citation":{"mla":"Li, Zihao, et al. “First-Star Imprints in a Metal-Poor Galaxy Overdensity near the End of Reionization.” <i>Nature Astronomy</i>, Springer Nature, 2026, doi:<a href=\"https://doi.org/10.1038/s41550-026-02993-5\">10.1038/s41550-026-02993-5</a>.","apa":"Li, Z., Kakiichi, K., Christensen, L., Cai, Z., D’Odorico, V., Matthee, J. J., … Zhu, Y. (2026). First-star imprints in a metal-poor galaxy overdensity near the end of reionization. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-026-02993-5\">https://doi.org/10.1038/s41550-026-02993-5</a>","short":"Z. Li, K. Kakiichi, L. Christensen, Z. Cai, V. D’Odorico, J.J. Matthee, D. Kashino, R. Bordoloi, R. Mackenzie, T.A.M. Berg, I. Vanni, S. Salvadori, A. Venditti, S. Zhang, S.E.I. Bosman, E. Bañados, F.B. Davies, X. Fan, H.D. Jun, X. Jin, M. Li, S. Rojas-Ruiz, F. Wang, J. Yang, S. Zou, H. Zhang, Y. Zhu, Nature Astronomy (2026).","chicago":"Li, Zihao, Koki Kakiichi, Lise Christensen, Zheng Cai, Valentina D’Odorico, Jorryt J Matthee, Daichi Kashino, et al. “First-Star Imprints in a Metal-Poor Galaxy Overdensity near the End of Reionization.” <i>Nature Astronomy</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41550-026-02993-5\">https://doi.org/10.1038/s41550-026-02993-5</a>.","ama":"Li Z, Kakiichi K, Christensen L, et al. First-star imprints in a metal-poor galaxy overdensity near the end of reionization. <i>Nature Astronomy</i>. 2026. doi:<a href=\"https://doi.org/10.1038/s41550-026-02993-5\">10.1038/s41550-026-02993-5</a>","ieee":"Z. Li <i>et al.</i>, “First-star imprints in a metal-poor galaxy overdensity near the end of reionization,” <i>Nature Astronomy</i>. Springer Nature, 2026.","ista":"Li Z, Kakiichi K, Christensen L, Cai Z, D’Odorico V, Matthee JJ, Kashino D, Bordoloi R, Mackenzie R, Berg TAM, Vanni I, Salvadori S, Venditti A, Zhang S, Bosman SEI, Bañados E, Davies FB, Fan X, Jun HD, Jin X, Li M, Rojas-Ruiz S, Wang F, Yang J, Zou S, Zhang H, Zhu Y. 2026. First-star imprints in a metal-poor galaxy overdensity near the end of reionization. Nature Astronomy."},"language":[{"iso":"eng"}],"publisher":"Springer Nature","year":"2026","publication_identifier":{"eissn":["2397-3366"]},"publication":"Nature Astronomy","title":"First-star imprints in a metal-poor galaxy overdensity near the end of reionization","das_tickbox":"1","publication_status":"epub_ahead","doi":"10.1038/s41550-026-02993-5","department":[{"_id":"JoMa"}],"status":"public","supplementarymaterial":"yes","article_processing_charge":"No","date_created":"2026-10-11T22:02:07Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"23096","article_type":"original","author":[{"full_name":"Li, Zihao","last_name":"Li","first_name":"Zihao"},{"first_name":"Koki","full_name":"Kakiichi, Koki","last_name":"Kakiichi"},{"first_name":"Lise","full_name":"Christensen, Lise","last_name":"Christensen"},{"first_name":"Zheng","last_name":"Cai","full_name":"Cai, Zheng"},{"last_name":"D’Odorico","full_name":"D’Odorico, Valentina","first_name":"Valentina"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"first_name":"Rongmon","full_name":"Bordoloi, Rongmon","last_name":"Bordoloi"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"first_name":"Trystyn A.M.","full_name":"Berg, Trystyn A.M.","last_name":"Berg"},{"first_name":"Irene","last_name":"Vanni","full_name":"Vanni, Irene"},{"full_name":"Salvadori, Stefania","last_name":"Salvadori","first_name":"Stefania"},{"first_name":"Alessandra","full_name":"Venditti, Alessandra","last_name":"Venditti"},{"last_name":"Zhang","full_name":"Zhang, Shiwu","first_name":"Shiwu"},{"first_name":"Sarah E.I.","full_name":"Bosman, Sarah E.I.","last_name":"Bosman"},{"first_name":"Eduardo","full_name":"Bañados, Eduardo","last_name":"Bañados"},{"first_name":"Frederick B.","full_name":"Davies, Frederick B.","last_name":"Davies"},{"last_name":"Fan","full_name":"Fan, Xiaohui","first_name":"Xiaohui"},{"first_name":"Hyunsung D.","last_name":"Jun","full_name":"Jun, Hyunsung D."},{"full_name":"Jin, Xiangyu","last_name":"Jin","first_name":"Xiangyu"},{"full_name":"Li, Mingyu","last_name":"Li","first_name":"Mingyu"},{"first_name":"Sofía","full_name":"Rojas-Ruiz, Sofía","last_name":"Rojas-Ruiz"},{"full_name":"Wang, Feige","last_name":"Wang","first_name":"Feige"},{"first_name":"Jinyi","full_name":"Yang, Jinyi","last_name":"Yang"},{"first_name":"Siwei","full_name":"Zou, Siwei","last_name":"Zou"},{"full_name":"Zhang, Huanian","last_name":"Zhang","first_name":"Huanian"},{"last_name":"Zhu","full_name":"Zhu, Yongda","first_name":"Yongda"}],"type":"journal_article","abstract":[{"lang":"eng","text":"The first generation of stars, known as population III (Pop III), formed from primordial gas consisting solely of hydrogen and helium and is believed to have emerged only a few hundred million years after the Big Bang. Detecting the chemical enrichment of metal-poor circumgalactic gas offers a promising way to trace the enrichment signature of Pop III stars. Along the sight line to the quasar SDSS J0100+2802, a metal absorber at z = 5.945, showing over-abundant carbon and silicon compared with solar, has been reported to be consistent with the enrichment pattern of Pop III stars. Here, using data recorded by the James Webb Space Telescope, we report the discovery of an unusually metal-poor galaxy overdensity of 17 members (mean metallicity ~3% of solar) near this metal absorber, which is ~0.4 dex more metal-poor than coeval galaxies in similarly overdense environments. This less chemically evolved system may have provided favourable conditions for preserving the absorption signatures of Pop III enrichment. We infer a minimum dark matter halo mass of log(Mh,min/M⊙) = 10.68+0.93 −1.72, supporting late-time Pop III formation at the outskirts of atomic hydrogen cooling haloes. Our findings open a promising observational pathway to identifying the chemical imprints of the first stars and constrain the conditions for their formation."}],"acknowledgement":"This work is based on observations made with the NASA/ESA/CSA JWST, associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope, associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and 096.A-0095. We acknowledge the University of Copenhagen for giving this project access to the LUMI supercomputer owned by the EuroHPC Joint Undertaking and hosted by CSC (Finland) and the LUMI consortium through Denmark. Z.L. thanks Y. Ren for helpful discussions. We thank O. Zier, A. Smith, R. Kannan and E. Garaldi for helpful discussions about the THESAN-ZOOM simulation. Z.L. acknowledges the fellowship from the Cosmic Dawn Center, which is funded by the Danish National Research Foundation under grant no. 140. K.K. acknowledges support from the Villum Foundation (71574). L.C. is supported by DFF/Independent Research Fund Denmark (2032-00071). V.D. acknowledges financial support from the Bando Ricerca Fondamentale INAF 2022 Large Grant XQR-30. A.V. acknowledges funding from the Cosmic Frontier Center and the University of Texas at Austin’s College of Natural Sciences. S. Zou acknowledges support from the Chinese Academy of Sciences (E5295401).","researchdata_availability":"yes","dataavailabilitystatement":"This work is based on observations made with the NASA/ESA/CSA JWST, associated with the programmes GO-1243 and GO-2078, and the Very Large Telescope associated with ESO programmes X-shooter 0100.A-0625, 0102.A-0154, 1103.A-0817 and 096.A-0095. The JWST data are available via the Mikulski Archive for Space Telescopes at http://archive.stsci.edu under JWST programmes GO-2078 (ref. 127) and GO-1243 (ref. 128). The metal absorber catalogue of XQR-30 is available via GitHub at https://github.com/XQR-30/Metal-catalogue. The [O III] emitter catalogue from the EIGER survey is available via GitHub at https://eiger-jwst.github.io/data.html. Other data presented in this paper are available upon request to the corresponding author.","OA_type":"closed access","month":"09","date_updated":"2026-10-14T06:42:17Z","date_published":"2026-09-29T00:00:00Z","day":"29","quality_controlled":"1"},{"year":"2025","publisher":"Taylor & Francis","OA_place":"repository","citation":{"apa":"Matthee, J. J. (2025). JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. <i>Contemporary Physics</i>. Taylor &#38; Francis. <a href=\"https://doi.org/10.1080/00107514.2025.2586370\">https://doi.org/10.1080/00107514.2025.2586370</a>","mla":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” <i>Contemporary Physics</i>, vol. 66, no. 1–4, Taylor &#38; Francis, 2025, pp. 116–51, doi:<a href=\"https://doi.org/10.1080/00107514.2025.2586370\">10.1080/00107514.2025.2586370</a>.","short":"J.J. Matthee, Contemporary Physics 66 (2025) 116–151.","ista":"Matthee JJ. 2025. JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. Contemporary Physics. 66(1–4), 116–151.","ieee":"J. J. Matthee, “JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies,” <i>Contemporary Physics</i>, vol. 66, no. 1–4. Taylor &#38; Francis, pp. 116–151, 2025.","ama":"Matthee JJ. JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. <i>Contemporary Physics</i>. 2025;66(1-4):116-151. doi:<a href=\"https://doi.org/10.1080/00107514.2025.2586370\">10.1080/00107514.2025.2586370</a>","chicago":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” <i>Contemporary Physics</i>. Taylor &#38; Francis, 2025. <a href=\"https://doi.org/10.1080/00107514.2025.2586370\">https://doi.org/10.1080/00107514.2025.2586370</a>."},"scopus_import":"1","oa_version":"Preprint","fulldoi":"https://doi.org/10.1080/00107514.2025.2586370","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2511.04843","open_access":"1"}],"volume":66,"language":[{"iso":"eng"}],"doi":"10.1080/00107514.2025.2586370","arxiv":1,"department":[{"_id":"JoMa"}],"publication":"Contemporary Physics","publication_identifier":{"eissn":["1366-5812"],"issn":["0010-7514"]},"external_id":{"arxiv":["2511.04843"]},"publication_status":"published","title":"JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"}],"page":"116-151","article_type":"original","corr_author":"1","type":"journal_article","issue":"1-4","article_processing_charge":"No","status":"public","_id":"20864","date_created":"2025-12-29T12:05:25Z","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","date_updated":"2026-04-07T08:44:00Z","month":"12","quality_controlled":"1","day":"04","oa":1,"date_published":"2025-12-04T00:00:00Z","acknowledgement":"I thank Claudia Di Cesare, Edoardo Iani, Gauri Kotiwale and Wendy Sun for proofreading, Daichi Kashino, Gauri Kotiwale, Sara Mascia, Benjamín Navarette and Joris Witstok for their assistance in preparing some of the Figures, and Richard Ellis and Stephen Blundell for constructive comments. Funded by the European Union (ERC, AGENTS, 101076224).","intvolume":"        66","abstract":[{"lang":"eng","text":"Studies of the distant Universe are providing key insights into our understanding of the formation of galaxies. The advent of the James Webb Space Telescope (JWST) has significantly enhanced our observational capabilities, leading to an expanded redshift frontier, providing unprecedented detail in the characterisation of early galaxies and enabling the discovery of new populations of accreting black holes. This review aims to provide an introduction to the basic processes and components that shape the observed spectra of galaxies, with a focus on their relevance to techniques with which high-redshift galaxies are selected. The review further introduces specific topics that have attracted significant attention in recent literature, including the discovery of highly efficient galaxy formation in the early Universe, the relation between galaxies and the process of reionization, new insights into the formation of the first stars and the enrichment of interstellar gas with heavy elements, and breakthroughs in our understanding of the origins of supermassive black holes."}],"OA_type":"green"},{"date_updated":"2026-02-16T12:14:52Z","PlanS_conform":"1","month":"12","oa":1,"day":"01","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","date_published":"2025-12-01T00:00:00Z","file_date_updated":"2026-01-05T09:26:17Z","abstract":[{"text":"Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial for understanding the properties of cosmic reionizers because the opacity of the intergalactic medium (IGM) prevents the direct detection of LyC emission from sources during the Epoch of Reionization (EoR). In this study, we confirm two new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03 and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively. These two LyC candidate leakers were detected in a catalog of 91 spectroscopically confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed properties that were proposed as indirect indicators of LyC emission, such as Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according to these properties, stacked the LyC observations of this subsample, and assessed the limits of the escape fractions in the stacks. We aim to enhance our understanding of LyC escape mechanisms and improve our predictions of the LyC fesc during the EoR by analyzing the individual candidates and the stacks in the context of the currently limited sample of known LyC leakers at z ∼ 3.","lang":"eng"}],"intvolume":"       704","acknowledgement":"We acknowledge support from the National Science Foundation of China – 12225301, INAF Large grant “Spectroscopic survey with JWST” jand from PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and Postgraduate Scholarship Program under the grant of China Scholarship Council. P.W. and B.V. acknowledge support from the INAF Mini Grant ‘1.05.24.07.01 RSN1: Spatially Resolved Near-IR Emission of Intermediate-Redshift Jellyfish Galaxies’ (PI Watson). We acknowledge A. Acebron, C. Grillo, and P. Rosati for their fundamental contribution to the strong lensing analysis and results. We also extend our gratitude to the JWST and HST teams for their efforts in designing, building, and operating these transformative missions.","OA_type":"diamond","author":[{"last_name":"Liu","full_name":"Liu, Y.","first_name":"Y."