[{"year":"2025","oa":1,"file":[{"file_id":"20680","success":1,"creator":"dernst","access_level":"open_access","relation":"main_file","date_created":"2025-11-24T13:18:34Z","file_size":39736710,"checksum":"11d35c1c52c000f8c14bc6de2e9f4b3f","content_type":"application/pdf","date_updated":"2025-11-24T13:18:34Z","file_name":"2025_AstrophysicalJour_Yue.pdf"}],"language":[{"iso":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"doi":"10.3847/2041-8213/ae0e0e","issue":"1","PlanS_conform":"1","has_accepted_license":"1","month":"11","isi":1,"arxiv":1,"DOAJ_listed":"1","acknowledgement":"We thank the referee for valuable 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 program ID #3117 and #4713. Support for\r\nthis 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\r\nAssociation of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","type":"journal_article","volume":993,"OA_place":"publisher","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","file_date_updated":"2025-11-24T13:18:34Z","publication":"The Astrophysical Journal Letters","OA_type":"gold","date_published":"2025-11-01T00:00:00Z","article_number":"L12","date_created":"2025-11-16T23:01:24Z","external_id":{"isi":["001600890100001"],"arxiv":["2507.05381"]},"title":"Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars","author":[{"first_name":"Minghao","last_name":"Yue","full_name":"Yue, Minghao"},{"last_name":"Eilers","first_name":"Anna Christina","full_name":"Eilers, Anna Christina"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"full_name":"Davies, Frederick B.","first_name":"Frederick B.","last_name":"Davies"},{"first_name":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"full_name":"Kashino, Daichi","first_name":"Daichi","last_name":"Kashino"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"last_name":"Simcoe","first_name":"Robert A.","full_name":"Simcoe, Robert A."}],"date_updated":"2026-02-16T12:45:16Z","abstract":[{"text":"Ionized proximity zones around luminous quasars provide a unique laboratory to characterize the Lyα emission lines from z > 6 galaxies without significant attenuation from the intergalactic medium (IGM). However, Lyα line measurements for galaxies within high-redshift quasars’ proximity zones have been rare so far. Here we present deep spectroscopic observations obtained with the NIRSpec/Micro-Shutter Assembly (MSA) instrument on the James Webb Space Telescope of galaxies in two z > 6 quasar fields. We measure the Lyα line fluxes for 50 galaxies at 6 < z < 7 with UV absolute magnitude M UV < −19 (median M UV = −19.97), among which 15 are located near the luminous quasars, i.e., within Δv < 2500 km s−1. We find that galaxies near the quasars show significant flux blueward of the systemic Lyα wavelength, and have higher Lyα equivalent width compared to galaxies at similar redshifts that are not located within the quasars’ environment. Our result indicates little or no redshift evolution for the Lyα emitter fraction from z ∼ 6.4 to z ∼ 5. Leveraging the low IGM opacity in the quasars’ vicinity, we evaluate the Lyα escape fraction (f esc Ly α) of high-redshift galaxies. Our analysis suggests that galaxies at 〈z〉 ≈ 6.4 have an average f esc Ly α = 0.14 ± 0.04. This value is consistent with reionization models where the Lyman continuum escape fraction is low ( fescLyC ≲ 0.1 ) for luminous galaxies, and where the most luminous galaxies have only a minor contribution to the total ionizing photon budget. © 2025. The Author(s). Published by the American Astronomical Society.","lang":"eng"}],"article_type":"original","scopus_import":"1","intvolume":" 993","department":[{"_id":"JoMa"}],"day":"01","_id":"20649","article_processing_charge":"Yes","oa_version":"Published Version","quality_controlled":"1","citation":{"chicago":"Yue, Minghao, Anna Christina Eilers, Jorryt J Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, and Robert A. Simcoe. “Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ae0e0e.","ama":"Yue M, Eilers AC, Matthee JJ, et al. Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars. The Astrophysical Journal Letters. 2025;993(1). doi:10.3847/2041-8213/ae0e0e","apa":"Yue, M., Eilers, A. C., Matthee, J. J., Naidu, R. P., Bordoloi, R., Davies, F. B., … Simcoe, R. A. (2025). Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae0e0e","short":"M. Yue, A.C. Eilers, J.J. Matthee, R.P. Naidu, R. Bordoloi, F.B. Davies, J.F. Hennawi, D. Kashino, R. Mackenzie, R.A. Simcoe, The Astrophysical Journal Letters 993 (2025).","mla":"Yue, Minghao, et al. “Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars.” The Astrophysical Journal Letters, vol. 993, no. 1, L12, IOP Publishing, 2025, doi:10.3847/2041-8213/ae0e0e.","ieee":"M. Yue et al., “Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars,” The Astrophysical Journal Letters, vol. 993, no. 1. IOP Publishing, 2025.","ista":"Yue M, Eilers AC, Matthee JJ, Naidu RP, Bordoloi R, Davies FB, Hennawi JF, Kashino D, Mackenzie R, Simcoe RA. 2025. Escape fractions from unattenuated Lyα emitters around luminous z > 6 quasars. The Astrophysical Journal Letters. 993(1), L12."},"ddc":["520"],"publisher":"IOP Publishing"},{"abstract":[{"text":"We used observations from the JWST Emission Line Survey (JELS) to measure the half-light radii (re) of 23 Hα-emitting starforming (SF) galaxies at z = 6.1 in the PRIMER/COSMOS field. Galaxy sizes were measured in JWST near-infrared camera observations in rest-frame Hα (tracing recent star formation) with the F466N and F470N narrow-band filters from JELS, and\r\ncompared against rest-R- and V -band (tracing established stellar populations) and near-ultraviolet sizes. We find a size–stellar mass(re − M∗) relationship with a slope that is consistent with literature values at lower redshifts, though offset to lowersizes. We observe a large scatter in re at low stellar mass (M∗ < 10^8.4 Mo) which we believe is the result of bursty star formation histories (SFHs) of SF galaxies at the Epoch of Reionization (EoR). We find that the stellar and ionized gas components are similar in size at z = 6.1. The evidence of already-established stellar components in these Hα emitters (HAEs) indicates previous episodes of star formation have occurred. As such, following other JELS studies finding our HAEs are undergoing a current burst of star formation, we believe our results indicate that SF galaxies at the end of the EoR have already experienced a bursty SFH. From our re − M∗ relationship, we find re,F444W = 0.76 ± 0.46 kpc for fixed stellar mass M∗ = 10^9.25 M, which is in agreement with other observations and simulations of SF galaxies in the literature. We find a close-pair (major) merger fraction of (fmaj. merger =0.44 ± 0.22) fmerger = 0.43 ± 0.11 for galaxy separations d <~ 25 kpc, which is in agreement with other z ≈ 6 studies.","lang":"eng"}],"date_updated":"2025-12-01T15:25:11Z","external_id":{"isi":["001611415800001"]},"date_created":"2025-11-23T23:01:37Z","author":[{"full_name":"Stephenson, H. M.O.","first_name":"H. M.O.","last_name":"Stephenson"},{"full_name":"Stott, J. P.","last_name":"Stott","first_name":"J. P."},{"first_name":"C. A.","last_name":"Pirie","full_name":"Pirie, C. A."},{"first_name":"K. J.","last_name":"Duncan","full_name":"Duncan, K. J."},{"full_name":"Mcleod, D. J.","first_name":"D. J.","last_name":"Mcleod"},{"full_name":"Best, P. N.","first_name":"P. N.","last_name":"Best"},{"last_name":"Brinch","first_name":"M.","full_name":"Brinch, M."},{"last_name":"Clausen","first_name":"M.","full_name":"Clausen, M."},{"last_name":"Cochrane","first_name":"R. K.","full_name":"Cochrane, R. K."},{"full_name":"Dunlop, J. S.","first_name":"J. S.","last_name":"Dunlop"},{"full_name":"Flury, S. R.","first_name":"S. R.","last_name":"Flury"},{"full_name":"Geach, J. E.","first_name":"J. E.","last_name":"Geach"},{"full_name":"Hale, C. L.","last_name":"Hale","first_name":"C. L."},{"full_name":"Ibar, E.","first_name":"E.","last_name":"Ibar"},{"full_name":"Li, Zefeng","last_name":"Li","first_name":"Zefeng"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Mclure, R. J.","first_name":"R. J.","last_name":"Mclure"},{"full_name":"Ossa-Fuentes, L.","last_name":"Ossa-Fuentes","first_name":"L."},{"full_name":"Patrick, A. L.","first_name":"A. L.","last_name":"Patrick"},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."}],"title":"The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization","OA_type":"gold","date_published":"2025-12-01T00:00:00Z","file_date_updated":"2025-11-24T10:35:15Z","publication":"Monthly Notices of the Royal Astronomical Society","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","publisher":"Oxford University Press","ddc":["520"],"citation":{"apa":"Stephenson, H. M. O., Stott, J. P., Pirie, C. A., Duncan, K. J., Mcleod, D. J., Best, P. N., … Swinbank, A. M. (2025). The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1725","ama":"Stephenson HMO, Stott JP, Pirie CA, et al. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 2025;544(2):1412-1431. doi:10.1093/mnras/staf1725","chicago":"Stephenson, H. M.O., J. P. Stott, C. A. Pirie, K. J. Duncan, D. J. Mcleod, P. N. Best, M. Brinch, et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1725.","ista":"Stephenson HMO, Stott JP, Pirie CA, Duncan KJ, Mcleod DJ, Best PN, Brinch M, Clausen M, Cochrane RK, Dunlop JS, Flury SR, Geach JE, Hale CL, Ibar E, Li Z, Matthee JJ, Mclure RJ, Ossa-Fuentes L, Patrick AL, Sobral D, Swinbank AM. 2025. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 544(2), 1412–1431.","ieee":"H. M. O. Stephenson et al., “The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization,” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2. Oxford University Press, pp. 1412–1431, 2025.","short":"H.M.O. Stephenson, J.P. Stott, C.A. Pirie, K.J. Duncan, D.J. Mcleod, P.N. Best, M. Brinch, M. Clausen, R.K. Cochrane, J.S. Dunlop, S.R. Flury, J.E. Geach, C.L. Hale, E. Ibar, Z. Li, J.J. Matthee, R.J. Mclure, L. Ossa-Fuentes, A.L. Patrick, D. Sobral, A.M. Swinbank, Monthly Notices of the Royal Astronomical Society 544 (2025) 1412–1431.","mla":"Stephenson, H. M. O., et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2, Oxford University Press, 2025, pp. 1412–31, doi:10.1093/mnras/staf1725."},"quality_controlled":"1","_id":"20660","article_processing_charge":"Yes","oa_version":"Published Version","day":"01","intvolume":" 544","department":[{"_id":"JoMa"}],"article_type":"original","scopus_import":"1","DOAJ_listed":"1","isi":1,"month":"12","issue":"2","doi":"10.1093/mnras/staf1725","has_accepted_license":"1","PlanS_conform":"1","page":"1412-1431","language":[{"iso":"eng"}],"file":[{"relation":"main_file","date_created":"2025-11-24T10:35:15Z","checksum":"ddb3f429d2246bbf536efb4b0e52f3a8","file_size":3625308,"content_type":"application/pdf","file_name":"2025_MonthlyNoticesRAS_Stephenson.pdf","date_updated":"2025-11-24T10:35:15Z","file_id":"20678","success":1,"creator":"dernst","access_level":"open_access"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"status":"public","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":544,"OA_place":"publisher","type":"journal_article","acknowledgement":"This work makes use of ASTROPY, 7 a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018, 2022), as well as the NUMPY (C. R. Harris et al. 2020) and SCIPY (P.Virtanen et al. 2020) packages(see also T. E. Oliphant 2007). All plots\r\nwere created using the MATPLOTLIB 2D graphics PYTHON package (J. D. Hunter 2007). Conversions between redshift and lookback time in our selected cosmological model were done using the Javascript cosmological calculator from E. L. Wright (2006).8 The authors would like to thank the anonymous referee for their constructive comments and suggestions which have strengthened the analysis of this work and improved the paper. The authors also gratefully acknowledge Ian Smail for providing valuable feedback and helping to guide the science of this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space\r\nTelescope. The data were obtained from the Mikulski Archive for Space Telescopes9 at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GO no. 2321 (JELS) and GO no. 1837 (PRIMER). The authors acknowledge the PRIMER team for developing their observing program with a zero-exclusive-access period. HMOS acknowledges support from an STFC PhD studentship and the Faculty of Science and Technology at Lancaster University. PNB is grateful for support from the UK STFC\r\nvia grants ST/V000594/1 and ST/Y000951/1. JSD acknowledges the support of the Royal Society via a Royal Society Research Professorship. LOF acknowledges funding by ANID BECAS/DOCTORADO NACIONAL 21220499.CLH acknowledges support from the Oxford\r\nHintze Centre for Astrophysical Surveys which is funded through generous support from the Hintze family charity foundation. EI gratefully acknowledge financial support from ANID – MILENIO –NCN2024 112 and ANID FONDECYT Regular 1221846. For the purpose of open access, the authors have applied a Creative Commons attribution (CC BY) licence to any author accepted manuscript version arising."},{"OA_place":"publisher","volume":544,"status":"public","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"acknowledgement":"This research was supported in part by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research was supported in part by The Dr Albert Shimmins Fund through the Albert Shimmins Postgraduate Writing Up Award (University of Melbourne). 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 programmes JWST-ERS-1324, JWST-GO-2561, and JWST-DDT-2756. BV and PW acknowledge support from the INAF Large Grant 2022 ‘Extragalactic Surveys with JWST’ (PI Pentericci), the INAF Mini\r\nGrant ‘1.05.24.07.01 RSN1: Spatially-Resolved Near-IR Emission of Intermediate-Redshift Jellyfish Galaxies’ (PI Watson), and are supported by the European Union – NextGenerationEU RFF M4C2 1.1 PRIN 2022 project 2022ZSL4BL INSIGHT. MB acknowledges support from the ERC Advanced Grant FIRSTLIGHT and Slovenian national research agency ARIS through grants N1-0238 and P1-0188. ","type":"journal_article","month":"12","DOAJ_listed":"1","arxiv":1,"isi":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"date_created":"2025-11-24T09:02:04Z","relation":"main_file","file_name":"2025_MonthlyNoticesRAS_Dalmasso.pdf","date_updated":"2025-11-24T09:02:04Z","checksum":"2caff0a3b81fed114408377323298b43","file_size":1952887,"content_type":"application/pdf","file_id":"20674","access_level":"open_access","creator":"dernst","success":1}],"language":[{"iso":"eng"}],"oa":1,"year":"2025","has_accepted_license":"1","page":"1915-1925","PlanS_conform":"1","issue":"2","doi":"10.1093/mnras/staf1837","ddc":["520"],"quality_controlled":"1","citation":{"chicago":"Dalmasso, Nicolò, Peter J. Watson, Tommaso Treu, Michele Trenti, Benedetta Vulcani, Themiya Nanayakkara, Maruša Bradač, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1837.","apa":"Dalmasso, N., Watson, P. J., Treu, T., Trenti, M., Vulcani, B., Nanayakkara, T., … Pentericci, L. (2025). Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1837","ama":"Dalmasso N, Watson PJ, Treu T, et al. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. Monthly Notices of the Royal Astronomical Society. 2025;544(2):1915-1925. doi:10.1093/mnras/staf1837","short":"N. Dalmasso, P.J. Watson, T. Treu, M. Trenti, B. Vulcani, T. Nanayakkara, M. Bradač, T. Jones, K. Boyett, X. Wang, S. Mascia, L. Pentericci, Monthly Notices of the Royal Astronomical Society 544 (2025) 1915–1925.","mla":"Dalmasso, Nicolò, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2, Oxford University Press, 2025, pp. 1915–25, doi:10.1093/mnras/staf1837.","ieee":"N. Dalmasso et al., “Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2. Oxford University Press, pp. 1915–1925, 2025.","ista":"Dalmasso N, Watson PJ, Treu T, Trenti M, Vulcani B, Nanayakkara T, Bradač M, Jones T, Boyett K, Wang X, Mascia S, Pentericci L. 2025. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. Monthly Notices of the Royal Astronomical Society. 544(2), 1915–1925."},"publisher":"Oxford University Press","department":[{"_id":"JoMa"}],"intvolume":" 544","article_type":"original","scopus_import":"1","article_processing_charge":"Yes","oa_version":"Published Version","_id":"20661","day":"01","author":[{"first_name":"Nicolò","last_name":"Dalmasso","full_name":"Dalmasso, Nicolò"},{"last_name":"Watson","first_name":"Peter J.","full_name":"Watson, Peter J."