},{"last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"first_name":"L.","full_name":"Pentericci, L.","last_name":"Pentericci"},{"first_name":"P.","last_name":"Watson","full_name":"Watson, P."},{"full_name":"Alavi, A.","last_name":"Alavi","first_name":"A."},{"full_name":"Bergamini, P.","last_name":"Bergamini","first_name":"P."},{"first_name":"M.","last_name":"Bradač","full_name":"Bradač, M."},{"first_name":"A.","full_name":"Calabrò, A.","last_name":"Calabrò"},{"last_name":"Glazebrook","full_name":"Glazebrook, K.","first_name":"K."},{"first_name":"A.","full_name":"Henry, A.","last_name":"Henry"},{"first_name":"M.","last_name":"Llerena","full_name":"Llerena, M."},{"full_name":"Merlin, E.","last_name":"Merlin","first_name":"E."},{"first_name":"B.","last_name":"Metha","full_name":"Metha, B."},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"first_name":"L.","full_name":"Napolitano, L.","last_name":"Napolitano"},{"first_name":"N.","last_name":"Roy","full_name":"Roy, N."},{"first_name":"B.","full_name":"Siana, B.","last_name":"Siana"},{"last_name":"Vanzella","full_name":"Vanzella, E.","first_name":"E."},{"first_name":"B.","last_name":"Vulcani","full_name":"Vulcani, B."},{"last_name":"Wang","full_name":"Wang, X.","first_name":"X."}],"article_type":"original","type":"journal_article","article_processing_charge":"No","status":"public","_id":"20932","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-01-04T23:01:35Z","has_accepted_license":"1","ddc":["520"],"doi":"10.1051/0004-6361/202556410","arxiv":1,"department":[{"_id":"JoMa"}],"article_number":"A328","publication":"Astronomy & Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"external_id":{"arxiv":["2507.11045"]},"title":"A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field","publication_status":"published","publisher":"EDP Sciences","year":"2025","DOAJ_listed":"1","OA_place":"publisher","citation":{"ama":"Liu Y, Mascia S, Pentericci L, et al. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>. 2025;704. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556410\">10.1051/0004-6361/202556410</a>","chicago":"Liu, Y., Sara Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202556410\">https://doi.org/10.1051/0004-6361/202556410</a>.","ista":"Liu Y, Mascia S, Pentericci L, Watson P, Alavi A, Bergamini P, Bradač M, Calabrò A, Glazebrook K, Henry A, Llerena M, Merlin E, Metha B, Nanayakkara T, Napolitano L, Roy N, Siana B, Vanzella E, Vulcani B, Wang X. 2025. A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy &#38; Astrophysics. 704, A328.","ieee":"Y. Liu <i>et al.</i>, “A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field,” <i>Astronomy &#38; Astrophysics</i>, vol. 704. EDP Sciences, 2025.","short":"Y. Liu, S. Mascia, L. Pentericci, P. Watson, A. Alavi, P. Bergamini, M. Bradač, A. Calabrò, K. Glazebrook, A. Henry, M. Llerena, E. Merlin, B. Metha, T. Nanayakkara, L. Napolitano, N. Roy, B. Siana, E. Vanzella, B. Vulcani, X. Wang, Astronomy &#38; Astrophysics 704 (2025).","mla":"Liu, Y., et al. “A Lyman Continuum Analysis of ∼100 Galaxies at z Spec∼ 3 in the Abell 2744 Cluster Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 704, A328, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556410\">10.1051/0004-6361/202556410</a>.","apa":"Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P., … Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556410\">https://doi.org/10.1051/0004-6361/202556410</a>"},"scopus_import":"1","oa_version":"Published Version","file":[{"checksum":"3e6061f3c4bfb521b3333ea4913c241a","file_size":4642530,"date_updated":"2026-01-05T09:26:17Z","file_name":"2025_AstronomyAstrophysics_Liu.pdf","content_type":"application/pdf","file_id":"20938","relation":"main_file","creator":"dernst","access_level":"open_access","success":1,"date_created":"2026-01-05T09:26:17Z"}],"fulldoi":"https://doi.org/10.1051/0004-6361/202556410","volume":704,"language":[{"iso":"eng"}]},{"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","day":"09","oa":1,"date_published":"2025-12-09T00:00:00Z","date_updated":"2026-02-09T06:41:48Z","month":"12","PlanS_conform":"1","OA_type":"gold","intvolume":"       995","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.","file_date_updated":"2026-02-09T06:39:23Z","abstract":[{"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.","lang":"eng"}],"issue":"1","type":"journal_article","author":[{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"de Graaff","full_name":"de Graaff, Anna","first_name":"Anna"},{"full_name":"Ma, Yilun 逸伦","last_name":"Ma","first_name":"Yilun 逸伦"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Rachel","full_name":"Bezanson, Rachel","last_name":"Bezanson"},{"first_name":"Leindert A.","full_name":"Boogaard, Leindert A.","last_name":"Boogaard"},{"first_name":"Nikko J.","last_name":"Cleri","full_name":"Cleri, Nikko J."},{"first_name":"Harley","last_name":"Katz","full_name":"Katz, Harley"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"last_name":"Maseda","full_name":"Maseda, Michael V.","first_name":"Michael V."},{"first_name":"Ian","last_name":"McConachie","full_name":"McConachie, Ian"},{"full_name":"Miller, Tim B.","last_name":"Miller","first_name":"Tim B."},{"full_name":"Price, Sedona H.","last_name":"Price","first_name":"Sedona H."},{"first_name":"Katherine A.","full_name":"Suess, Katherine A.","last_name":"Suess"},{"last_name":"van Dokkum","full_name":"van Dokkum, Pieter","first_name":"Pieter"},{"first_name":"Bingjie 冰洁","last_name":"Wang 王","full_name":"Wang 王, Bingjie 冰洁"},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."}],"article_type":"original","_id":"21057","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-01-28T15:21:47Z","article_processing_charge":"Yes","status":"public","arxiv":1,"department":[{"_id":"JoMa"}],"has_accepted_license":"1","doi":"10.3847/1538-4357/ae1500","ddc":["520"],"external_id":{"arxiv":["2411.03424"]},"publication_status":"published","title":"Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication":"The Astrophysical Journal","article_number":"118","DOAJ_listed":"1","OA_place":"publisher","year":"2025","publisher":"IOP Publishing","volume":995,"language":[{"iso":"eng"}],"oa_version":"Published Version","citation":{"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>","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>.","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.","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>","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>."},"scopus_import":"1","fulldoi":"https://doi.org/10.3847/1538-4357/ae1500","file":[{"date_updated":"2026-02-09T06:39:23Z","file_name":"2025_AstrophysicalJournal_Setton.pdf","checksum":"2a424eb43748a6370ff058c98adb15c6","file_size":1989640,"relation":"main_file","creator":"dernst","file_id":"21163","content_type":"application/pdf","access_level":"open_access","date_created":"2026-02-09T06:39:23Z","success":1}]},{"oa":1,"quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"12","date_published":"2025-09-12T00:00:00Z","date_updated":"2026-02-09T07:14:08Z","PlanS_conform":"1","month":"09","OA_type":"gold","file_date_updated":"2026-02-09T07:10:29Z","abstract":[{"lang":"eng","text":"Luminous broad Hα emission and red rest-optical spectral energy distributions (SEDs) are the hallmark of compact little red dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei (AGN). However, the lack of observed far-infrared (FIR) emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new Atacama Large Millimeter/submillimeter Array imaging, new and existing JWST/MIRI imaging, and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs (z = 3.1 and z = 4.47) to place the strongest constraints on the IR luminosity in LRDs to date. The detections at λrest = 1–4 μm imply flat slopes in the rest-IR, ruling out a contribution from hot (T ≳ 500 K) dust. Similarly, FIR nondetections rule out any appreciable cold (T ≲ 75 K) dust component. Assuming energy balance, these observations are inconsistent with the typical FIR dust emission of dusty starbursts and quasar tori, which usually show a mixture of cold and hot dust. Additionally, our [C ii] nondetections rule out typical dusty starbursts. We compute empirical maximum IR SEDs and find that both LRDs must have log(LIR/L ) 12.2 at the 3σ level. These limits are in tension with the predictions of rest-optical spectrophotometric fits, be they galaxy-only, AGN-only, or composite. It is unlikely that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature distribution that conspires to avoid current observing facilities. Rather, we favor an intrinsically redder LRD SED model that alleviates the need for strong dust attenuation."}],"intvolume":"       991","acknowledgement":"Support for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. D.S. acknowledges Zhengrong Li for kindly sharing model dust SEDs, Tim Rawle for helping with accessing archival Herschel Lensing Survey data, and Xiaohui Fan for helpful conversations that steered the direction of this work. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2024.00826.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. 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 (DOI: 10.17909/m7ks-wg55), 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 #6761.\r\n\r\nSupport for this work was provided by NSF/AAG #2306950. 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, Inc., under NASA contract NAS5-26555. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant DNRF140. 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. The work 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. S.A. acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University of Arizona.","type":"journal_article","author":[{"last_name":"Setton","full_name":"Setton, David J.","first_name":"David J."},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"first_name":"Justin S.","last_name":"Spilker","full_name":"Spilker, Justin S."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."},{"first_name":"Ivo","full_name":"Labbé, Ivo","last_name":"Labbé"},{"first_name":"Yilun 逸伦","full_name":"Ma, Yilun 逸伦","last_name":"Ma"},{"first_name":"Bingjie 冰洁","last_name":"Wang","full_name":"Wang, Bingjie 冰洁"},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"first_name":"Anna","full_name":"de Graaff, Anna","last_name":"de Graaff"},{"first_name":"Stacey","full_name":"Alberts, Stacey","last_name":"Alberts"},{"first_name":"Rachel","full_name":"Bezanson, Rachel","last_name":"Bezanson"},{"first_name":"Leindert A.","full_name":"Boogaard, Leindert A.","last_name":"Boogaard"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"first_name":"Sam E.","last_name":"Cutler","full_name":"Cutler, Sam E."},{"full_name":"Cleri, Nikko J.","last_name":"Cleri","first_name":"Nikko J."},{"last_name":"Cooper","full_name":"Cooper, Olivia R.","first_name":"Olivia R."},{"first_name":"Pratika","last_name":"Dayal","full_name":"Dayal, Pratika"},{"full_name":"Fujimoto, Seiji","last_name":"Fujimoto","first_name":"Seiji"},{"first_name":"Lukas J.","full_name":"Furtak, Lukas J.","last_name":"Furtak"},{"first_name":"Andy D.","full_name":"Goulding, Andy D.","last_name":"Goulding"},{"first_name":"Michaela","last_name":"Hirschmann","full_name":"Hirschmann, Michaela"},{"first_name":"Vasily","full_name":"Kokorev, Vasily","last_name":"Kokorev"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"full_name":"McConachie, Ian","last_name":"McConachie","first_name":"Ian"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Miller, Tim B.","last_name":"Miller","first_name":"Tim B."},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"first_name":"Richard","full_name":"Pan, Richard","last_name":"Pan"},{"last_name":"Price","full_name":"Price, Sedona H.","first_name":"Sedona H."},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"first_name":"John R.","full_name":"Weaver, John R.","last_name":"Weaver"},{"full_name":"Xiao, Mengyuan","last_name":"Xiao","first_name":"Mengyuan"},{"first_name":"Yunchong","full_name":"Zhang, Yunchong","last_name":"Zhang"},{"last_name":"Zitrin","full_name":"Zitrin, Adi","first_name":"Adi"}],"article_type":"original","_id":"21058","date_created":"2026-01-28T15:23:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"Yes","status":"public","arxiv":1,"department":[{"_id":"JoMa"}],"has_accepted_license":"1","ddc":["520"],"doi":"10.3847/2041-8213/ade78b","external_id":{"arxiv":["2503.02059"]},"title":"A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots","publication_status":"published","article_number":"L10","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"publication":"The Astrophysical Journal Letters","DOAJ_listed":"1","OA_place":"publisher","publisher":"IOP Publishing","year":"2025","volume":991,"language":[{"iso":"eng"}],"scopus_import":"1","citation":{"apa":"Setton, D. J., Greene, J. E., Spilker, J. S., Williams, C. C., Labbé, I., Ma, Y. 逸伦, … Zitrin, A. (2025). A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ade78b\">https://doi.org/10.3847/2041-8213/ade78b</a>","mla":"Setton, David J., et al. “A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots.” <i>The Astrophysical Journal Letters</i>, vol. 991, L10, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ade78b\">10.3847/2041-8213/ade78b</a>.","short":"D.J. Setton, J.E. Greene, J.S. Spilker, C.C. Williams, I. Labbé, Y.逸伦 Ma, B.冰洁 Wang, K.E. Whitaker, J. Leja, A. de Graaff, S. Alberts, R. Bezanson, L.A. Boogaard, G. Brammer, S.E. Cutler, N.J. Cleri, O.R. Cooper, P. Dayal, S. Fujimoto, L.J. Furtak, A.D. Goulding, M. Hirschmann, V. Kokorev, M.V. Maseda, I. McConachie, J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, R. Pan, S.H. Price, K.A. Suess, J.R. Weaver, M. Xiao, Y. Zhang, A. Zitrin, The Astrophysical Journal Letters 991 (2025).","ieee":"D. J. Setton <i>et al.</i>, “A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots,” <i>The Astrophysical Journal Letters</i>, vol. 991. IOP Publishing, 2025.","ista":"Setton DJ, Greene JE, Spilker JS, Williams CC, Labbé I, Ma Y逸伦, Wang B冰洁, Whitaker KE, Leja J, de Graaff A, Alberts S, Bezanson R, Boogaard LA, Brammer G, Cutler SE, Cleri NJ, Cooper OR, Dayal P, Fujimoto S, Furtak LJ, Goulding AD, Hirschmann M, Kokorev V, Maseda MV, McConachie I, Matthee JJ, Miller TB, Naidu RP, Oesch PA, Pan R, Price SH, Suess KA, Weaver JR, Xiao M, Zhang Y, Zitrin A. 2025. A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. The Astrophysical Journal Letters. 991, L10.","chicago":"Setton, David J., Jenny E. Greene, Justin S. Spilker, Christina C. Williams, Ivo Labbé, Yilun 逸伦 Ma, Bingjie 冰洁 Wang, et al. “A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ade78b\">https://doi.org/10.3847/2041-8213/ade78b</a>.","ama":"Setton DJ, Greene JE, Spilker JS, et al. A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots. <i>The Astrophysical Journal Letters</i>. 2025;991. doi:<a href=\"https://doi.org/10.3847/2041-8213/ade78b\">10.3847/2041-8213/ade78b</a>"},"oa_version":"Published Version","file":[{"access_level":"open_access","date_created":"2026-02-09T07:10:29Z","success":1,"file_size":1394204,"checksum":"799518db92ded4e166df4234195af998","file_name":"2025_AstrophysicalJournalLetters_Setton.pdf","date_updated":"2026-02-09T07:10:29Z","relation":"main_file","creator":"dernst","content_type":"application/pdf","file_id":"21165"}],"fulldoi":"https://doi.org/10.3847/2041-8213/ade78b"},{"type":"journal_article","corr_author":"1","article_type":"original","author":[{"first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia"},{"full_name":"Pentericci, L.","last_name":"Pentericci","first_name":"L."},{"first_name":"M.","last_name":"Llerena","full_name":"Llerena, M."},{"first_name":"A.","last_name":"Calabrò","full_name":"Calabrò, A."},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"last_name":"Flury","full_name":"Flury, S.","first_name":"S."},{"last_name":"Pacucci","full_name":"Pacucci, F.","first_name":"F."},{"first_name":"A.","last_name":"Jaskot","full_name":"Jaskot, A."},{"last_name":"Amorín","full_name":"Amorín, R. O.","first_name":"R. O."},{"last_name":"Bhatawdekar","full_name":"Bhatawdekar, R.","first_name":"R."},{"last_name":"Castellano","full_name":"Castellano, M.","first_name":"M."},{"first_name":"N.","last_name":"Cleri","full_name":"Cleri, N."},{"last_name":"Costantin","full_name":"Costantin, L.","first_name":"L."},{"first_name":"K.","last_name":"Davis","full_name":"Davis, K."},{"first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare"},{"first_name":"M.","full_name":"Dickinson, M.","last_name":"Dickinson"},{"full_name":"Fontana, A.","last_name":"Fontana","first_name":"A."},{"first_name":"Y.","full_name":"Guo, Y.","last_name":"Guo"},{"first_name":"M.","last_name":"Giavalisco","full_name":"Giavalisco, M."},{"first_name":"B. W.","full_name":"Holwerda, B. W.","last_name":"Holwerda"},{"first_name":"W.","last_name":"Hu","full_name":"Hu, W."},{"last_name":"Huertas-Company","full_name":"Huertas-Company, M.","first_name":"M."},{"last_name":"Jung","full_name":"Jung, Intae","first_name":"Intae"},{"first_name":"J.","full_name":"Kartaltepe, J.","last_name":"Kartaltepe"},{"full_name":"Kashino, D.","last_name":"Kashino","first_name":"D."},{"full_name":"Koekemoer, A. M.","last_name":"Koekemoer","first_name":"A. M."},{"first_name":"R. A.","full_name":"Lucas, R. A.","last_name":"Lucas"},{"first_name":"J.","last_name":"Lotz","full_name":"Lotz, J."},{"first_name":"L.","last_name":"Napolitano","full_name":"Napolitano, L."},{"full_name":"Jogee, S.","last_name":"Jogee","first_name":"S."},{"first_name":"S.","full_name":"Wilkins, S.","last_name":"Wilkins"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-01-28T15:24:24Z","_id":"21060","status":"public","article_processing_charge":"No","date_published":"2025-09-01T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","day":"01","oa":1,"PlanS_conform":"1","month":"09","date_updated":"2026-02-09T07:33:46Z","OA_type":"diamond","acknowledgement":"This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GTO 1243, ERS 1345, DDT 2750, and GTO 1180, 1181, 3215, 1210, 1286. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge support from the INAF Large Grant 2022 “Extragalactic Surveys with JWST” (PI Pentericci). We acknowledge support from INAF Mini-grant “Reionization and Fundamental Cosmology with High-Redshift Galaxies” and from PRIN 2022 MUR project 2022CB3PJ3 - First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU. RA acknowledges support of Grant PID2023-147386NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU, and the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/10.13039/50110001103. The project that gave rise to these results received the support of a fellowship from the “la Caixa” Foundation (ID 100010434). The fellowship code is LCF/BQ/PR24/12050015. LC acknowledges support from grants PID2022-139567NB-I00 and PIB2021-127718NB-I00 funded by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by “ERDF A way of making Europe”.","intvolume":"       701","file_date_updated":"2026-02-09T07:28:08Z","abstract":[{"text":"Compact, star-forming galaxies with high star formation rate surface densities (ΣSFR) are often efficient Lyman continuum (LyC) emitters at z ≤ 4.5, likely because intense stellar feedback creates low-density channels that allow photons to escape. Irregular or disturbed morphologies, such as those resulting from mergers, can also facilitate LyC escape by creating anisotropic gas distributions. We investigated the influence of galaxy morphology on LyC production and escape at redshifts 5 ≤ z ≤ 7 using observations from various James Webb Space Telescope (JWST) surveys. Our sample consists of 436 sources, which are predominantly low-mass (∼10^8.15 M\f), star-forming galaxies with ionizing photon efficiency (ξion) values consistent with canonical expectations. Since direct measurements of fesc are not possible during the Epoch of  Reionization (EoR), we predicted fesc for high-redshift galaxies by applying survival analysis to a subsample of LyC emitters from the Low-Redshift Lyman Continuum Survey (LzLCS), selected to be direct analogs of reionization-era galaxies. We find that these galaxies exhibit, on average, modest predicted escape fractions (∼0.04). In addition, we evaluated the correlation between morphological features and LyC emission. Our findings indicate that neither ξion nor the predicted fesc values show a significant correlation with the presence of merger signatures. This suggests that in low-mass galaxies at z ≥ 5, strong morphological disturbances are not the primary mechanism driving LyC emission and leakage. Instead, compactness and star formation activity likely play a more pivotal role in regulating LyC escape. ","lang":"eng"}],"OA_place":"publisher","DOAJ_listed":"1","year":"2025","publisher":"EDP Sciences","language":[{"iso":"eng"}],"volume":701,"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"fulldoi":"https://doi.org/10.1051/0004-6361/202553760","file":[{"success":1,"date_created":"2026-02-09T07:28:08Z","access_level":"open_access","file_id":"21166","content_type":"application/pdf","creator":"dernst","relation":"main_file","file_name":"2025_AstronomyAstrophysics_Mascia.pdf","date_updated":"2026-02-09T07:28:08Z","file_size":9994234,"checksum":"990e384ca19e14b35296712d3b9e2919"}],"citation":{"short":"S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury, F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L. Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco, B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino, A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy &#38; Astrophysics 701 (2025).","mla":"Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 701, A122, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>.","apa":"Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury, S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>","chicago":"Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee, S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>.","ama":"Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>","ieee":"S. Mascia <i>et al.</i>, “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.","ista":"Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W, Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy &#38; Astrophysics. 701, A122."},"oa_version":"Published Version","scopus_import":"1","department":[{"_id":"JoMa"}],"arxiv":1,"doi":"10.1051/0004-6361/202553760","ddc":["520"],"has_accepted_license":"1","publication_status":"published","title":"Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe","external_id":{"arxiv":["2501.08268"]},"publication":"Astronomy & Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_number":"A122"},{"title":"GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7","publication_status":"published","article_number":"46","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication":"The Astrophysical Journal","department":[{"_id":"JoMa"}],"ddc":["520"],"doi":"10.3847/1538-4357/ade9a1","has_accepted_license":"1","language":[{"iso":"eng"}],"volume":989,"file":[{"checksum":"9e08e77ce6d818fafd074e2b6c30bc43","file_size":14405059,"file_name":"2025_AstrophysicalJournal_Fujimoto.pdf","date_updated":"2026-02-09T07:57:01Z","relation":"main_file","creator":"dernst","file_id":"21167","content_type":"application/pdf","access_level":"open_access","date_created":"2026-02-09T07:57:01Z","success":1}],"fulldoi":"https://doi.org/10.3847/1538-4357/ade9a1","oa_version":"Published Version","scopus_import":"1","citation":{"ieee":"S. Fujimoto <i>et al.</i>, “GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7,” <i>The Astrophysical Journal</i>, vol. 989. IOP Publishing, 2025.","ista":"Fujimoto S, Naidu RP, Chisholm J, Atek H, Endsley R, Kokorev V, Furtak LJ, Pan R, Liu B, Bromm V, Venditti A, Visbal E, Sarmento R, Weibel A, Oesch PA, Brammer G, Schaerer D, Adamo A, Berg DA, Bezanson R, Bouwens R, Chemerynska I, Claeyssens A, Dessauges-Zavadsky M, Frebel A, Korber D, Labbe I, Marques-Chaves R, Matthee JJ, McQuinn KBW, Muñoz JB, Natarajan P, Saldana-Lopez A, Suess KA, Volonteri M, Zitrin A. 2025. GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7. The Astrophysical Journal. 989, 46.","chicago":"Fujimoto, Seiji, Rohan P. Naidu, John Chisholm, Hakim Atek, Ryan Endsley, Vasily Kokorev, Lukas J. Furtak, et al. “GLIMPSE: An Ultrafaint ≃10^5 M⊙ Pop III Galaxy Candidate and First Constraints on the Pop III UV Luminosity Function at z ≃  6–7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade9a1\">https://doi.org/10.3847/1538-4357/ade9a1</a>.","ama":"Fujimoto S, Naidu RP, Chisholm J, et al. GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7. <i>The Astrophysical Journal</i>. 2025;989. doi:<a href=\"https://doi.org/10.3847/1538-4357/ade9a1\">10.3847/1538-4357/ade9a1</a>","apa":"Fujimoto, S., Naidu, R. P., Chisholm, J., Atek, H., Endsley, R., Kokorev, V., … Zitrin, A. (2025). GLIMPSE: An ultrafaint ≃10^5 M⊙ Pop III galaxy candidate and first constraints on the Pop III UV luminosity function at z ≃  6–7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade9a1\">https://doi.org/10.3847/1538-4357/ade9a1</a>","mla":"Fujimoto, Seiji, et al. “GLIMPSE: An Ultrafaint ≃10^5 M⊙ Pop III Galaxy Candidate and First Constraints on the Pop III UV Luminosity Function at z ≃  6–7.” <i>The Astrophysical Journal</i>, vol. 989, 46, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade9a1\">10.3847/1538-4357/ade9a1</a>.","short":"S. Fujimoto, R.P. Naidu, J. Chisholm, H. Atek, R. Endsley, V. Kokorev, L.J. Furtak, R. Pan, B. Liu, V. Bromm, A. Venditti, E. Visbal, R. Sarmento, A. Weibel, P.A. Oesch, G. Brammer, D. Schaerer, A. Adamo, D.A. Berg, R. Bezanson, R. Bouwens, I. Chemerynska, A. Claeyssens, M. Dessauges-Zavadsky, A. Frebel, D. Korber, I. Labbe, R. Marques-Chaves, J.J. Matthee, K.B.W. McQuinn, J.B. Muñoz, P. Natarajan, A. Saldana-Lopez, K.A. Suess, M. Volonteri, A. Zitrin, The Astrophysical Journal 989 (2025)."},"OA_place":"publisher","DOAJ_listed":"1","publisher":"IOP Publishing","year":"2025","OA_type":"gold","abstract":[{"text":"Detecting the first generation of stars, Population III (Pop III), has been a long-standing goal in astrophysics, yet they remain elusive even in the JWST era. Here we present a novel NIRCam-based selection method for Pop III galaxies, and carefully validate it through completeness and contamination simulations. We systematically search ≃ 500 arcmin2 across JWST legacy fields for Pop III candidates, including GLIMPSE, which, assisted by gravitational lensing, has produced JWST’s deepest NIRCam imaging thus far. We discover one promising Pop III galaxy candidate (GLIMPSE-16043) at z=6.50 -0.24 +0.03, a moderately lensed galaxy (µ = + 2.9 -0.2 +0.1) with an intrinsic UV magnitude of MUV= -15.89 -0.14 +0.12. It exhibits key Pop III features: strong Hα emission (rest-frame EW 2810 ± 550 Å); a Balmer jump; no dust (UV slope β = −2.34 ± 0.36); and undetectable metal lines (e.g., [O III]; [O III]/Hβ < 0.44), implying a gas-phase metallicity of Zgas/Z⊙ < 0.5%. These properties indicate the presence of a nascent, metal-deficient young stellar population (<5 Myr) with a stellar mass of ≃105 M⊙. Intriguingly, this source deviates significantly from the extrapolated UV–metallicity relation derived from recent JWST observations at z = 4–10, consistent with UV enhancement by a top-heavy Pop III initial mass function or the presence of an extremely metal-poor active galactic nucleus. We also  derive the first observational constraints on the Pop III UV luminosity function at z ≃ 6–7. The volume density of GLIMPSE-16043 (≈10^−4 cMpc−3) is in excellent agreement with theoretical predictions, independently reinforcing its plausibility. This study demonstrates the power of our novel NIRCam method to finally reveal distant galaxies even more pristine than the Milky Way’s most metal-poor satellites, thereby promising to bring us closer to the first generation of stars than we have ever been before.","lang":"eng"}],"file_date_updated":"2026-02-09T07:57:01Z","intvolume":"       989","acknowledgement":"We are grateful to the CEERS, PRIMER, JOF, UNCOVER, and GLIMPSE teams for developing their NIRCam surveys, and to the various JWST and HST surveys acknowledged in Section 3 that enabled our search. We thank Kimihiko Nakajima and Kohei Inayoshi for sharing Pop III and/or AGN templates, Steven Finkelstein for comments on the completeness and contamination rate simulation, Aaron Yung for SEDs of simulated galaxies, Joel Leja, Ben Johnson, and Sandro Tacchella for advise on SED fitting, and Takashi Kojima and Hiroto Yanagisawa for discussions.