},{"first_name":"Tommaso","last_name":"Treu","full_name":"Treu, Tommaso"},{"last_name":"Trenti","first_name":"Michele","full_name":"Trenti, Michele"},{"full_name":"Vulcani, Benedetta","last_name":"Vulcani","first_name":"Benedetta"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Maruša","last_name":"Bradač","full_name":"Bradač, Maruša"},{"full_name":"Jones, Tucker","last_name":"Jones","first_name":"Tucker"},{"first_name":"Kristan","last_name":"Boyett","full_name":"Boyett, Kristan"},{"first_name":"Xin","last_name":"Wang","full_name":"Wang, Xin"},{"first_name":"Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"full_name":"Pentericci, Laura","first_name":"Laura","last_name":"Pentericci"}],"title":"Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies","external_id":{"arxiv":["2510.27036"],"isi":["001615620500001"]},"date_created":"2025-11-23T23:01:38Z","abstract":[{"lang":"eng","text":"We analyse James Webb Space Telescope (JWST) Near Infrared Imager and Slitless Spectrograph (NIRISS) and Near Infrared Spectrograph (NIRSpec) spectroscopic observations in the Abell 2744 galaxy cluster field. From approximately 120 candidates, we identify 12 objects with at least two prominent emission lines among [O II] λ3727, H β λ4861, [O III] λ4959, [O III] λ5007, and H α λ6563 that are spectroscopically confirmed by both instruments. Our key findings reveal systematic differences between the two spectrographs based on source morphology and shutter aperture placement. Compact objects show comparable or higher\r\nintegrated flux in NIRSpec relative to NIRISS (within 1σ uncertainties), while extended sources consistently display higher flux in NIRISS measurements. This pattern reflects NIRSpec’s optimal coverage for compact objects while potentially undersampling extended sources. Quantitative analysis demonstrates that NIRSpec recovers at least 63 per cent of NIRISS-measured flux when the slit covers >15 per cent of the source or when Re < 1 kpc. For lower coverage or larger effective radii, the recovered flux varies from 24 per cent to 63 per cent. When studying the H α λ6563/[O III] λ5007 emission line ratio, we observe that\r\nmeasurements from these different spectrographs can vary by up to ∼0.3 dex, with significant implications for metallicity and star formation rate characterizations for individual galaxies. These results highlight the importance of considering instrumental effects when combining multi-instrument spectroscopic data and demonstrate that source morphology critically influences flux\r\nrecovery between slit-based and slitless spectroscopic modes in JWST observations."}],"date_updated":"2025-12-01T15:23:21Z","file_date_updated":"2025-11-24T09:02:04Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2025-12-01T00:00:00Z","OA_type":"gold"},{"_id":"18854","article_processing_charge":"No","oa_version":"Published Version","day":"06","intvolume":" 693","department":[{"_id":"JoMa"}],"article_type":"original","scopus_import":"1","publisher":"EDP Sciences","ddc":["520"],"quality_controlled":"1","citation":{"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 & Astrophysics. 693, A60.","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 & Astrophysics 693 (2025).","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.” Astronomy & Astrophysics, vol. 693, A60, EDP Sciences, 2025, doi:10.1051/0004-6361/202450243.","ieee":"K. E. Heintz 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,” Astronomy & Astrophysics, vol. 693. EDP Sciences, 2025.","ama":"Heintz KE, Brammer GB, Watson D, et al. The JWST-PRIMAL archival survey: A JWST/NIRSpec reference sample for the physical properties and Lyman-α absorption and emission of ∼600 galaxies at z = 5.0-13.4. Astronomy & Astrophysics. 2025;693. doi:10.1051/0004-6361/202450243","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202450243","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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202450243."},"article_number":"A60","OA_type":"diamond","date_published":"2025-01-06T00:00:00Z","file_date_updated":"2025-01-20T09:17:33Z","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","abstract":[{"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.","lang":"eng"}],"date_updated":"2026-02-16T12:07:37Z","external_id":{"isi":["001390856800001"]},"date_created":"2025-01-19T23:01:52Z","author":[{"full_name":"Heintz, K. E.","last_name":"Heintz","first_name":"K. E."},{"full_name":"Brammer, G. B.","first_name":"G. B.","last_name":"Brammer"},{"last_name":"Watson","first_name":"D.","full_name":"Watson, D."},{"last_name":"Oesch","first_name":"P. A.","full_name":"Oesch, P. A."},{"full_name":"Keating, L. C.","last_name":"Keating","first_name":"L. C."},{"last_name":"Hayes","first_name":"M. J.","full_name":"Hayes, M. J."},{"first_name":"Unknown","last_name":"Abdurro'Uf","full_name":"Abdurro'Uf, Unknown"},{"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."},{"first_name":"C. R.","last_name":"Christiansen","full_name":"Christiansen, C. R."},{"full_name":"Cullen, F.","last_name":"Cullen","first_name":"F."},{"full_name":"Davé, R.","first_name":"R.","last_name":"Davé"},{"full_name":"Dayal, P.","first_name":"P.","last_name":"Dayal"},{"last_name":"Ferrara","first_name":"A.","full_name":"Ferrara, A."},{"last_name":"Finlator","first_name":"K.","full_name":"Finlator, K."},{"full_name":"Fynbo, J. P.U.","last_name":"Fynbo","first_name":"J. P.U."},{"full_name":"Flury, S. R.","first_name":"S. R.","last_name":"Flury"},{"full_name":"Gelli, V.","last_name":"Gelli","first_name":"V."},{"last_name":"Gillman","first_name":"S.","full_name":"Gillman, S."},{"full_name":"Gottumukkala, R.","first_name":"R.","last_name":"Gottumukkala"},{"full_name":"Gould, K.","first_name":"K.","last_name":"Gould"},{"first_name":"T. R.","last_name":"Greve","full_name":"Greve, T. R."},{"first_name":"S. E.","last_name":"Hardin","full_name":"Hardin, S. E."},{"full_name":"Hsiao, T. Y.Y.","last_name":"Hsiao","first_name":"T. Y.Y."},{"first_name":"A.","last_name":"Hutter","full_name":"Hutter, A."},{"first_name":"P.","last_name":"Jakobsson","full_name":"Jakobsson, P."},{"full_name":"Killi, M.","first_name":"M.","last_name":"Killi"},{"last_name":"Khosravaninezhad","first_name":"N.","full_name":"Khosravaninezhad, N."},{"full_name":"Laursen, P.","first_name":"P.","last_name":"Laursen"},{"last_name":"Lee","first_name":"M. M.","full_name":"Lee, M. M."},{"first_name":"G. E.","last_name":"Magdis","full_name":"Magdis, G. E."},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Naidu, R. P.","last_name":"Naidu","first_name":"R. P."},{"first_name":"D.","last_name":"Narayanan","full_name":"Narayanan, D."},{"full_name":"Pollock, C.","last_name":"Pollock","first_name":"C."},{"last_name":"Prescott","first_name":"M. K.M.","full_name":"Prescott, M. K.M."},{"last_name":"Rusakov","first_name":"V.","full_name":"Rusakov, V."},{"first_name":"M.","last_name":"Shuntov","full_name":"Shuntov, M."},{"full_name":"Sneppen, A.","last_name":"Sneppen","first_name":"A."},{"first_name":"R.","last_name":"Smit","full_name":"Smit, R."},{"full_name":"Tanvir, N. R.","last_name":"Tanvir","first_name":"N. R."},{"first_name":"C.","last_name":"Terp","full_name":"Terp, C."},{"full_name":"Toft, S.","first_name":"S.","last_name":"Toft"},{"full_name":"Valentino, F.","first_name":"F.","last_name":"Valentino"},{"full_name":"Vijayan, A. P.","first_name":"A. P.","last_name":"Vijayan"},{"full_name":"Weaver, J. R.","last_name":"Weaver","first_name":"J. R."},{"full_name":"Wise, J. H.","last_name":"Wise","first_name":"J. H."},{"full_name":"Witstok, J.","last_name":"Witstok","first_name":"J."}],"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","type":"journal_article","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).","status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":693,"OA_place":"publisher","doi":"10.1051/0004-6361/202450243","has_accepted_license":"1","file":[{"file_name":"2025_AstronomyAstrophysics_Heintz.pdf","date_updated":"2025-01-20T09:17:33Z","checksum":"67a791080ade9bfb449d249de2af7456","file_size":4513466,"content_type":"application/pdf","date_created":"2025-01-20T09:17:33Z","relation":"main_file","access_level":"open_access","creator":"dernst","success":1,"file_id":"18858"}],"language":[{"iso":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"isi":1,"month":"01"},{"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"author":[{"full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens","first_name":"Adélaïde"},{"full_name":"Adamo, Angela","first_name":"Angela","last_name":"Adamo"},{"first_name":"Matteo","last_name":"Messa","full_name":"Messa, Matteo"},{"first_name":"Miroslava","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","first_name":"Ivan","last_name":"Kramarenko"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."}],"title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","external_id":{"arxiv":["2410.10974"],"isi":["001420026000001"]},"date_created":"2025-02-23T23:01:55Z","date_updated":"2026-02-16T11:51:48Z","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"}],"publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file_date_updated":"2025-02-25T06:38:43Z","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2025-03-01T00:00:00Z","OA_type":"gold","citation":{"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.","mla":"Claeyssens, Adélaïde, et al. “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, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:10.1093/mnras/staf058.","ieee":"A. Claeyssens et al., “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, 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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf058.","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. Monthly Notices of the Royal Astronomical Society. 