\r\n\r\nWe made extensive use of the DAWN JWST Archive for various comparisons presented in this paper. Some of the data products presented herein were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140. The prism spectra used in this paper were observed as part of the following programs, and we are grateful to these teams for helping build the rich spectroscopic legacy of JWST: 1180, 1181, 1210, 1286, 3215 (A. J. Bunker et al. 2024; F. D’Eugenio et al. 2024); 1211–1215 (M. V. Maseda et al. 2024); 1345 (S. L. Finkelstein et al. 2024); 1433 (T. Y.-Y. Hsiao et al. 2024); 1747 (G. Roberts-Borsani et al. 2025); 2028 (X. Wang et al. 2024); 2073 (PI: J. Hennawi); 2198 (L. Barrufet et al. 2025); 2282 (L. D. Bradley et al. 2023); 2561 (R. Bezanson et al. 2024; S. H. Price et al. 2024); 2565 (T. Nanayakkara et al. 2023); 2750 (P. Arrabal Haro et al. 2023b); 2756 (PI: W. Chen); 2767 (C. C. Williams et al. 2023); 3073 (M. Castellano et al. 2024); 4106 (PI: E. Nelson); 4233 (A. de Graaff et al. 2025); 4446 (B. L. Frye et al. 2024); 4557 (PI: H. Yan); 6541 (PI: E. Egami); 6585 (PI: D. Coulter).\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. The specific observations can be accessed via doi: 10.17909/xpxt-a441. These observations include data associated with program No. 03293. Support for program No. 03293 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.\r\n\r\nThis project has received funding from NASA through the NASA Hubble Fellowship grant HST-HF2-51505.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract 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. H.A. and I.C. acknowledge 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. I.C. acknowledges funding support from the Initiative Physique des Infinis (IPI), a research training program of the Idex SUPER at Sorbonne Université. 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. P.N. acknowledges support from the Gordon and Betty Moore Foundation and the John Templeton Foundation that fund the black hole Initiative (BHI) at Harvard University, where she serves as one of the PIs. B.L. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1—390900948 (the Heidelberg STRUCTURES Excellence Cluster). Y.S. and G.M. have received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 833925, project STAREX).","date_published":"2025-08-04T00:00:00Z","oa":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"04","quality_controlled":"1","month":"08","PlanS_conform":"1","date_updated":"2026-02-09T08:11:01Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-01-28T15:25:17Z","_id":"21061","status":"public","article_processing_charge":"Yes","type":"journal_article","article_type":"original","author":[{"last_name":"Fujimoto","full_name":"Fujimoto, Seiji","first_name":"Seiji"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Hakim","full_name":"Atek, Hakim","last_name":"Atek"},{"first_name":"Ryan","full_name":"Endsley, Ryan","last_name":"Endsley"},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"first_name":"Lukas J.","last_name":"Furtak","full_name":"Furtak, Lukas J."},{"full_name":"Pan, Richard","last_name":"Pan","first_name":"Richard"},{"last_name":"Liu","full_name":"Liu, Boyuan","first_name":"Boyuan"},{"last_name":"Bromm","full_name":"Bromm, Volker","first_name":"Volker"},{"full_name":"Venditti, Alessandra","last_name":"Venditti","first_name":"Alessandra"},{"full_name":"Visbal, Eli","last_name":"Visbal","first_name":"Eli"},{"full_name":"Sarmento, Richard","last_name":"Sarmento","first_name":"Richard"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"first_name":"Angela","last_name":"Adamo","full_name":"Adamo, Angela"},{"first_name":"Danielle A.","last_name":"Berg","full_name":"Berg, Danielle A."},{"full_name":"Bezanson, Rachel","last_name":"Bezanson","first_name":"Rachel"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"first_name":"Iryna","full_name":"Chemerynska, Iryna","last_name":"Chemerynska"},{"first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens"},{"first_name":"Miroslava","full_name":"Dessauges-Zavadsky, Miroslava","last_name":"Dessauges-Zavadsky"},{"last_name":"Frebel","full_name":"Frebel, Anna","first_name":"Anna"},{"full_name":"Korber, Damien","last_name":"Korber","first_name":"Damien"},{"last_name":"Labbe","full_name":"Labbe, Ivo","first_name":"Ivo"},{"first_name":"Rui","full_name":"Marques-Chaves, Rui","last_name":"Marques-Chaves"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Kristen B. W.","last_name":"McQuinn","full_name":"McQuinn, Kristen B. W."},{"full_name":"Muñoz, Julian B.","last_name":"Muñoz","first_name":"Julian B."},{"last_name":"Natarajan","full_name":"Natarajan, Priyamvada","first_name":"Priyamvada"},{"full_name":"Saldana-Lopez, Alberto","last_name":"Saldana-Lopez","first_name":"Alberto"},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"first_name":"Marta","full_name":"Volonteri, Marta","last_name":"Volonteri"},{"last_name":"Zitrin","full_name":"Zitrin, Adi","first_name":"Adi"}]},{"publication_status":"published","title":"Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5","external_id":{"arxiv":["2412.02846"]},"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication":"The Astrophysical Journal","article_number":"246","department":[{"_id":"JoMa"}],"arxiv":1,"doi":"10.3847/1538-4357/ade886","ddc":["520"],"has_accepted_license":"1","language":[{"iso":"eng"}],"volume":988,"fulldoi":"https://doi.org/10.3847/1538-4357/ade886","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"file":[{"success":1,"date_created":"2026-02-09T08:20:14Z","access_level":"open_access","content_type":"application/pdf","file_id":"21168","relation":"main_file","creator":"dernst","checksum":"a49fbed72f2ff9c0b13129acb6f44f9d","file_size":6237415,"date_updated":"2026-02-09T08:20:14Z","file_name":"2025_AstrophysicalJournal_Matthee.pdf"}],"citation":{"ieee":"J. J. Matthee <i>et al.</i>, “Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” <i>The Astrophysical Journal</i>, vol. 988, no. 2. IOP Publishing, 2025.","ista":"Matthee JJ, Naidu RP, Kotiwale G, Furtak LJ, Kramarenko I, Mackenzie R, Greene J, Adamo A, Bouwens RJ, Di Cesare C, Eilers A-C, de Graaff A, Heintz KE, Kashino D, Maseda MV, Tacchella S, Torralba Torregrosa A. 2025. Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. The Astrophysical Journal. 988(2), 246.","ama":"Matthee JJ, Naidu RP, Kotiwale G, et al. Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. 2025;988(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gauri Kotiwale, Lukas J. Furtak, Ivan Kramarenko, Ruari Mackenzie, Jenny Greene, et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>.","short":"J.J. Matthee, R.P. Naidu, G. Kotiwale, L.J. Furtak, I. Kramarenko, R. Mackenzie, J. Greene, A. Adamo, R.J. Bouwens, C. Di Cesare, A.-C. Eilers, A. de Graaff, K.E. Heintz, D. Kashino, M.V. Maseda, S. Tacchella, A. Torralba Torregrosa, The Astrophysical Journal 988 (2025).","apa":"Matthee, J. J., Naidu, R. P., Kotiwale, G., Furtak, L. J., Kramarenko, I., Mackenzie, R., … Torralba Torregrosa, A. (2025). Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>","mla":"Matthee, Jorryt J., et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>."},"oa_version":"Published Version","scopus_import":"1","OA_place":"publisher","DOAJ_listed":"1","year":"2025","publisher":"IOP Publishing","OA_type":"gold","acknowledgement":"We thank the referee for their constructive comments that helped to improve the paper. We thank Junyao Li for sharing model output shown in Figure 13, Rob Crain for sharing results from the ONLYAGN EAGLE model shown in Figure 15, and Adi Zitrin for comments. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge funding from JWST program GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS 5-26555. A.A. acknowledges support by the Swedish research council Vetenskapsrådet (2021-05559).","intvolume":"       988","file_date_updated":"2026-02-09T08:20:14Z","abstract":[{"text":"JWST observations have unveiled faint active galactic nuclei (AGNs) at high redshift that provide insights into the formation of supermassive black holes (SMBHs). However, disentangling their stellar from AGN light is challenging. Here, we use an empirical approach to infer the average stellar mass of five faint broad-line (BL) Hα emitters at z = 4–5 with BH masses ≈6 × 10^6 M⊙, with a method independent of their spectral energy distribution (SED). We use the deep JWST/NIRcam grism survey “All the Little Things” to measure the overdensities around BL-Hα emitters and around a spectroscopic reference sample of ∼300 galaxies. In our reference sample, we find that megaparsec-scale overdensity correlates with stellar mass. Their large-scale environments suggest that BL-Hα emitters are hosted by galaxies with stellar masses ≈5 × 10^7 M⊙, ≈40 times lower than those inferred from galaxy-only SED fits. Adding measurements around more luminous z ≈ 6 AGNs, we find tentative correlations between line width, BH mass, and the overdensity, suggestive of a steep BH to halo mass relation. The main implications are (1) when BH masses are taken at face value, we confirm extremely high BH to stellar mass ratios of ≈10%, (2) the galaxies of low stellar mass that host growing SMBHs are in tension with typical hydrodynamical simulations, except those without feedback, (3) a 1% duty cycle implied by the host mass hints at super-Eddington accretion, (4) the masses are at odds with an interpretation of the line broadening in terms of high stellar density, (5) our results imply a luminosity-dependent diversity of galaxy masses, environments, and SEDs among AGN samples.","lang":"eng"}],"date_published":"2025-07-29T00:00:00Z","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"29","quality_controlled":"1","oa":1,"month":"07","PlanS_conform":"1","date_updated":"2026-02-09T08:22:01Z","date_created":"2026-01-28T15:25:42Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"21062","status":"public","article_processing_charge":"Yes","issue":"2","type":"journal_article","article_type":"original","corr_author":"1","author":[{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","last_name":"Kotiwale"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"last_name":"Greene","full_name":"Greene, Jenny","first_name":"Jenny"},{"last_name":"Adamo","full_name":"Adamo, Angela","first_name":"Angela"},{"full_name":"Bouwens, Rychard J.","last_name":"Bouwens","first_name":"Rychard J."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia"},{"full_name":"Eilers, Anna-Christina","last_name":"Eilers","first_name":"Anna-Christina"},{"full_name":"de Graaff, Anna","last_name":"de Graaff","first_name":"Anna"},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"},{"last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto"}]},{"department":[{"_id":"JoMa"}],"arxiv":1,"doi":"10.1093/mnras/staf030","ddc":["520"],"has_accepted_license":"1","publication_status":"published","title":"Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures","external_id":{"arxiv":["2309.04525"]},"publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"OA_place":"publisher","DOAJ_listed":"1","year":"2025","publisher":"Oxford University Press","language":[{"iso":"eng"}],"volume":537,"fulldoi":"https://doi.org/10.1093/mnras/staf030","file":[{"content_type":"application/pdf","file_id":"21169","creator":"dernst","relation":"main_file","checksum":"4cbade43244eaa8b60bb05a90ae613da","file_size":2787493,"date_updated":"2026-02-09T08:39:19Z","file_name":"2025_MonthlyNoticesRAS_HerardDemanche.pdf","success":1,"date_created":"2026-02-09T08:39:19Z","access_level":"open_access"}],"oa_version":"Published Version","citation":{"ieee":"T. Herard-Demanche <i>et al.</i>, “Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 2. Oxford University Press, pp. 788–808, 2025.","ista":"Herard-Demanche T, Bouwens RJ, Oesch PA, Naidu RP, Decarli R, Nelson EJ, Brammer G, Weibel A, Xiao M, Stefanon M, Walter F, Matthee JJ, Meyer RA, Wuyts S, Reddy N, Rowland L, van Leeuwen I, Haro PA, Dannerbauer H, Shapley AE, Chisholm J, van Dokkum P, Labbe I, Illingworth G, Schaerer D, Shivaei I. 2025. Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. 537(2), 788–808.","ama":"Herard-Demanche T, Bouwens RJ, Oesch PA, et al. Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(2):788-808. doi:<a href=\"https://doi.org/10.1093/mnras/staf030\">10.1093/mnras/staf030</a>","chicago":"Herard-Demanche, Thomas, Rychard J Bouwens, Pascal A Oesch, Rohan P Naidu, Roberto Decarli, Erica J Nelson, Gabriel Brammer, et al. “Mapping Dusty Galaxy Growth at z &#62; 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf030\">https://doi.org/10.1093/mnras/staf030</a>.","apa":"Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., Naidu, R. P., Decarli, R., Nelson, E. J., … Shivaei, I. (2025). Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf030\">https://doi.org/10.1093/mnras/staf030</a>","mla":"Herard-Demanche, Thomas, et al. “Mapping Dusty Galaxy Growth at z &#62; 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 2, Oxford University Press, 2025, pp. 788–808, doi:<a href=\"https://doi.org/10.1093/mnras/staf030\">10.1093/mnras/staf030</a>.","short":"T. Herard-Demanche, R.J. Bouwens, P.A. Oesch, R.P. Naidu, R. Decarli, E.J. Nelson, G. Brammer, A. Weibel, M. Xiao, M. Stefanon, F. Walter, J.J. Matthee, R.A. Meyer, S. Wuyts, N. Reddy, L. Rowland, I. van Leeuwen, P.A. Haro, H. Dannerbauer, A.E. Shapley, J. Chisholm, P. van Dokkum, I. Labbe, G. Illingworth, D. Schaerer, I. Shivaei, Monthly Notices of the Royal Astronomical Society 537 (2025) 788–808."},"date_published":"2025-02-01T00:00:00Z","day":"01","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","oa":1,"month":"02","PlanS_conform":"1","date_updated":"2026-02-09T08:50:55Z","OA_type":"gold","intvolume":"       537","acknowledgement":"We are grateful to Roberto Neri and collaborators for providing us with spatially resolved information on both the dust-continuum and [C ii] line emission from their high spatial resolution PdBI observations. This project was made possible in part by the Leiden University Fund/Bouwens Astrophysics Fund. RJB acknowledges support from NWO grants 600.065.140.11N211 (vrij competitie) and TOP grant TOP1.16.057. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. Support for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. RPN acknowledges funding from JWST programs GO-1933 and GO-2279. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the CIDEGENT/2021/059 grant, from project PID2019-109592GB-I00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación. This study forms part of the Astrophysics and High Energy Physics programme and was supported by MCIN with funding from European Union NextGenerationEU (PRTR-C17.I1) and by Generalitat Valenciana under the project n. ASFAE/2022/025. RAM acknowledges support from the ERC Advanced Grant 740246 (Cosmic_Gas) and the Swiss National Science Foundation through project grant 200020_207349.\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 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 no. 1895.\r\n\r\nThis paper made use of several publicly available software packages. We are indebted to the respective authors for their work: ipython (Pérez & Granger 2007), matplotlib (Hunter 2007), numpy (Oliphant 2006), scipy (Virtanen et al. 2020), jupyter (Kluyver et al. 2016), astropy (Astropy Collaboration 2013, 2018), grizli (v1.7.11; Brammer 2018; Brammer et al. 2022), eazy (Brammer, van Dokkum & Coppi 2008), and SExtractor (Bertin & Arnouts 1996).","file_date_updated":"2026-02-09T08:39:19Z","abstract":[{"text":"We report the detection of a 13σ Hα emission line from HDF850.1 at z = 5.188 ± 0.001 using the FRESCO (First Reionization Era SpectroscopicallyComplete Observations) NIRCam F444W grism observations. Detection of Hα in HDF850.1 is noteworthy, given its high far-infrared (IR) luminosity, substantial dust obscuration, and the historical challenges in deriving its redshift.\r\nHDF850.1 shows a clear detection in the F444W imaging data, distributed between a northern and southern component, mirroring that seen in [C II] from the Plateau de Bure Interferometer. Modelling the spectral energy distribution of each component separately, we find that the northern component has a higher mass, star formation rate (SFR), and dust extinction than the southern component. The observed Hα emission appears to arise entirely from the less-obscured southern component and shows a similar \u0004v∼ + 130 km s −1 velocity offset to that seen for [C II] relative to the source systemic redshift. Leveraging Hα-derived redshiftsfrom FRESCO observations, we find that HDF850.1 isforming in one of the richest environments identified to date at z > 5, with 100 z = 5.17–5.20 galaxies distributed across 13 smaller structures and a ∼(15 cMpc)3 volume. Based on the evolution of analogous structures in cosmological simulations, the z = 5.17–5.20 structures seem likely to collapse into\r\na single > 1014M cluster by z ∼ 0. Comparing galaxy properties forming within this overdensity with those outside, we find the masses, SFRs, and UV luminosities inside the overdensity to be clearly higher. The prominence of Hα line emission from HDF850.1 and other known highly obscured z > 5 galaxies illustrates the potential of NIRCam-grism programs to map both\r\nthe early build-up of IR-luminous galaxies and overdense structures.","lang":"eng"}],"type":"journal_article","issue":"2","page":"788-808","article_type":"original","author":[{"first_name":"Thomas","last_name":"Herard-Demanche","full_name":"Herard-Demanche, Thomas"},{"first_name":"Rychard J","full_name":"Bouwens, Rychard J","last_name":"Bouwens"},{"first_name":"Pascal A","last_name":"Oesch","full_name":"Oesch, Pascal A"},{"first_name":"Rohan P","full_name":"Naidu, Rohan P","last_name":"Naidu"},{"first_name":"Roberto","last_name":"Decarli","full_name":"Decarli, Roberto"},{"full_name":"Nelson, Erica J","last_name":"Nelson","first_name":"Erica J"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"last_name":"Weibel","full_name":"Weibel, Andrea","first_name":"Andrea"},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"},{"first_name":"Mauro","full_name":"Stefanon, Mauro","last_name":"Stefanon"},{"first_name":"Fabian","full_name":"Walter, Fabian","last_name":"Walter"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Romain A","full_name":"Meyer, Romain A","last_name":"Meyer"},{"first_name":"Stijn","last_name":"Wuyts","full_name":"Wuyts, Stijn"},{"last_name":"Reddy","full_name":"Reddy, Naveen","first_name":"Naveen"},{"last_name":"Rowland","full_name":"Rowland, Lucie","first_name":"Lucie"},{"full_name":"van Leeuwen, Ivana","last_name":"van Leeuwen","first_name":"Ivana"},{"first_name":"Pablo Arrabal","last_name":"Haro","full_name":"Haro, Pablo Arrabal"},{"last_name":"Dannerbauer","full_name":"Dannerbauer, Helmut","first_name":"Helmut"},{"last_name":"Shapley","full_name":"Shapley, Alice E","first_name":"Alice E"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"last_name":"van Dokkum","full_name":"van Dokkum, Pieter","first_name":"Pieter"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"full_name":"Illingworth, Garth","last_name":"Illingworth","first_name":"Garth"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"}],"date_created":"2026-01-28T15:25:53Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"21063","status":"public","article_processing_charge":"Yes"},{"department":[{"_id":"JoMa"}],"has_accepted_license":"1","doi":"10.3847/1538-4357/ae089c","ddc":["520"],"publication_status":"published","title":"Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization","publication":"The Astrophysical Journal","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_number":"86","DOAJ_listed":"1","OA_place":"publisher","year":"2025","publisher":"IOP Publishing","volume":994,"language":[{"iso":"eng"}],"citation":{"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>.","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>","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).","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>.","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.","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."},"oa_version":"Published Version","scopus_import":"1","fulldoi":"https://doi.org/10.3847/1538-4357/ae089c","file":[{"date_created":"2026-04-13T07:53:00Z","success":1,"access_level":"open_access","relation":"main_file","creator":"dernst","content_type":"application/pdf","file_id":"21731","file_name":"2025_AstrophysicalJournal_Rinaldi.pdf","date_updated":"2026-04-13T07:53:00Z","checksum":"5d13b0ad3e9f56cbe29c5de0ba5757c8","file_size":10298729}],"day":"20","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","oa":1,"date_published":"2025-11-20T00:00:00Z","date_updated":"2026-04-13T07:54:11Z","PlanS_conform":"1","month":"11","OA_type":"gold","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).","intvolume":"       994","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"}],"file_date_updated":"2026-04-13T07:53:00Z","type":"journal_article","issue":"1","author":[{"first_name":"Pierluigi","full_name":"Rinaldi, Pierluigi","last_name":"Rinaldi"},{"first_name":"Pablo G.","full_name":"Pérez-González, Pablo G.","last_name":"Pérez-González"},{"full_name":"Rieke, George H.","last_name":"Rieke","first_name":"George H."},{"full_name":"Lyu, Jianwei","last_name":"Lyu","first_name":"Jianwei"},{"last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco","first_name":"Francesco"},{"first_name":"Zihao","full_name":"Wu, Zihao","last_name":"Wu"},{"full_name":"Carniani, Stefano","last_name":"Carniani","first_name":"Stefano"},{"first_name":"Tobias J.","last_name":"Looser","full_name":"Looser, Tobias J."},{"full_name":"Shivaei, Irene","last_name":"Shivaei","first_name":"Irene"},{"first_name":"Leindert A.","full_name":"Boogaard, Leindert A.","last_name":"Boogaard"},{"full_name":"Diaz-Santos, Tanio","last_name":"Diaz-Santos","first_name":"Tanio"},{"last_name":"Colina","full_name":"Colina, Luis","first_name":"Luis"},{"last_name":"Östlin","full_name":"Östlin, Göran","first_name":"Göran"},{"first_name":"Stacey","full_name":"Alberts, Stacey","last_name":"Alberts"},{"last_name":"Álvarez-Márquez","full_name":"Álvarez-Márquez, Javier","first_name":"Javier"},{"last_name":"Annuziatella","full_name":"Annuziatella, Marianna","first_name":"Marianna"},{"last_name":"Aravena","full_name":"Aravena, Manuel","first_name":"Manuel"},{"first_name":"Rachana","last_name":"Bhatawdekar","full_name":"Bhatawdekar, Rachana"},{"first_name":"Andrew J.","full_name":"Bunker, Andrew J.","last_name":"Bunker"},{"first_name":"Karina I.","last_name":"Caputi","full_name":"Caputi, Karina I."},{"last_name":"Charlot","full_name":"Charlot, Stéphane","first_name":"Stéphane"},{"first_name":"Alejandro","full_name":"Crespo Gómez, Alejandro","last_name":"Crespo Gómez"},{"first_name":"Mirko","last_name":"Curti","full_name":"Curti, Mirko"},{"full_name":"Eckart, Andreas","last_name":"Eckart","first_name":"Andreas"},{"first_name":"Steven","full_name":"Gillman, Steven","last_name":"Gillman"},{"full_name":"Hainline, Kevin","last_name":"Hainline","first_name":"Kevin"},{"first_name":"Nimisha","last_name":"Kumari","full_name":"Kumari, Nimisha"},{"full_name":"Hjorth, Jens","last_name":"Hjorth","first_name":"Jens"},{"last_name":"Iani","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"first_name":"Zhiyuan","last_name":"Ji","full_name":"Ji, Zhiyuan"},{"first_name":"Benjamin D.","last_name":"Johnson","full_name":"Johnson, Benjamin D."},{"last_name":"Jones","full_name":"Jones, Gareth C.","first_name":"Gareth C."},{"first_name":"Álvaro","full_name":"Labiano, Álvaro","last_name":"Labiano"},{"full_name":"Maiolino, Roberto","last_name":"Maiolino","first_name":"Roberto"},{"first_name":"Jens","full_name":"Melinder, Jens","last_name":"Melinder"},{"first_name":"Thibaud","last_name":"Moutard","full_name":"Moutard, Thibaud"},{"full_name":"Peissker, Florian","last_name":"Peissker","first_name":"Florian"},{"full_name":"Rieke, Marcia","last_name":"Rieke","first_name":"Marcia"},{"full_name":"Robertson, Brant","last_name":"Robertson","first_name":"Brant"},{"last_name":"Scholtz","full_name":"Scholtz, Jan","first_name":"Jan"},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"full_name":"Van Der Werf, Paul P.","last_name":"Van Der Werf","first_name":"Paul P."},{"full_name":"Walter, Fabian","last_name":"Walter","first_name":"Fabian"},{"first_name":"Christina C.","last_name":"Williams","full_name":"Williams, Christina C."},{"first_name":"Chris","last_name":"Willott","full_name":"Willott, Chris"},{"full_name":"Witstok, Joris","last_name":"Witstok","first_name":"Joris"},{"first_name":"Hannah","full_name":"Übler, Hannah","last_name":"Übler"},{"first_name":"Yongda","last_name":"Zhu","full_name":"Zhu, Yongda"}],"article_type":"original","_id":"21727","date_created":"2026-04-12T22:01:53Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"Yes","status":"public"},{"_id":"18854","date_created":"2025-01-19T23:01:52Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","status":"public","type":"journal_article","isi":1,"author":[{"first_name":"K. E.","full_name":"Heintz, K. E.","last_name":"Heintz"},{"first_name":"G. B.","last_name":"Brammer","full_name":"Brammer, G. B."},{"first_name":"D.","full_name":"Watson, D.","last_name":"Watson"},{"last_name":"Oesch","full_name":"Oesch, P. A.","first_name":"P. A."},{"full_name":"Keating, L. C.","last_name":"Keating","first_name":"L. C."},{"first_name":"M. J.","last_name":"Hayes","full_name":"Hayes, M. J."},{"first_name":"Unknown","full_name":"Abdurro'Uf, Unknown","last_name":"Abdurro'Uf"},{"first_name":"K. Z.","last_name":"Arellano-Córdova","full_name":"Arellano-Córdova, K. Z."},{"first_name":"A. C.","last_name":"Carnall","full_name":"Carnall, A. C."},{"full_name":"Christiansen, C. R.","last_name":"Christiansen","first_name":"C. R."},{"last_name":"Cullen","full_name":"Cullen, F.","first_name":"F."},{"first_name":"R.","full_name":"Davé, R.","last_name":"Davé"},{"first_name":"P.","full_name":"Dayal, P.","last_name":"Dayal"},{"first_name":"A.","last_name":"Ferrara","full_name":"Ferrara, A."},{"first_name":"K.","full_name":"Finlator, K.","last_name":"Finlator"},{"first_name":"J. P.U.","last_name":"Fynbo","full_name":"Fynbo, J. P.U."},{"first_name":"S. R.","full_name":"Flury, S. R.","last_name":"Flury"},{"first_name":"V.","last_name":"Gelli","full_name":"Gelli, V."},{"last_name":"Gillman","full_name":"Gillman, S.","first_name":"S."},{"first_name":"R.","full_name":"Gottumukkala, R.","last_name":"Gottumukkala"},{"full_name":"Gould, K.","last_name":"Gould","first_name":"K."},{"first_name":"T. R.","last_name":"Greve","full_name":"Greve, T. R."},{"first_name":"S. E.","full_name":"Hardin, S. E.","last_name":"Hardin"},{"last_name":"Hsiao","full_name":"Hsiao, T. Y.Y.","first_name":"T. Y.Y."