2025;537(3):2535-2558. doi:10.1093/mnras/staf058","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf058"},"quality_controlled":"1","ddc":["520"],"publisher":"Oxford University Press","scopus_import":"1","article_type":"original","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"intvolume":" 537","day":"01","article_processing_charge":"No","oa_version":"Published Version","_id":"19066","month":"03","arxiv":1,"isi":1,"DOAJ_listed":"1","oa":1,"year":"2025","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"date_updated":"2025-02-25T06:38:43Z","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf","content_type":"application/pdf","file_size":35099276,"checksum":"431aef05755e6b5472f5e9b4c326cf84","date_created":"2025-02-25T06:38:43Z","relation":"main_file","access_level":"open_access","creator":"dernst","success":1,"file_id":"19084"}],"language":[{"iso":"eng"}],"page":"2535-2558","has_accepted_license":"1","issue":"3","doi":"10.1093/mnras/staf058","OA_place":"publisher","volume":537,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","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.","type":"journal_article"},{"abstract":[{"text":"Context. The hydrogen Lyman-alpha (Lyα) line, the brightest rest-frame ultraviolet line of high-redshift galaxies, exhibits a large variety of shapes, which is due to factors at different scales, from the interstellar medium to the intergalactic medium (IGM).\r\nAims. The aim of this work is to provide a systematic inventory and classification of the spectral shapes of Lyα emission lines to better understand the general population of high-redshift Lyα emitting galaxies (LAEs).\r\nMethods. Using the unprecedentedly deep data from the MUSE eXtremely Deep Field (MXDF; up to 140 hour exposure time), we selected 477 galaxies observed in the ∼2.8−6.6 redshift range, 15 of which have a systemic redshift from nebular lines. We developed a method to classify Lyα emission lines in four spectral and three spatial categories by combining a pure spectral analysis with a narrow-band image analysis. We measured spectral properties, such as the peak separation and the blue-to-total flux ratio for the double-peaked galaxies.\r\nResults. To ensure a robust sample for statistical analysis, we define two unbiased subsets, inclusive and restrictive, by applying thresholds for signal-to-noise ratio, peak separation, and Lyα luminosity, yielding a final unbiased sample of 206 galaxies. Our analysis reveals that between 32% and 51% of the galaxies exhibit double-peaked profiles, with peak separations ranging from 150 km s−1 to nearly 1600 km s−1. The fraction of double-peaked galaxies seems to evolve dependently with the Lyα luminosity, while we do not see a severe decrease in this fraction with redshift, which is expected given the IGM attenuation at high redshift. An artificial increase in the number of double-peaked galaxies at the highest redshifts may cause the observation of a plateau instead of a decrease. A notable number of these double-peaked profiles show blue-dominated spectra, suggesting unique gas dynamics and inflow characteristics in some high-redshift galaxies. The consequent fraction of blue-dominated spectra needs to be confirmed by obtaining new systemic redshift measurements. Among the double-peaked galaxies, 4% are spurious detections, that is, the blue and red peaks do not come from the same spatial location. Around 20% out of the 477 sources of the parent sample lie in a complex environment, meaning there are other clumps or galaxies at the same redshift within a distance of 30 kpc.\r\nConclusions. Our results suggest that the double-peaked LAE fraction may trace the evolution of IGM attenuation, but the faintest galaxies must be observed at high redshift. We also need more data to confirm the trend seen at low redshift. In addition, it is crucial to obtain secure systemic redshifts for LAEs to better constrain the nature of the Lyα double-peaked lines. Statistical samples of double-peaked and triple-peaked galaxies are a promising probe of the evolution of the physical properties of galaxies across cosmic time.","lang":"eng"}],"date_updated":"2026-02-16T12:08:40Z","author":[{"full_name":"Vitte, Eloïse","first_name":"Eloïse","last_name":"Vitte"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"full_name":"Hibon, Pascale","first_name":"Pascale","last_name":"Hibon"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Alcalde Pampliega, Belén","first_name":"Belén","last_name":"Alcalde Pampliega"},{"last_name":"Kerutt","first_name":"Josephine","full_name":"Kerutt, Josephine"},{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Guo, Yucheng","first_name":"Yucheng","last_name":"Guo"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"last_name":"Pharo","first_name":"John","full_name":"Pharo, John"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"last_name":"Boogaard","first_name":"Leindert","full_name":"Boogaard, Leindert"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Thierry","last_name":"Contini","full_name":"Contini, Thierry"}],"title":"The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies","date_created":"2025-02-23T23:01:56Z","external_id":{"isi":["001417357000009"]},"article_number":"A100","date_published":"2025-02-01T00:00:00Z","OA_type":"hybrid","publication":"Astronomy & Astrophysics","file_date_updated":"2025-02-25T07:19:34Z","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","ddc":["520"],"quality_controlled":"1","citation":{"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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202450426.","ama":"Vitte E, Verhamme A, Hibon P, et al. The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies. Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202450426","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202450426","ieee":"E. Vitte et al., “The MUSE eXtremely Deep Field: Classifying the spectral shapes of Ly α -emitting galaxies,” Astronomy & Astrophysics, vol. 694. EDP Sciences, 2025.","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 & Astrophysics 694 (2025).","mla":"Vitte, Eloïse, et al. “The MUSE EXtremely Deep Field: Classifying the Spectral Shapes of Ly α -Emitting Galaxies.” Astronomy & Astrophysics, vol. 694, A100, EDP Sciences, 2025, doi:10.1051/0004-6361/202450426.","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 & Astrophysics. 694, A100."},"oa_version":"Published Version","article_processing_charge":"No","_id":"19069","day":"01","department":[{"_id":"JoMa"}],"intvolume":" 694","scopus_import":"1","article_type":"original","isi":1,"month":"02","has_accepted_license":"1","doi":"10.1051/0004-6361/202450426","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"date_created":"2025-02-25T07:19:34Z","relation":"main_file","date_updated":"2025-02-25T07:19:34Z","file_name":"2025_AstronomyAstrophysics_Vitte.pdf","file_size":3444203,"checksum":"ed2a5bba313e54ed250be348bd8c1d95","content_type":"application/pdf","file_id":"19087","access_level":"open_access","creator":"dernst","success":1}],"language":[{"iso":"eng"}],"oa":1,"year":"2025","status":"public","publication_identifier":{"issnl":["0004-6361"],"eissn":["1432-0746"],"issn":["0004-6361"]},"OA_place":"publisher","volume":694,"type":"journal_article","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)."},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","file_date_updated":"2025-02-25T07:05:19Z","publication":"Astronomy & Astrophysics","OA_type":"diamond","date_published":"2025-02-01T00:00:00Z","article_number":"A82","date_created":"2025-02-23T23:01:56Z","external_id":{"isi":["001414753300028"]},"author":[{"full_name":"Sawant, P.","first_name":"P.","last_name":"Sawant"},{"full_name":"Nanni, A.","first_name":"A.","last_name":"Nanni"},{"full_name":"Romano, M.","first_name":"M.","last_name":"Romano"},{"first_name":"D.","last_name":"Donevski","full_name":"Donevski, D."},{"full_name":"Bruzual, G.","last_name":"Bruzual","first_name":"G."},{"last_name":"Ysard","first_name":"N.","full_name":"Ysard, N."},{"last_name":"Lemaux","first_name":"B. C.","full_name":"Lemaux, B. C."},{"last_name":"Inami","first_name":"H.","full_name":"Inami, H."},{"full_name":"Calura, F.","last_name":"Calura","first_name":"F."},{"last_name":"Pozzi","first_name":"F.","full_name":"Pozzi, F."},{"first_name":"K.","last_name":"Małek","full_name":"Małek, K."},{"first_name":"J.","last_name":"Junais","full_name":"Junais, 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.","first_name":"M.","last_name":"Hamed"},{"full_name":"Ginolfi, M.","first_name":"M.","last_name":"Ginolfi"},{"last_name":"Zamorani","first_name":"G.","full_name":"Zamorani, G."},{"last_name":"Lorenzon","first_name":"G.","full_name":"Lorenzon, G."},{"first_name":"J.","last_name":"Molina","full_name":"Molina, J."},{"full_name":"Bardelli, S.","last_name":"Bardelli","first_name":"S."},{"last_name":"Ibar","first_name":"E.","full_name":"Ibar, E."},{"last_name":"Vergani","first_name":"D.","full_name":"Vergani, D."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare","first_name":"Claudia"},{"last_name":"Béthermin","first_name":"M.","full_name":"Béthermin, M."