},{"full_name":"Hutter, A.","last_name":"Hutter","first_name":"A."},{"first_name":"P.","full_name":"Jakobsson, P.","last_name":"Jakobsson"},{"first_name":"M.","full_name":"Killi, M.","last_name":"Killi"},{"first_name":"N.","full_name":"Khosravaninezhad, N.","last_name":"Khosravaninezhad"},{"first_name":"P.","last_name":"Laursen","full_name":"Laursen, P."},{"last_name":"Lee","full_name":"Lee, M. M.","first_name":"M. M."},{"first_name":"G. E.","last_name":"Magdis","full_name":"Magdis, G. E."},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Naidu","full_name":"Naidu, R. P.","first_name":"R. P."},{"first_name":"D.","last_name":"Narayanan","full_name":"Narayanan, D."},{"first_name":"C.","full_name":"Pollock, C.","last_name":"Pollock"},{"full_name":"Prescott, M. K.M.","last_name":"Prescott","first_name":"M. K.M."},{"full_name":"Rusakov, V.","last_name":"Rusakov","first_name":"V."},{"last_name":"Shuntov","full_name":"Shuntov, M.","first_name":"M."},{"first_name":"A.","full_name":"Sneppen, A.","last_name":"Sneppen"},{"last_name":"Smit","full_name":"Smit, R.","first_name":"R."},{"last_name":"Tanvir","full_name":"Tanvir, N. R.","first_name":"N. R."},{"last_name":"Terp","full_name":"Terp, C.","first_name":"C."},{"full_name":"Toft, S.","last_name":"Toft","first_name":"S."},{"first_name":"F.","last_name":"Valentino","full_name":"Valentino, F."},{"last_name":"Vijayan","full_name":"Vijayan, A. P.","first_name":"A. P."},{"full_name":"Weaver, J. R.","last_name":"Weaver","first_name":"J. R."},{"full_name":"Wise, J. H.","last_name":"Wise","first_name":"J. H."},{"last_name":"Witstok","full_name":"Witstok, J.","first_name":"J."}],"article_type":"original","OA_type":"diamond","acknowledgement":"We would like to thank the referee for a detailed and constructive report, greatly improving the presentation of the results in this work. We would like to thank Peter Jakobsen for his vision and heroic endeavor in optimally designing the JWST/NIRSpec instrument and some of its first on-sky observations and for enlightening discussions about the intricacies of the NIRSpec data. Further, we would like to thank John Chisholm for helpful clarifications and discussions related to the escape fraction of ionizing photons and Aayush Saxena for enlightening conversations on the escape and absorption of Lyman-α photons. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. The data products presented herein were retrieved from the DAWN JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center, which is funded by the Danish National Research Foundation under grant DNRF140. P.D. acknowledge support from the NWO grant 016.VIDI.189.162 (“ODIN\") and warmly thanks the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. Support from the ERC Advanced Grant INTERSTELLAR H2020/740120 is kindly acknowledged (A.F.). S.G. acknowledges financial support from the Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. M.K. was supported by the ANID BASAL project FB210003. G.E.M. acknowledges financial support from the Villum Young Investigator grants 37440 and 13160 and the Cosmic Dawn Center. J.W. acknowledges support from the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, by the UKRI Frontier Research grant RISEandFALL. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. F.C. acknowledges support from a UKRI Frontier Research Guarantee Grant (PI Cullen; grant reference EP/X021025/1). J.H.W. acknowledges support by NSF grant AST-2108020 and NASA grants 80NSSC20K0520 and 80NSSC21K1053. NRT acknowledges support through STFC consolidated grant ST/W000857/1. M.J.H. is supported by the Swedish Research Council, VetenskapsrÅdet, and is fellow of the Knut & Alice Wallenberg foundation. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. Software: This work made use of and acknowledge the following software: NumPy (Harris et al. 2020), Matplotlib (Hunter 2007), LMfit (Newville et al. 2014), SciPy (Virtanen et al. 2020), grizli (Brammer 2023a), Astrodrizzle (Gonzaga et al. 2012), and MsaExp (v0.3; Brammer 2023b).","intvolume":"       693","file_date_updated":"2025-01-20T09:17:33Z","abstract":[{"lang":"eng","text":"Context. One of the surprising early findings with JWST has been the discovery of a strong “roll-over” or a softening of the absorption edge of Lyα in a large number of galaxies at z ≳ 6, in addition to systematic offsets from photometric redshift estimates and fundamental galaxy scaling relations. This has been interpreted as strong cumulative damped Lyα absorption (DLA) wings from high column densities of neutral atomic hydrogen (H I), signifying major gas accretion events in the formation of these galaxies.\r\nAims. To explore this new phenomenon systematically, we assembled the JWST/NIRSpec PRImordial gas Mass AssembLy (PRIMAL) legacy survey of 584 galaxies at z = 5.0 − 13.4, designed to study the physical properties and gas in and around galaxies during the reionization epoch.\r\nMethods. We characterized this benchmark sample in full and spectroscopically derived the galaxy redshifts, metallicities, star formation rates, and ultraviolet (UV) slopes. We defined a new diagnostic, the Lyα damping parameter DLyα, to measure and quantify the net effect of Lyα emission strength, the H I fraction in the intergalactic medium, or the local H I column density for each source. The JWST-PRIMAL survey is based on the spectroscopic DAWN JWST Archive (DJA-Spec). We describe DJA-Spec in this paper, detailing the reduction methods, the post-processing steps, and basic analysis tools. All the software, reduced spectra, and spectroscopically derived quantities and catalogs are made publicly available in dedicated repositories.\r\nResults. We find that the fraction of galaxies showing strong integrated DLAs with NHI > 1021 cm−2 only increases slightly from ≈60% at z ≈ 6 up to ≈65 − 90% at z > 8. Similarly, the prevalence and prominence of Lyα emission is found to increase with decreasing redshift, in qualitative agreement with previous observational results. Strong Lyα emitters (LAEs) are predominantly found to be associated with low-metallicity and UV faint galaxies. By contrast, strong DLAs are observed in galaxies with a variety of intrinsic physical properties, but predominantly at high redshifts and low metallicities.\r\nConclusions. Our results indicate that strong DLAs likely reflect a particular early assembly phase of reionization-era galaxies, at which point they are largely dominated by pristine H I gas accretion. At z = 8 − 10, this gas gradually cools and forms into stars that ionize their local surroundings, forming large ionized bubbles and producing strong observed Lyα emission at z < 8."}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","day":"06","oa":1,"date_published":"2025-01-06T00:00:00Z","date_updated":"2026-02-16T12:07:37Z","month":"01","volume":693,"language":[{"iso":"eng"}],"scopus_import":"1","citation":{"apa":"Heintz, K. E., Brammer, G. B., Watson, D., Oesch, P. A., Keating, L. C., Hayes, M. J., … Witstok, J. (2025). The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450243\">https://doi.org/10.1051/0004-6361/202450243</a>","mla":"Heintz, K. E., et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600 Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 693, A60, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450243\">10.1051/0004-6361/202450243</a>.","short":"K.E. Heintz, G.B. Brammer, D. Watson, P.A. Oesch, L.C. Keating, M.J. Hayes, U. Abdurro’Uf, K.Z. Arellano-Córdova, A.C. Carnall, C.R. Christiansen, F. Cullen, R. Davé, P. Dayal, A. Ferrara, K. Finlator, J.P.U. Fynbo, S.R. Flury, V. Gelli, S. Gillman, R. Gottumukkala, K. Gould, T.R. Greve, S.E. Hardin, T.Y.Y. Hsiao, A. Hutter, P. Jakobsson, M. Killi, N. Khosravaninezhad, P. Laursen, M.M. Lee, G.E. Magdis, J.J. Matthee, R.P. Naidu, D. Narayanan, C. Pollock, M.K.M. Prescott, V. Rusakov, M. Shuntov, A. Sneppen, R. Smit, N.R. Tanvir, C. Terp, S. Toft, F. Valentino, A.P. Vijayan, J.R. Weaver, J.H. Wise, J. Witstok, Astronomy &#38; Astrophysics 693 (2025).","ista":"Heintz KE, Brammer GB, Watson D, Oesch PA, Keating LC, Hayes MJ, Abdurro’Uf U, Arellano-Córdova KZ, Carnall AC, Christiansen CR, Cullen F, Davé R, Dayal P, Ferrara A, Finlator K, Fynbo JPU, Flury SR, Gelli V, Gillman S, Gottumukkala R, Gould K, Greve TR, Hardin SE, Hsiao TYY, Hutter A, Jakobsson P, Killi M, Khosravaninezhad N, Laursen P, Lee MM, Magdis GE, Matthee JJ, Naidu RP, Narayanan D, Pollock C, Prescott MKM, Rusakov V, Shuntov M, Sneppen A, Smit R, Tanvir NR, Terp C, Toft S, Valentino F, Vijayan AP, Weaver JR, Wise JH, Witstok J. 2025. The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy &#38; Astrophysics. 693, A60.","ieee":"K. E. Heintz <i>et al.</i>, “The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 693. EDP Sciences, 2025.","chicago":"Heintz, K. E., G. B. Brammer, D. Watson, P. A. Oesch, L. C. Keating, M. J. Hayes, Unknown Abdurro’Uf, et al. “The JWST-PRIMAL Archival Survey: A JWST/NIRSpec Reference Sample for the Physical Properties and Lyman-α Absorption and Emission of ∼600 Galaxies at z = 5.0-13.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202450243\">https://doi.org/10.1051/0004-6361/202450243</a>.","ama":"Heintz KE, Brammer GB, Watson D, et al. The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. <i>Astronomy &#38; Astrophysics</i>. 2025;693. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450243\">10.1051/0004-6361/202450243</a>"},"oa_version":"Published Version","fulldoi":"https://doi.org/10.1051/0004-6361/202450243","file":[{"date_created":"2025-01-20T09:17:33Z","success":1,"access_level":"open_access","relation":"main_file","creator":"dernst","content_type":"application/pdf","file_id":"18858","file_size":4513466,"checksum":"67a791080ade9bfb449d249de2af7456","date_updated":"2025-01-20T09:17:33Z","file_name":"2025_AstronomyAstrophysics_Heintz.pdf"}],"OA_place":"publisher","year":"2025","publisher":"EDP Sciences","external_id":{"isi":["001390856800001"]},"publication_status":"published","title":"The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4","publication":"Astronomy & Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_number":"A60","department":[{"_id":"JoMa"}],"has_accepted_license":"1","doi":"10.1051/0004-6361/202450243","ddc":["520"]},{"author":[{"first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"first_name":"Matteo","full_name":"Messa, Matteo","last_name":"Messa"},{"last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava","first_name":"Miroslava"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."}],"page":"2535-2558","article_type":"original","issue":"3","type":"journal_article","isi":1,"article_processing_charge":"No","status":"public","_id":"19066","date_created":"2025-02-23T23:01:55Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2026-02-16T11:51:48Z","month":"03","oa":1,"day":"01","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"quality_controlled":"1","date_published":"2025-03-01T00:00:00Z","abstract":[{"text":"We present a sample of 1956 individual stellar clumps at redshift 0.7 < z < 10, detected with JWST/NIRCam in 476 galaxies lensed by the galaxy cluster Abell2744. The lensed clumps present magnifications ranging between μ = 1.8 and μ = 300. We perform simultaneous size-photometry estimates in 20 JWST/NIRCam median and broad-band filters from 0.7 to 5 μm.\r\nSpectral energy distribution (SED) fitting analyses enable us to recover the physical properties of the clumps. The majority of the clumps are spatially resolved and have effective radii in the range Reff = 10–700 pc. We restrict this first study to the 1751 post-reionization era clumps with redshift < 5.5. We find a significant evolution of the average clump ages, star formation rates (SFRs), SFR surface densities, and metallicity with increasing redshift, while median stellar mass and stellar mass surface densities are similar in the probed redshift range. We observe a strong correlation between the clump properties and the properties of their host galaxies, with more massive galaxies hosting more massive and older clumps. We find that clumps closer to their host galactic centre are on average more massive, while their ages do not show clear sign of migration. We find that clumps at cosmic noon sample the upper-mass end of the mass function to higher masses than at z > 3, reflecting the rapid increase towards the peak of the cosmic star formation history. We conclude that the results achieved over the studied redshift range are in agreement with expectation of in situ clump formation scenario from large-scale disc fragmentation. ","lang":"eng"}],"file_date_updated":"2025-02-25T06:38:43Z","acknowledgement":"The authors thank the International Space Science Institute for sponsoring the ISSI team: ‘Star Formation within rapidly evolving galaxies’ where many ideas discussed in this article have been brainstormed. AA and AC acknowledge support by the Swedish research council Vetenskapsrådet (2021-05559). MM acknowledges the financial support through grant PRIN-MIUR 2020SKSTHZ. JM and IK acknowledge support 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. RPN acknowledges funding from JWST programme GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","intvolume":"       537","OA_type":"gold","publisher":"Oxford University Press","year":"2025","DOAJ_listed":"1","OA_place":"publisher","scopus_import":"1","citation":{"ieee":"A. Claeyssens <i>et al.</i>, “Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3. Oxford University Press, pp. 2535–2558, 2025.","ista":"Claeyssens A, Adamo A, Messa M, Dessauges-Zavadsky M, Richard J, Kramarenko I, Matthee JJ, Naidu RP. 2025. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. 