},{"first_name":"D.","last_name":"Burgarella","full_name":"Burgarella, D."},{"full_name":"Cassata, P.","first_name":"P.","last_name":"Cassata"},{"first_name":"M.","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, M."},{"last_name":"D'Onghia","first_name":"E.","full_name":"D'Onghia, E."},{"first_name":"Y.","last_name":"Dubois","full_name":"Dubois, Y."},{"first_name":"G. E.","last_name":"Magdis","full_name":"Magdis, G. E."},{"full_name":"Mendez-Hernandez, H.","last_name":"Mendez-Hernandez","first_name":"H."}],"title":"The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies","date_updated":"2026-02-16T12:08:24Z","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"}],"article_type":"original","scopus_import":"1","intvolume":" 694","department":[{"_id":"JoMa"}],"day":"01","_id":"19070","article_processing_charge":"Yes","oa_version":"Published Version","citation":{"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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202451542.","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202451542","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. Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202451542","mla":"Sawant, P., et al. “The ALPINE-ALMA [CII] Survey: Unveiling the Baryon Evolution in the Interstellar Medium of z ∼ 5 Star-Forming Galaxies.” Astronomy & Astrophysics, vol. 694, A82, EDP Sciences, 2025, doi:10.1051/0004-6361/202451542.","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 & Astrophysics 694 (2025).","ieee":"P. Sawant et al., “The ALPINE-ALMA [CII] survey: Unveiling the baryon evolution in the interstellar medium of z ∼ 5 star-forming galaxies,” Astronomy & Astrophysics, 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 & Astrophysics. 694, A82."},"quality_controlled":"1","ddc":["520"],"publisher":"EDP Sciences","year":"2025","oa":1,"language":[{"iso":"eng"}],"file":[{"success":1,"creator":"dernst","access_level":"open_access","file_id":"19086","checksum":"792cbcda14148c352dc8c5a26058827d","file_size":7624067,"content_type":"application/pdf","file_name":"2025_AstronomyAstrophysics_Sawant.pdf","date_updated":"2025-02-25T07:05:19Z","relation":"main_file","date_created":"2025-02-25T07:05:19Z"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"doi":"10.1051/0004-6361/202451542","has_accepted_license":"1","month":"02","isi":1,"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.","type":"journal_article","volume":694,"OA_place":"publisher","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"status":"public"},{"ddc":["520"],"citation":{"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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202452363.","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. Astronomy & Astrophysics. 2025;694. doi:10.1051/0004-6361/202452363","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202452363","ieee":"A. Covelo-Paz et al., “An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy,” Astronomy & Astrophysics, vol. 694. EDP Sciences, 2025.","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 & 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.” Astronomy & Astrophysics, vol. 694, A178, EDP Sciences, 2025, doi:10.1051/0004-6361/202452363.","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 & Astrophysics. 694, A178."},"quality_controlled":"1","publisher":"EDP Sciences","department":[{"_id":"JoMa"}],"intvolume":" 694","scopus_import":"1","article_type":"original","article_processing_charge":"No","oa_version":"Published Version","_id":"19284","day":"12","author":[{"full_name":"Covelo-Paz, Alba","first_name":"Alba","last_name":"Covelo-Paz"},{"last_name":"Giovinazzo","first_name":"Emma","full_name":"Giovinazzo, Emma"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"first_name":"Romain A.","last_name":"Meyer","full_name":"Meyer, Romain A."},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"last_name":"Fudamoto","first_name":"Yoshinobu","full_name":"Fudamoto, Yoshinobu"},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"first_name":"Jamie","last_name":"Lin","full_name":"Lin, Jamie"},{"full_name":"Matharu, Jasleen","last_name":"Matharu","first_name":"Jasleen"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Anna","last_name":"Velichko","full_name":"Velichko, Anna"},{"first_name":"Victoria","last_name":"Bollo","full_name":"Bollo, Victoria"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"last_name":"Illingworth","first_name":"Garth D.","full_name":"Illingworth, Garth D."},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","first_name":"Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048"},{"full_name":"Magee, Daniel","first_name":"Daniel","last_name":"Magee"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Nelson, Erica","first_name":"Erica","last_name":"Nelson"},{"full_name":"Reddy, Naveen","last_name":"Reddy","first_name":"Naveen"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"last_name":"Stefanon","first_name":"Mauro","full_name":"Stefanon, Mauro"},{"last_name":"Xiao","first_name":"Mengyuan","full_name":"Xiao, Mengyuan"}],"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"]},"date_created":"2025-03-02T23:01:54Z","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."}],"date_updated":"2026-02-16T12:08:59Z","publication":"Astronomy & Astrophysics","file_date_updated":"2025-03-04T09:29:01Z","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A178","date_published":"2025-02-12T00:00:00Z","OA_type":"diamond","OA_place":"publisher","volume":694,"status":"public","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"acknowledgement":"This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with 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.","type":"journal_article","month":"02","arxiv":1,"isi":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"language":[{"iso":"eng"}],"file":[{"date_created":"2025-03-04T09:29:01Z","relation":"main_file","content_type":"application/pdf","checksum":"b1e74644a0cd37550e9a553f8675c93f","file_size":1865856,"date_updated":"2025-03-04T09:29:01Z","file_name":"2025_AstronomyAstrophysics_CoveloPaz.pdf","file_id":"19285","access_level":"open_access","success":1,"creator":"dernst"}],"oa":1,"year":"2025","has_accepted_license":"1","related_material":{"link":[{"relation":"software","url":" https://github.com/astroalba/fresco"}]},"doi":"10.1051/0004-6361/202452363"},{"oa":1,"year":"2025","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"language":[{"iso":"eng"}],"file":[{"date_created":"2025-03-10T11:54:52Z","relation":"main_file","file_size":1194131,"content_type":"application/pdf","checksum":"1d33a8eb59f42a0c7a943c8859e9b883","date_updated":"2025-03-10T11:54:52Z","file_name":"2025_AstrophysicalJour_Banerjee.pdf","file_id":"19379","access_level":"open_access","success":1,"creator":"dernst"}],"has_accepted_license":"1","doi":"10.3847/1538-4357/ada7e9","issue":"2","month":"02","isi":1,"DOAJ_listed":"1","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).","type":"journal_article","OA_place":"publisher","volume":980,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"status":"public","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"The Astrophysical Journal","file_date_updated":"2025-03-10T11:54:52Z","date_published":"2025-02-20T00:00:00Z","OA_type":"gold","article_number":"171","author":[{"first_name":"Eshita","last_name":"Banerjee","full_name":"Banerjee, Eshita"},{"first_name":"Sowgat","last_name":"Muzahid","full_name":"Muzahid, Sowgat"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"first_name":"Nicolas","last_name":"Bouché","full_name":"Bouché, Nicolas"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Johnson, Sean D.","last_name":"Johnson","first_name":"Sean D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"}],"title":"MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3","external_id":{"isi":["001421001500001"]},"date_created":"2025-03-09T23:01:26Z","date_updated":"2026-02-16T12:42:00Z","abstract":[{"text":"We present a comprehensive analysis of H i absorption around 96 Lyα emitters (LAEs) at z ≈ 3.3 (median Lyα luminosity ≈1042 erg s−1). These LAEs were identified within eight MUSE fields, each (math. formular) on the sky and centered on a bright background quasar, as part of the MUSEQuBES survey. Using Voigt profile fitting for all H i absorbers detected within ±500 km s−1 of these LAEs, we compiled a catalog of 800 H i absorption components. Our analysis shows that H i absorption is enhanced near the LAEs compared to the intergalactic medium. However, no trend is found between the column densities of H i absorbers and their impact parameters from the LAEs (spanning ≈54–260 pkpc). Additionally, all galaxies associated with Lyman-limit systems have impact parameters >50 pkpc from the quasar sightlines, suggesting that true absorber hosts may be too faint to detect. The LAEs show an overall H i covering fraction (fc(H i)) of ≈88% for a threshold (math. formular) (H i) = 15. Notably, at the same threshold, the LAEs in pairs/groups exhibit a 100% H i covering fraction out to ≈250 pkpc. In contrast, isolated LAEs consistently show a lower fc(H i) of ≈80%. This environmental influence on fc(H i) is also evident up to ≈300 km s−1 in differential bins of line-of-sight velocity. We find an anticorrelation between fc(H i) and the equivalent width of rest-frame Lyα emission (EW0). Based on the Lyα shell model, this could imply that gas-rich galaxies tend to reside in gas-rich environments or that the LAEs with higher EW0 are more efficient at ionizing their surrounding medium.","lang":"eng"}],"scopus_import":"1","article_type":"original","department":[{"_id":"JoMa"}],"intvolume":" 980","day":"20","article_processing_charge":"Yes","oa_version":"Published Version","_id":"19365","quality_controlled":"1","citation":{"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 et al., “MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3,” The Astrophysical Journal, vol. 980, no. 2. IOP Publishing, 2025.","mla":"Banerjee, Eshita, et al. “MUSEQuBES: Connecting H i Absorption with Lyα Emitters at z ≈ 3.3.” The Astrophysical Journal, vol. 980, no. 2, 171, IOP Publishing, 2025, doi:10.3847/1538-4357/ada7e9.","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).","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. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ada7e9","ama":"Banerjee E, Muzahid S, Schaye J, et al. MUSEQuBES: Connecting H i Absorption with Lyα emitters at z ≈ 3.3. The Astrophysical Journal. 2025;980(2). doi:10.3847/1538-4357/ada7e9","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.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ada7e9."},"ddc":["520"],"publisher":"IOP Publishing"},{"tmp":{"name":"Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)","short":"CC BY-NC-ND (4.0)","image":"/images/cc_by_nc_nd.png","legal_code_url":"https://creativecommons.org/licenses/by-nc-nd/4.0/legalcode"},"file":[{"file_id":"20134","access_level":"open_access","creator":"dernst","success":1,"date_created":"2025-08-05T12:49:36Z","relation":"main_file","file_name":"2025_NatureAstronomy_Wang.pdf","date_updated":"2025-08-05T12:49:36Z","checksum":"a0e65fe3374bd755b18ba03fd5e42a3f","content_type":"application/pdf","file_size":4912850}],"language":[{"iso":"eng"}],"oa":1,"year":"2025","page":"710-719","has_accepted_license":"1","doi":"10.1038/s41550-025-02500-2","license":"https://creativecommons.org/licenses/by-nc-nd/4.0/","month":"03","arxiv":1,"isi":1,"acknowledgement":"We thank B. Wang, P. Madau, M. Dotti, A. de la Vega, Y. Guo, C. Bacchini, Z. Cai, C. Conselice, A. Dekel, S. Faber, F. Fraternali, L. Ho, F. Jiang, S. Kassin, D. Koo, N. Mandelker, S. Mao and D. Xu for the valuable and insightful discussions regarding the research topics relevant to this paper. This project was supported by the European Research Council (ERC) Consolidator Grant no. 864361 (CosmicWeb). A.P. acknowledges the support from Fondazione Cariplo grant no. 2020-0902. M.V.M. acknowledges funding from NASA by means of HST-GO-17065. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programme no. 1835. Support for programme no. 1835 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 is 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 5-26555. These observations are associated with programme 17065. 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. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. This work is also based on observations collected at the European Southern Observatory under ESO programme 110.23ZX.","type":"journal_article","OA_place":"publisher","volume":9,"status":"public","publication_identifier":{"eissn":["2397-3366"]},"file_date_updated":"2025-08-05T12:49:36Z","publication":"Nature Astronomy","publication_status":"published","pmid":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2025-03-17T00:00:00Z","OA_type":"hybrid","author":[{"full_name":"Wang, Weichen","last_name":"Wang","first_name":"Weichen"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Pensabene, Antonio","last_name":"Pensabene","first_name":"Antonio"},{"full_name":"Galbiati, Marta","first_name":"Marta","last_name":"Galbiati"},{"full_name":"Travascio, Andrea","first_name":"Andrea","last_name":"Travascio"},{"first_name":"Charles C.","last_name":"Steidel","full_name":"Steidel, Charles C."},{"full_name":"Maseda, Michael V.","last_name":"Maseda","first_name":"Michael V."},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"full_name":"De Beer, Stephanie","first_name":"Stephanie","last_name":"De Beer"},{"full_name":"Fossati, Matteo","first_name":"Matteo","last_name":"Fossati"},{"full_name":"Fumagalli, Michele","first_name":"Michele","last_name":"Fumagalli"},{"full_name":"Gallego, Sofia G.","last_name":"Gallego","first_name":"Sofia G."},{"last_name":"Lazeyras","first_name":"Titouan","full_name":"Lazeyras, Titouan"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Quadri, Giada","first_name":"Giada","last_name":"Quadri"}],"title":"A giant disk galaxy two billion years after the Big Bang","date_created":"2025-04-06T22:01:32Z","external_id":{"isi":["001447477100001"],"arxiv":["2409.17956"],"pmid":["40417329"]},"abstract":[{"lang":"eng","text":"Observational studies have shown that galaxy disks were already in place in the first few billion years of the Universe. The early disks detected so far, with typical half-light radii of 3 kpc at stellar masses around 1011 M⊙ for redshift z ≈ 3, are significantly smaller than today’s disks with similar masses, which is in agreement with expectations from current galaxy models. Here we report observations of a giant disk at z = 3.25, when the Universe was only two billion years old, with a half-light radius of 9.6 kpc and stellar mass of (math formular). This galaxy is larger than any other kinematically confirmed disks at similar epochs and is surprisingly similar to today’s largest disks with regard to size and mass. James Webb Space Telescope imaging and spectroscopy reveal its spiral morphology and a rotational velocity consistent with a local Tully–Fisher relationship. Multiwavelength observations show that it lies in an exceptionally dense environment, where the galaxy number density is more than ten times higher than the cosmic average and mergers are frequent. The discovery of such a giant disk suggests the presence of favourable physical conditions for large-disk formation in dense environments in the early Universe, which may include efficient accretion of gas carrying coherent angular momentum and non-destructive mergers between exceptionally gas-rich progenitor galaxies."}],"date_updated":"2025-09-30T11:25:14Z","department":[{"_id":"JoMa"}],"intvolume":" 9","scopus_import":"1","article_type":"original","oa_version":"Published Version","article_processing_charge":"No","_id":"19504","day":"17","ddc":["520"],"citation":{"ista":"Wang W, Cantalupo S, Pensabene A, Galbiati M, Travascio A, Steidel CC, Maseda MV, Pezzulli G, De Beer S, Fossati M, Fumagalli M, Gallego SG, Lazeyras T, Mackenzie R, Matthee JJ, Nanayakkara T, Quadri G. 2025. A giant disk galaxy two billion years after the Big Bang. Nature Astronomy. 9, 710–719.","ieee":"W. Wang et al., “A giant disk galaxy two billion years after the Big Bang,” Nature Astronomy, vol. 9. Springer Nature, pp. 710–719, 2025.","mla":"Wang, Weichen, et al. “A Giant Disk Galaxy Two Billion Years after the Big Bang.” Nature Astronomy, vol. 9, Springer Nature, 2025, pp. 710–19, doi:10.1038/s41550-025-02500-2.","short":"W. Wang, S. Cantalupo, A. Pensabene, M. Galbiati, A. Travascio, C.C. Steidel, M.V. Maseda, G. Pezzulli, S. De Beer, M. Fossati, M. Fumagalli, S.G. Gallego, T. Lazeyras, R. Mackenzie, J.J. Matthee, T. Nanayakkara, G. Quadri, Nature Astronomy 9 (2025) 710–719.","apa":"Wang, W., Cantalupo, S., Pensabene, A., Galbiati, M., Travascio, A., Steidel, C. C., … Quadri, G. (2025). A giant disk galaxy two billion years after the Big Bang. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-025-02500-2","ama":"Wang W, Cantalupo S, Pensabene A, et al. A giant disk galaxy two billion years after the Big Bang. Nature Astronomy. 2025;9:710-719. doi:10.1038/s41550-025-02500-2","chicago":"Wang, Weichen, Sebastiano Cantalupo, Antonio Pensabene, Marta Galbiati, Andrea Travascio, Charles C. Steidel, Michael V. Maseda, et al. “A Giant Disk Galaxy Two Billion Years after the Big Bang.” Nature Astronomy. Springer Nature, 2025. https://doi.org/10.1038/s41550-025-02500-2."},"quality_controlled":"1","publisher":"Springer Nature"},{"publisher":"IOP Publishing","ddc":["520"],"quality_controlled":"1","citation":{"ama":"Weibel A, De Graaff A, Setton DJ, et al. RUBIES reveals a massive quiescent galaxy at z = 7.3. The Astrophysical Journal. 