537(3), 2535–2558.","chicago":"Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky, Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>.","ama":"Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(3):2535-2558. doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>","apa":"Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J., Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>","mla":"Claeyssens, Adélaïde, et al. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>.","short":"A. Claeyssens, A. Adamo, M. Messa, M. Dessauges-Zavadsky, J. Richard, I. Kramarenko, J.J. Matthee, R.P. Naidu, Monthly Notices of the Royal Astronomical Society 537 (2025) 2535–2558."},"oa_version":"Published Version","file":[{"file_size":35099276,"checksum":"431aef05755e6b5472f5e9b4c326cf84","date_updated":"2025-02-25T06:38:43Z","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf","content_type":"application/pdf","file_id":"19084","relation":"main_file","creator":"dernst","access_level":"open_access","success":1,"date_created":"2025-02-25T06:38:43Z"}],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"fulldoi":"https://doi.org/10.1093/mnras/staf058","volume":537,"language":[{"iso":"eng"}],"has_accepted_license":"1","ddc":["520"],"doi":"10.1093/mnras/staf058","arxiv":1,"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"external_id":{"arxiv":["2410.10974"],"isi":["001420026000001"]},"title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","publication_status":"published"},{"ddc":["520"],"doi":"10.1051/0004-6361/202450426","has_accepted_license":"1","department":[{"_id":"JoMa"}],"article_number":"A100","publication":"Astronomy & Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"],"issnl":["0004-6361"]},"title":"The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies","publication_status":"published","external_id":{"isi":["001417357000009"]},"publisher":"EDP Sciences","year":"2025","OA_place":"publisher","file":[{"file_id":"19087","content_type":"application/pdf","relation":"main_file","creator":"dernst","file_name":"2025_AstronomyAstrophysics_Vitte.pdf","date_updated":"2025-02-25T07:19:34Z","file_size":3444203,"checksum":"ed2a5bba313e54ed250be348bd8c1d95","success":1,"date_created":"2025-02-25T07:19:34Z","access_level":"open_access"}],"fulldoi":"https://doi.org/10.1051/0004-6361/202450426","citation":{"ama":"Vitte E, Verhamme A, Hibon P, et al. The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450426\">10.1051/0004-6361/202450426</a>","chicago":"Vitte, Eloïse, Anne Verhamme, Pascale Hibon, Floriane Leclercq, Belén Alcalde Pampliega, Josephine Kerutt, Haruka Kusakabe, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202450426\">https://doi.org/10.1051/0004-6361/202450426</a>.","ieee":"E. Vitte <i>et al.</i>, “The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.","ista":"Vitte E, Verhamme A, Hibon P, Leclercq F, Alcalde Pampliega B, Kerutt J, Kusakabe H, Matthee JJ, Guo Y, Bacon R, Maseda M, Richard J, Pharo J, Schaye J, Boogaard L, Nanayakkara T, Contini T. 2025. The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. Astronomy &#38; Astrophysics. 694, A100.","short":"E. Vitte, A. Verhamme, P. Hibon, F. Leclercq, B. Alcalde Pampliega, J. Kerutt, H. Kusakabe, J.J. Matthee, Y. Guo, R. Bacon, M. Maseda, J. Richard, J. Pharo, J. Schaye, L. Boogaard, T. Nanayakkara, T. Contini, Astronomy &#38; Astrophysics 694 (2025).","mla":"Vitte, Eloïse, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A100, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450426\">10.1051/0004-6361/202450426</a>.","apa":"Vitte, E., Verhamme, A., Hibon, P., Leclercq, F., Alcalde Pampliega, B., Kerutt, J., … Contini, T. (2025). The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450426\">https://doi.org/10.1051/0004-6361/202450426</a>"},"oa_version":"Published Version","scopus_import":"1","language":[{"iso":"eng"}],"volume":694,"month":"02","date_updated":"2026-02-16T12:08:40Z","date_published":"2025-02-01T00:00:00Z","oa":1,"quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"01","file_date_updated":"2025-02-25T07:19:34Z","abstract":[{"lang":"eng","text":"Context. The hydrogen Lyman-alpha (Lyα) line, the brightest rest-frame ultraviolet line of high-redshift galaxies, exhibits a large variety of shapes, which is due to factors at different scales, from the interstellar medium to the intergalactic medium (IGM).\r\nAims. The aim of this work is to provide a systematic inventory and classification of the spectral shapes of Lyα emission lines to better understand the general population of high-redshift Lyα emitting galaxies (LAEs).\r\nMethods. Using the unprecedentedly deep data from the MUSE eXtremely Deep Field (MXDF; up to 140 hour exposure time), we selected 477 galaxies observed in the ∼2.8−6.6 redshift range, 15 of which have a systemic redshift from nebular lines. We developed a method to classify Lyα emission lines in four spectral and three spatial categories by combining a pure spectral analysis with a narrow-band image analysis. We measured spectral properties, such as the peak separation and the blue-to-total flux ratio for the double-peaked galaxies.\r\nResults. To ensure a robust sample for statistical analysis, we define two unbiased subsets, inclusive and restrictive, by applying thresholds for signal-to-noise ratio, peak separation, and Lyα luminosity, yielding a final unbiased sample of 206 galaxies. Our analysis reveals that between 32% and 51% of the galaxies exhibit double-peaked profiles, with peak separations ranging from 150 km s−1 to nearly 1600 km s−1. The fraction of double-peaked galaxies seems to evolve dependently with the Lyα luminosity, while we do not see a severe decrease in this fraction with redshift, which is expected given the IGM attenuation at high redshift. An artificial increase in the number of double-peaked galaxies at the highest redshifts may cause the observation of a plateau instead of a decrease. A notable number of these double-peaked profiles show blue-dominated spectra, suggesting unique gas dynamics and inflow characteristics in some high-redshift galaxies. The consequent fraction of blue-dominated spectra needs to be confirmed by obtaining new systemic redshift measurements. Among the double-peaked galaxies, 4% are spurious detections, that is, the blue and red peaks do not come from the same spatial location. Around 20% out of the 477 sources of the parent sample lie in a complex environment, meaning there are other clumps or galaxies at the same redshift within a distance of 30 kpc.\r\nConclusions. Our results suggest that the double-peaked LAE fraction may trace the evolution of IGM attenuation, but the faintest galaxies must be observed at high redshift. We also need more data to confirm the trend seen at low redshift. In addition, it is crucial to obtain secure systemic redshifts for LAEs to better constrain the nature of the Lyα double-peaked lines. Statistical samples of double-peaked and triple-peaked galaxies are a promising probe of the evolution of the physical properties of galaxies across cosmic time."}],"acknowledgement":"EV and AV acknowledges the support from the SNF grants PP00P2 176808 and 211023. HK acknowledges support from Japan Society for the Promotion of Science (JSPS) Overseas Research Fellowship as well as JSPS Research Fellowships for Young Scientists. JP acknowledges funding by the Deutsche Forschungsgemeinschaft, Grant Wi 1369/31-1. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of ASTROPY, which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018, 2022), and other software and packages: MPDAF (Piqueras et al. 2019), PHOTUTILS (Bradley 2023), NUMPY (van der Walt et al. 2011), SCIPY (Virtanen et al. 2020). The plots in this paper were created using MATPLOTLIB (Hunter 2007).","intvolume":"       694","OA_type":"hybrid","article_type":"original","author":[{"first_name":"Eloïse","last_name":"Vitte","full_name":"Vitte, Eloïse"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"},{"full_name":"Hibon, Pascale","last_name":"Hibon","first_name":"Pascale"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"Belén","last_name":"Alcalde Pampliega","full_name":"Alcalde Pampliega, Belén"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Guo","full_name":"Guo, Yucheng","first_name":"Yucheng"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"first_name":"John","full_name":"Pharo, John","last_name":"Pharo"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"},{"last_name":"Contini","full_name":"Contini, Thierry","first_name":"Thierry"}],"isi":1,"type":"journal_article","status":"public","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2025-02-23T23:01:56Z","_id":"19069"},{"file_date_updated":"2025-02-25T07:05:19Z","abstract":[{"text":"Context. Recent observations suggest a significant and rapid buildup of dust in galaxies at high redshift (z > 4); this presents new challenges to our understanding of galaxy formation in the early Universe. Although our understanding of the physics of dust production and destruction in a galaxy’s interstellar medium (ISM) is improving, investigating the baryonic processes in the early universe remains a complex task owing to the inherent degeneracies in cosmological simulations and chemical evolution models.\r\nAims. In this work we characterized the evolution of 98 z ∼ 5 star-forming galaxies observed as part of the ALMA Large Program ALPINE by constraining the physical processes underpinning the gas and dust production, consumption, and destruction in their ISM.\r\nMethods. We made use of chemical evolution models to simultaneously reproduce the observed dust and gas content of our galaxies, obtained respectively from spectral energy distribution (SED) fitting and ionized carbon measurements. For each galaxy we constrained the initial gas mass, gas inflows and outflows, and efficiencies of dust growth and destruction. We tested these models with both the canonical Chabrier and a top-heavy initial mass function (IMF); the latter allowed rapid dust production on shorter timescales.\r\nResults. We successfully reproduced the gas and dust content in most of the older galaxies (≳600 Myr) regardless of the assumed IMF, predicting dust production primarily through Type II supernovae (SNe) and no dust growth in the ISM, as well as moderate inflow of primordial gas. In the case of intermediate-age galaxies (300−600 Myr), we reproduced the gas and dust content through Type II SNe and dust growth in ISM, though we observed an overprediction of dust mass in older galaxies, potentially indicating an unaccounted dust destruction mechanism and/or an overestimation of the observed dust masses. The number of young galaxies (≲300 Myr) reproduced, increases for models assuming top-heavy IMF but with maximal prescriptions of dust production. Galactic outflows are required (up to a mass-loading factor of 2) to reproduce the observed gas and dust mass, and to recover the decreasing trend of gas and dust over stellar mass with age. Assuming the Chabrier IMF, models are able to reproduce ∼65% of the total sample, while with top-heavy IMF the fraction increases to ∼93%, alleviating the tension between the observations and the models. Observations from the James Webb Space Telescope (JWST) will allow us to remove degeneracies in the diverse intrinsic properties of these galaxies (e.g., star formation histories and metallicity), thereby refining our models.","lang":"eng"}],"acknowledgement":"We warmly thank the referee for her/his useful comments and suggestions that greatly improved the quality of our paper. P.S., A.N., and M.R. acknowledge support from the Narodowe Centrum Nauki (UMO2020/38/E/ST9/00077). M.R. acknowledges support from the Foundation for Polish Science (FNP) under the program START 063.2023. D.D. acknowledges support from the National Science Center (NCN) grant SONATA (UMO2020/39/D/ST9/00720). J. and K.M. are grateful for the support from the Polish National Science Centre via grant UMO-018/30/E/ST9/00082. J. acknowledges support from the European Union (MSCA EDUCADO, GA 101119830 and WIDERA ExGal-Twin, GA 101158446). M.B. gratefully acknowledges support from the ANID BASAL project FB210003 and from the FONDECYT regular grant 1211000. This work was supported by the French government through the France 2030 investment plan managed by the National Research Agency (ANR), as part of the Initiative of Excellence of Université Côte d’Azur under reference number ANR-15-IDEX-01. M.H. acknowledges support from the Polish National Science Center (UMO-2022/45/N/ST9/01336). E.I. acknowledges funding by ANID FONDECYT Regular 1221846. G.E.M. acknowledges the Villum Fonden research grant 13160 “Gas to stars, stars to dust: tracing star formation across cosmic time”, grant 37440, “The Hidden Cosmos”, and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140.","intvolume":"       694","OA_type":"diamond","month":"02","date_updated":"2026-02-16T12:08:24Z","date_published":"2025-02-01T00:00:00Z","oa":1,"quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"01","status":"public","article_processing_charge":"Yes","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2025-02-23T23:01:56Z","_id":"19070","article_type":"original","author":[{"first_name":"P.","last_name":"Sawant","full_name":"Sawant, P."},{"last_name":"Nanni","full_name":"Nanni, A.","first_name":"A."},{"full_name":"Romano, M.","last_name":"Romano","first_name":"M."},{"first_name":"D.","last_name":"Donevski","full_name":"Donevski, D."},{"last_name":"Bruzual","full_name":"Bruzual, G.","first_name":"G."},{"first_name":"N.","full_name":"Ysard, N.","last_name":"Ysard"},{"full_name":"Lemaux, B. C.","last_name":"Lemaux","first_name":"B. C."},{"full_name":"Inami, H.","last_name":"Inami","first_name":"H."},{"last_name":"Calura","full_name":"Calura, F.","first_name":"F."},{"last_name":"Pozzi","full_name":"Pozzi, F.","first_name":"F."},{"last_name":"Małek","full_name":"Małek, K.","first_name":"K."},{"last_name":"Junais","full_name":"Junais, J.","first_name":"J."},{"full_name":"Boquien, M.","last_name":"Boquien","first_name":"M."},{"full_name":"Faisst, A. L.","last_name":"Faisst","first_name":"A. L."},{"full_name":"Hamed, M.","last_name":"Hamed","first_name":"M."},{"first_name":"M.","last_name":"Ginolfi","full_name":"Ginolfi, M."},{"last_name":"Zamorani","full_name":"Zamorani, G.","first_name":"G."},{"first_name":"G.","full_name":"Lorenzon, G.","last_name":"Lorenzon"},{"last_name":"Molina","full_name":"Molina, J.","first_name":"J."},{"full_name":"Bardelli, S.","last_name":"Bardelli","first_name":"S."},{"first_name":"E.","full_name":"Ibar, E.","last_name":"Ibar"},{"full_name":"Vergani, D.","last_name":"Vergani","first_name":"D."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","full_name":"Di Cesare, Claudia","last_name":"Di Cesare"},{"last_name":"Béthermin","full_name":"Béthermin, M.","first_name":"M."},{"full_name":"Burgarella, D.","last_name":"Burgarella","first_name":"D."},{"last_name":"Cassata","full_name":"Cassata, P.","first_name":"P."},{"first_name":"M.","full_name":"Dessauges-Zavadsky, M.","last_name":"Dessauges-Zavadsky"},{"first_name":"E.","full_name":"D'Onghia, E.","last_name":"D'Onghia"},{"full_name":"Dubois, Y.","last_name":"Dubois","first_name":"Y."},{"full_name":"Magdis, G. E.","last_name":"Magdis","first_name":"G. E."},{"first_name":"H.","last_name":"Mendez-Hernandez","full_name":"Mendez-Hernandez, H."}],"isi":1,"type":"journal_article","article_number":"A82","publication":"Astronomy & Astrophysics","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"title":"The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies","publication_status":"published","external_id":{"isi":["001414753300028"]},"ddc":["520"],"doi":"10.1051/0004-6361/202451542","has_accepted_license":"1","department":[{"_id":"JoMa"}],"file":[{"relation":"main_file","creator":"dernst","file_id":"19086","content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_Sawant.pdf","date_updated":"2025-02-25T07:05:19Z","checksum":"792cbcda14148c352dc8c5a26058827d","file_size":7624067,"date_created":"2025-02-25T07:05:19Z","success":1,"access_level":"open_access"}],"fulldoi":"https://doi.org/10.1051/0004-6361/202451542","scopus_import":"1","citation":{"ieee":"P. Sawant <i>et al.</i>, “The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.","ista":"Sawant P, Nanni A, Romano M, Donevski D, Bruzual G, Ysard N, Lemaux BC, Inami H, Calura F, Pozzi F, Małek K, Junais J, Boquien M, Faisst AL, Hamed M, Ginolfi M, Zamorani G, Lorenzon G, Molina J, Bardelli S, Ibar E, Vergani D, Di Cesare C, Béthermin M, Burgarella D, Cassata P, Dessauges-Zavadsky M, D’Onghia E, Dubois Y, Magdis GE, Mendez-Hernandez H. 2025. The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. Astronomy &#38; Astrophysics. 694, A82.","chicago":"Sawant, P., A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B. C. Lemaux, et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202451542\">https://doi.org/10.1051/0004-6361/202451542</a>.","ama":"Sawant P, Nanni A, Romano M, et al. The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451542\">10.1051/0004-6361/202451542</a>","short":"P. Sawant, A. Nanni, M. Romano, D. Donevski, G. Bruzual, N. Ysard, B.C. Lemaux, H. Inami, F. Calura, F. Pozzi, K. Małek, J. Junais, M. Boquien, A.L. Faisst, M. Hamed, M. Ginolfi, G. Zamorani, G. Lorenzon, J. Molina, S. Bardelli, E. Ibar, D. Vergani, C. Di Cesare, M. Béthermin, D. Burgarella, P. Cassata, M. Dessauges-Zavadsky, E. D’Onghia, Y. Dubois, G.E. Magdis, H. Mendez-Hernandez, Astronomy &#38; Astrophysics 694 (2025).","apa":"Sawant, P., Nanni, A., Romano, M., Donevski, D., Bruzual, G., Ysard, N., … Mendez-Hernandez, H. (2025). The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451542\">https://doi.org/10.1051/0004-6361/202451542</a>","mla":"Sawant, P., et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A82, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451542\">10.1051/0004-6361/202451542</a>."},"oa_version":"Published Version","language":[{"iso":"eng"}],"volume":694,"publisher":"EDP Sciences","year":"2025","OA_place":"publisher"},{"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication":"Astronomy & Astrophysics","article_number":"A178","publication_status":"published","title":"An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy","external_id":{"isi":["001420194600001"],"arxiv":["2409.17241"]},"doi":"10.1051/0004-6361/202452363","ddc":["520"],"has_accepted_license":"1","department":[{"_id":"JoMa"}],"arxiv":1,"fulldoi":"https://doi.org/10.1051/0004-6361/202452363","file":[{"access_level":"open_access","date_created":"2025-03-04T09:29:01Z","success":1,"checksum":"b1e74644a0cd37550e9a553f8675c93f","file_size":1865856,"file_name":"2025_AstronomyAstrophysics_CoveloPaz.pdf","date_updated":"2025-03-04T09:29:01Z","creator":"dernst","relation":"main_file","file_id":"19285","content_type":"application/pdf"}],"citation":{"short":"A. Covelo-Paz, E. Giovinazzo, P.A. Oesch, R.A. Meyer, A. Weibel, G. Brammer, Y. Fudamoto, J. Kerutt, J. Lin, J. Matharu, R.P. Naidu, A. Velichko, V. Bollo, R. Bouwens, J. Chisholm, G.D. Illingworth, I. Kramarenko, D. Magee, M. Maseda, J.J. Matthee, E. Nelson, N. Reddy, D. Schaerer, M. Stefanon, M. Xiao, Astronomy &#38; Astrophysics 694 (2025).","mla":"Covelo-Paz, Alba, et al. “An Hα View of Galaxy Buildup in the First 2 Gyr: Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 694, A178, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202452363\">10.1051/0004-6361/202452363</a>.","apa":"Covelo-Paz, A., Giovinazzo, E., Oesch, P. A., Meyer, R. A., Weibel, A., Brammer, G., … Xiao, M. (2025). An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202452363\">https://doi.org/10.1051/0004-6361/202452363</a>","chicago":"Covelo-Paz, Alba, Emma Giovinazzo, Pascal A. Oesch, Romain A. Meyer, Andrea Weibel, Gabriel Brammer, Yoshinobu Fudamoto, et al. “An Hα View of Galaxy Buildup in the First 2 Gyr: Luminosity Functions at z ∼ 4−6.5 from NIRCam/Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202452363\">https://doi.org/10.1051/0004-6361/202452363</a>.","ama":"Covelo-Paz A, Giovinazzo E, Oesch PA, et al. An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2025;694. doi:<a href=\"https://doi.org/10.1051/0004-6361/202452363\">10.1051/0004-6361/202452363</a>","ieee":"A. Covelo-Paz <i>et al.</i>, “An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 694. EDP Sciences, 2025.","ista":"Covelo-Paz A, Giovinazzo E, Oesch PA, Meyer RA, Weibel A, Brammer G, Fudamoto Y, Kerutt J, Lin J, Matharu J, Naidu RP, Velichko A, Bollo V, Bouwens R, Chisholm J, Illingworth GD, Kramarenko I, Magee D, Maseda M, Matthee JJ, Nelson E, Reddy N, Schaerer D, Stefanon M, Xiao M. 2025. An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy. Astronomy &#38; Astrophysics. 694, A178."},"oa_version":"Published Version","scopus_import":"1","language":[{"iso":"eng"}],"volume":694,"year":"2025","publisher":"EDP Sciences","OA_place":"publisher","acknowledgement":"This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program Nos. 1895 and 3577. The authors sincerely thank the CONGRESS team (PIs: Egami & Sun) for developing their observing program with a zero-exclusive-access period. We thank Aswin Vijayan and Harley Katz for their help in analyzing the simulation data from FLARES and SPHINX. 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. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. Support for program #1895 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. 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. MS acknowledges support from the European Research Commission Consolidator Grant 101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and from project PID2023-149420NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU.","intvolume":"       694","file_date_updated":"2025-03-04T09:29:01Z","abstract":[{"lang":"eng","text":"The Hα nebular emission line is an optimal tracer for recent star formation in galaxies. With the advent of JWST, this line has recently become observable at z > 3 for the first time. We present a catalog of 1050 Hα emitters at 3.7 < z < 6.7 in the GOODS fields obtained from a blind search in JWST NIRCam/grism data. We made use of the FRESCO survey’s 124 arcmin2 of observations in GOODS-North and GOODS-South with the F444W filter, probing Hα at 4.9 < z < 6.7, and the CONGRESS survey’s 62 arcmin2 of observations in GOODS-North with F356W, probing Hα at 3.8 < z < 5.1. We found an overdensity with 98 sources at z ∼ 4.4 in GOODS-N, and confirmed previously reported overdensities at z ∼ 5.2 in GOODS-N and at z ∼ 5.4 and z ∼ 5.9 in GOODS-S. We computed the observed Hα luminosity functions (LFs) in three bins centered at z ∼ 4.45, 5.30, and 6.15, which are the first such measurements at z > 3 obtained based purely on spectroscopic data, robustly tracing galaxy star formation rates (SFRs) beyond the peak of the cosmic star formation history. We compared our results with theoretical predictions from three different simulations and found good agreement at z ∼ 4 − 6. The UV LFs of this spectroscopically confirmed sample are in good agreement with pre-JWST measurements obtained with photometrically selected objects. Finally, we derived SFR functions and integrated them to compute the evolution of the cosmic SFR densities across z ∼ 4 − 6, finding values in good agreement with recent UV estimates from Lyman-break galaxies, which imply a continuous decrease in SFR density by a factor of three over z ∼ 4 to z ∼ 6. Our work shows the power of NIRCam grism observations to efficiently provide new tests for early galaxy formation models based on emission line statistics."}],"OA_type":"diamond","month":"02","date_updated":"2026-02-16T12:08:59Z","date_published":"2025-02-12T00:00:00Z","quality_controlled":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"12","oa":1,"status":"public","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2025-03-02T23:01:54Z","_id":"19284","related_material":{"link":[{"url":" https://github.com/astroalba/fresco","relation":"software"}]},"article_type":"original","author":[{"first_name":"Alba","full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz"},{"first_name":"Emma","full_name":"Giovinazzo, Emma","last_name":"Giovinazzo"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"first_name":"Romain A.","full_name":"Meyer, Romain A.","last_name":"Meyer"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"full_name":"Fudamoto, Yoshinobu","last_name":"Fudamoto","first_name":"Yoshinobu"},{"first_name":"Josephine","full_name":"Kerutt, Josephine","last_name":"Kerutt"},{"first_name":"Jamie","last_name":"Lin","full_name":"Lin, Jamie"},{"last_name":"Matharu","full_name":"Matharu, Jasleen","first_name":"Jasleen"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Anna","full_name":"Velichko, Anna","last_name":"Velichko"},{"first_name":"Victoria","last_name":"Bollo","full_name":"Bollo, Victoria"},{"first_name":"Rychard","last_name":"Bouwens","full_name":"Bouwens, Rychard"},{"full_name":"Chisholm, John","last_name":"Chisholm","first_name":"John"},{"last_name":"Illingworth","full_name":"Illingworth, Garth D.","first_name":"Garth D."},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan"},{"full_name":"Magee, Daniel","last_name":"Magee","first_name":"Daniel"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Nelson, Erica","last_name":"Nelson","first_name":"Erica"},{"first_name":"Naveen","full_name":"Reddy, Naveen","last_name":"Reddy"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Mauro","full_name":"Stefanon, Mauro","last_name":"Stefanon"},{"full_name":"Xiao, Mengyuan","last_name":"Xiao","first_name":"Mengyuan"}],"type":"journal_article","isi":1},{"type":"journal_article","isi":1,"issue":"2","article_type":"original","author":[{"first_name":"Eshita","last_name":"Banerjee","full_name":"Banerjee, Eshita"},{"first_name":"Sowgat","full_name":"Muzahid, Sowgat","last_name":"Muzahid"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"first_name":"Jérémy","full_name":"Blaizot, Jérémy","last_name":"Blaizot"},{"first_name":"Nicolas","last_name":"Bouché","full_name":"Bouché, Nicolas"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Johnson, Sean D.","last_name":"Johnson","first_name":"Sean D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2025-03-09T23:01:26Z","_id":"19365","status":"public","article_processing_charge":"Yes","date_published":"2025-02-20T00:00:00Z","oa":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"day":"20","quality_controlled":"1","month":"02","date_updated":"2026-02-16T12:42:00Z","OA_type":"gold","abstract":[{"lang":"eng","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."}],"file_date_updated":"2025-03-10T11:54:52Z","intvolume":"       980","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).","OA_place":"publisher","DOAJ_listed":"1","publisher":"IOP Publishing","year":"2025","language":[{"iso":"eng"}],"volume":980,"file":[{"access_level":"open_access","date_created":"2025-03-10T11:54:52Z","success":1,"date_updated":"2025-03-10T11:54:52Z","file_name":"2025_AstrophysicalJour_Banerjee.pdf","file_size":1194131,"checksum":"1d33a8eb59f42a0c7a943c8859e9b883","relation":"main_file","creator":"dernst","file_id":"19379","content_type":"application/pdf"}],"fulldoi":"https://doi.org/10.3847/1538-4357/ada7e9","scopus_import":"1","citation":{"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>.","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.","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.","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>.","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)."},"oa_version":"Published Version","department":[{"_id":"JoMa"}],"ddc":["520"],"doi":"10.3847/1538-4357/ada7e9","has_accepted_license":"1","title":"MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3","publication_status":"published","external_id":{"isi":["001421001500001"]},"article_number":"171","publication":"The Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]}}]