2025;983(1). doi:10.3847/1538-4357/adab7a","apa":"Weibel, A., De Graaff, A., Setton, D. J., Miller, T. B., Oesch, P. A., Brammer, G., … Wang, B. (2025). RUBIES reveals a massive quiescent galaxy at z = 7.3. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/adab7a","chicago":"Weibel, Andrea, Anna De Graaff, David J. Setton, Tim B. Miller, Pascal A. Oesch, Gabriel Brammer, Claudia D.P. Lagos, et al. “RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/adab7a.","ista":"Weibel A, De Graaff A, Setton DJ, Miller TB, Oesch PA, Brammer G, Lagos CDP, Whitaker KE, Williams CC, Baggen JFW, Bezanson R, Boogaard LA, Cleri NJ, Greene JE, Hirschmann M, Hviding RE, Kuruvanthodi A, Labbé I, Leja J, Maseda MV, Matthee JJ, Mcconachie I, Naidu RP, Roberts-Borsani G, Schaerer D, Suess KA, Valentino F, Van Dokkum P, Wang B. 2025. RUBIES reveals a massive quiescent galaxy at z = 7.3. The Astrophysical Journal. 983(1), 11.","ieee":"A. Weibel et al., “RUBIES reveals a massive quiescent galaxy at z = 7.3,” The Astrophysical Journal, vol. 983, no. 1. IOP Publishing, 2025.","short":"A. Weibel, A. De Graaff, D.J. Setton, T.B. Miller, P.A. Oesch, G. Brammer, C.D.P. Lagos, K.E. Whitaker, C.C. Williams, J.F.W. Baggen, R. Bezanson, L.A. Boogaard, N.J. Cleri, J.E. Greene, M. Hirschmann, R.E. Hviding, A. Kuruvanthodi, I. Labbé, J. Leja, M.V. Maseda, J.J. Matthee, I. Mcconachie, R.P. Naidu, G. Roberts-Borsani, D. Schaerer, K.A. Suess, F. Valentino, P. Van Dokkum, B. Wang, The Astrophysical Journal 983 (2025).","mla":"Weibel, Andrea, et al. “RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3.” The Astrophysical Journal, vol. 983, no. 1, 11, IOP Publishing, 2025, doi:10.3847/1538-4357/adab7a."},"article_processing_charge":"Yes","oa_version":"Published Version","_id":"19596","day":"10","department":[{"_id":"JoMa"}],"intvolume":" 983","scopus_import":"1","article_type":"original","abstract":[{"text":"We report the spectroscopic discovery of a massive quiescent galaxy at zspec = 7.29 ± 0.01, just ∼700 Myr after the big bang. RUBIES-UDS-QG-z7 was selected from public JWST/NIRCam and MIRI imaging from the PRIMER survey and observed with JWST/NIRSpec as part of RUBIES. The NIRSpec/PRISM spectrum reveals one of the strongest Balmer breaks observed thus far at z > 6, with no emission lines but tentative Balmer and Ca absorption features, as well as a Lyman break. Simultaneous modeling of the NIRSpec/PRISM spectrum and NIRCam and MIRI photometry (spanning 0.9–18 μm) shows that the galaxy formed a stellar mass of\r\n(math. formular) before z ∼ 8 and ceased forming stars 50–100 Myr prior to the time of observation, resulting in log (sSFR/Gyr- 1) < -1 . We measure a small physical size of (math formular) , which implies a high stellarmass surface density within the effective radius of (math formular) comparable to the highest densities measured in quiescent galaxies at z ∼ 2–5. The 3D stellar-mass density profile of RUBIES-UDS-QG-z7 is remarkably similar to the central densities of local massive ellipticals, suggesting that at least some of their cores may have already been in place at z > 7. The discovery of RUBIES-UDS-QG-z7 has strong implications for galaxy formation models: the estimated number density of quiescent galaxies at z ∼ 7 is >100 × larger than predicted from any model to date, indicating that quiescent galaxies have formed earlier than previously expected. ","lang":"eng"}],"date_updated":"2026-02-16T12:42:28Z","author":[{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"full_name":"Brammer, Gabriel","first_name":"Gabriel","last_name":"Brammer"},{"full_name":"Lagos, Claudia D.P.","last_name":"Lagos","first_name":"Claudia D.P."},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."},{"first_name":"Christina C.","last_name":"Williams","full_name":"Williams, Christina C."},{"full_name":"Baggen, Josephine F.W.","first_name":"Josephine F.W.","last_name":"Baggen"},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"last_name":"Cleri","first_name":"Nikko J.","full_name":"Cleri, Nikko J."},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"first_name":"Michaela","last_name":"Hirschmann","full_name":"Hirschmann, Michaela"},{"full_name":"Hviding, Raphael E.","last_name":"Hviding","first_name":"Raphael E."},{"full_name":"Kuruvanthodi, Adarsh","first_name":"Adarsh","last_name":"Kuruvanthodi"},{"first_name":"Ivo","last_name":"Labbé","full_name":"Labbé, Ivo"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"full_name":"Roberts-Borsani, Guido","last_name":"Roberts-Borsani","first_name":"Guido"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"last_name":"Valentino","first_name":"Francesco","full_name":"Valentino, Francesco"},{"last_name":"Van Dokkum","first_name":"Pieter","full_name":"Van Dokkum, Pieter"},{"last_name":"Wang","first_name":"Bingjie","full_name":"Wang, Bingjie"}],"title":"RUBIES reveals a massive quiescent galaxy at z = 7.3","date_created":"2025-04-20T22:01:28Z","external_id":{"isi":["001457334900001"],"arxiv":["2409.03829"]},"article_number":"11","date_published":"2025-04-10T00:00:00Z","OA_type":"gold","file_date_updated":"2025-04-22T09:08:17Z","publication":"The Astrophysical Journal","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"OA_place":"publisher","volume":983,"type":"journal_article","acknowledgement":"We thank the PRIMER team for making their imaging data publicly available immediately. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #4233. Support for program #4233 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #562. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF140). This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI), under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF), through project grant 200020_207349. Support for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. Support for this work for R.P.N. was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. T.B.M. was supported by a CIERA fellowship.\r\nAll software packages used in this work are publicly available on Github: grizli, msafit, msaexp, Prospector, and sedpy. We acknowledge: astropy (Astropy Collaboration et al. 2013, 2018, 2022), matplotlib (J. D. Hunter 2007), numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), lmfit (M. Newville et al. 2024), eMPT (N. Bonaventura et al. 2023), the jwst pipeline (H. Bushouse et al. 2024), msaexp (G. Brammer 2024a), and grizli (G. Brammer 2024b),.","DOAJ_listed":"1","arxiv":1,"isi":1,"month":"04","has_accepted_license":"1","doi":"10.3847/1538-4357/adab7a","issue":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_id":"19605","access_level":"open_access","success":1,"creator":"dernst","date_created":"2025-04-22T09:08:17Z","relation":"main_file","content_type":"application/pdf","file_size":1964589,"checksum":"a1132e0b18bb643f9a32674c6694375a","date_updated":"2025-04-22T09:08:17Z","file_name":"2025_AstrophysicalJour_Weibel.pdf"}],"language":[{"iso":"eng"}],"oa":1,"year":"2025"},{"month":"05","DOAJ_listed":"1","isi":1,"arxiv":1,"file":[{"date_created":"2025-05-19T07:08:39Z","relation":"main_file","checksum":"1a9ff4516d11808bc6947744473c9fc2","content_type":"application/pdf","file_size":3522072,"file_name":"2025_AstrophysicalJour_Wang.pdf","date_updated":"2025-05-19T07:08:39Z","file_id":"19707","access_level":"open_access","success":1,"creator":"dernst"}],"language":[{"iso":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"issue":"2","doi":"10.3847/1538-4357/adc1ca","has_accepted_license":"1","volume":984,"OA_place":"publisher","status":"public","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"acknowledgement":"B.W. and J.L. acknowledge support from JWST-GO-04233.009-A. R.L.D. is supported by the Australian Research Council through the Discovery Early Career Researcher Award (DECRA) Fellowship DE240100136 funded by the Australian Government. T.B.M. was supported by a CIERA postdoctoral fellowship. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant #140. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #562 (First Light at Cosmic Dawn: Exploiting the James Webb Space Telescope Revolution). The JWST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed here can be accessed via DOI:10.17909/c3t4-9p39. Computations for this research were performed on the Pennsylvania State University's Institute for Computational and Data Sciences' Roar supercomputer. This publication made use of the NASA Astrophysical Data System for bibliographic information.","type":"journal_article","external_id":{"arxiv":["2403.02304"],"isi":["001481589300001"]},"date_created":"2025-05-18T22:02:49Z","author":[{"last_name":"Wang","first_name":"Bingjie","full_name":"Wang, Bingjie"},{"full_name":"De Graaff, Anna","last_name":"De Graaff","first_name":"Anna"},{"first_name":"Rebecca L.","last_name":"Davies","full_name":"Davies, Rebecca L."},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"first_name":"Gabriel B.","last_name":"Brammer","full_name":"Brammer, Gabriel B."},{"full_name":"Goulding, Andy D.","last_name":"Goulding","first_name":"Andy D."},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"last_name":"Suess","first_name":"Katherine A.","full_name":"Suess, Katherine A."},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"full_name":"Katz, Harley","first_name":"Harley","last_name":"Katz"},{"full_name":"Labbé, Ivo","last_name":"Labbé","first_name":"Ivo"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Mcconachie","first_name":"Ian","full_name":"Mcconachie, Ian"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"first_name":"Hans Walter","last_name":"Rix","full_name":"Rix, Hans Walter"},{"full_name":"Setton, David J.","first_name":"David J.","last_name":"Setton"},{"first_name":"Katherine E.","last_name":"Whitaker","full_name":"Whitaker, Katherine E."}],"title":"RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow","abstract":[{"text":"The JWST discovery of \"little red dots\" (LRDs) is reshaping our picture of the early Universe, yet the physical mechanisms driving their compact size and UV-optical colors remain elusive. Here, we report an unusually bright LRD (zspec = 3.1) observed as part of the RUBIES program. This LRD exhibits broad emission lines (FWHM ∼ 4000 km s−1), a blue UV continuum, a clear Balmer break, and a red continuum sampled out to rest-frame 4 μm with MIRI. We develop a new joint galaxy and active galactic nucleus (AGN) model within the Prospector Bayesian inference framework and perform spectrophotometric modeling using NIRCam, MIRI, and NIRSpec/Prism observations. Our fiducial model reveals a M* ∼ 109 M⊙ galaxy alongside a dust-reddened AGN driving the optical emission. Explaining the rest-frame optical color as a reddened AGN requires AV ≳ 3, suggesting that a great majority of the accretion disk energy is reradiated as dust emission. Yet, despite clear AGN signatures, we find a surprising lack of hot torus emission, which implies that either the dust emission in this object must be cold, or the red continuum must instead be driven by a massive, evolved stellar population of the host galaxy—seemingly inconsistent with the high-EW broad lines (Hα rest-frame EW ∼ 800 Å). The widths and luminosities of Pa-β, Pa-δ, Pa-γ, and Hα imply a modest black hole mass of MBH ∼ 108 M⊙. Additionally, we identify a narrow blueshifted He i λ 1.083 μm absorption feature in NIRSpec/G395M spectra, signaling an ionized outflow with kinetic energy up to ∼1% the luminosity of the AGN. The low redshift of RUBIES-BLAGN-1, combined with the depth and richness of the JWST imaging and spectroscopic observations, provides a unique opportunity to build a physical model for these so-far mysterious LRDs, which may prove to be a crucial phase in the early formation of massive galaxies and their supermassive black holes.","lang":"eng"}],"date_updated":"2026-02-16T12:42:43Z","file_date_updated":"2025-05-19T07:08:39Z","publication":"The Astrophysical Journal","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","article_number":"121","OA_type":"gold","date_published":"2025-05-09T00:00:00Z","ddc":["520"],"quality_controlled":"1","citation":{"ista":"Wang B, De Graaff A, Davies RL, Greene JE, Leja J, Brammer GB, Goulding AD, Miller TB, Suess KA, Weibel A, Williams CC, Bezanson R, Boogaard LA, Cleri NJ, Hirschmann M, Katz H, Labbé I, Maseda MV, Matthee JJ, Mcconachie I, Naidu RP, Oesch PA, Rix HW, Setton DJ, Whitaker KE. 2025. RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. The Astrophysical Journal. 984(2), 121.","short":"B. Wang, A. De Graaff, R.L. Davies, J.E. Greene, J. Leja, G.B. Brammer, A.D. Goulding, T.B. Miller, K.A. Suess, A. Weibel, C.C. Williams, R. Bezanson, L.A. Boogaard, N.J. Cleri, M. Hirschmann, H. Katz, I. Labbé, M.V. Maseda, J.J. Matthee, I. Mcconachie, R.P. Naidu, P.A. Oesch, H.W. Rix, D.J. Setton, K.E. Whitaker, The Astrophysical Journal 984 (2025).","mla":"Wang, Bingjie, et al. “RUBIES: JWST/NIRSpec Confirmation of an Infrared-Luminous, Broad-Line Little Red Dot with an Ionized Outflow.” The Astrophysical Journal, vol. 984, no. 2, 121, IOP Publishing, 2025, doi:10.3847/1538-4357/adc1ca.","ieee":"B. Wang et al., “RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow,” The Astrophysical Journal, vol. 984, no. 2. IOP Publishing, 2025.","apa":"Wang, B., De Graaff, A., Davies, R. L., Greene, J. E., Leja, J., Brammer, G. B., … Whitaker, K. E. (2025). RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/adc1ca","ama":"Wang B, De Graaff A, Davies RL, et al. RUBIES: JWST/NIRSpec confirmation of an infrared-luminous, broad-line Little Red Dot with an ionized outflow. The Astrophysical Journal. 2025;984(2). doi:10.3847/1538-4357/adc1ca","chicago":"Wang, Bingjie, Anna De Graaff, Rebecca L. Davies, Jenny E. Greene, Joel Leja, Gabriel B. Brammer, Andy D. Goulding, et al. “RUBIES: JWST/NIRSpec Confirmation of an Infrared-Luminous, Broad-Line Little Red Dot with an Ionized Outflow.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/adc1ca."},"publisher":"IOP Publishing","intvolume":" 984","department":[{"_id":"JoMa"}],"article_type":"original","scopus_import":"1","_id":"19700","article_processing_charge":"Yes","oa_version":"Published Version","day":"09"},{"DOAJ_listed":"1","arxiv":1,"month":"12","PlanS_conform":"1","has_accepted_license":"1","doi":"10.1051/0004-6361/202556410","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"file":[{"file_id":"20938","access_level":"open_access","creator":"dernst","success":1,"date_created":"2026-01-05T09:26:17Z","relation":"main_file","file_name":"2025_AstronomyAstrophysics_Liu.pdf","date_updated":"2026-01-05T09:26:17Z","content_type":"application/pdf","checksum":"3e6061f3c4bfb521b3333ea4913c241a","file_size":4642530}],"language":[{"iso":"eng"}],"oa":1,"year":"2025","status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"OA_place":"publisher","volume":704,"type":"journal_article","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.","abstract":[{"text":"Identifying Lyman continuum (LyC) leakers at intermediate redshifts is crucial for understanding the properties of cosmic reionizers because the opacity of the intergalactic medium (IGM) prevents the direct detection of LyC emission from sources during the Epoch of Reionization (EoR). In this study, we confirm two new LyC candidate leakers at z ∼ 3 in the Abell 2744 cluster field, with absolute escape fractions (fesc) of 0.83−0.80+0.15 and 0.74−0.70+0.23, respectively. The LyC emission was detected using HST/WFC3/F275W and F336W imaging. These two candidate leakers appear to be faint (MUV = −17.61 ± 0.06 and −18.22 ± 0.10), exhibit blue UV continuum slopes (β = −2.43 ± 0.05 and −1.92 ± 0.09), have low masses (M★ ∼ 107.51 ± 0.03 and 107.17 ± 0.15 M⊙) and Lyα equivalent widths of 90 ± 3 Å and 28 ± 12 Å, respectively. These two LyC candidate leakers were detected in a catalog of 91 spectroscopically confirmed sources using public spectra from the JWST and/or MUSE. We also analyzed properties that were proposed as indirect indicators of LyC emission, such as Lyα, the O32 ratio, and M★. We created a galaxy subsample that was selected according to these properties, stacked the LyC observations of this subsample, and assessed the limits of the escape fractions in the stacks. We aim to enhance our understanding of LyC escape mechanisms and improve our predictions of the LyC fesc during the EoR by analyzing the individual candidates and the stacks in the context of the currently limited sample of known LyC leakers at z ∼ 3.","lang":"eng"}],"date_updated":"2026-02-16T12:14:52Z","title":"A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field","author":[{"last_name":"Liu","first_name":"Y.","full_name":"Liu, Y."},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"first_name":"L.","last_name":"Pentericci","full_name":"Pentericci, L."},{"full_name":"Watson, P.","first_name":"P.","last_name":"Watson"},{"full_name":"Alavi, A.","first_name":"A.","last_name":"Alavi"},{"last_name":"Bergamini","first_name":"P.","full_name":"Bergamini, P."},{"full_name":"Bradač, M.","first_name":"M.","last_name":"Bradač"},{"first_name":"A.","last_name":"Calabrò","full_name":"Calabrò, A."},{"full_name":"Glazebrook, K.","first_name":"K.","last_name":"Glazebrook"},{"full_name":"Henry, A.","first_name":"A.","last_name":"Henry"},{"full_name":"Llerena, M.","last_name":"Llerena","first_name":"M."},{"first_name":"E.","last_name":"Merlin","full_name":"Merlin, E."},{"full_name":"Metha, B.","last_name":"Metha","first_name":"B."},{"full_name":"Nanayakkara, T.","first_name":"T.","last_name":"Nanayakkara"},{"full_name":"Napolitano, L.","last_name":"Napolitano","first_name":"L."},{"full_name":"Roy, N.","last_name":"Roy","first_name":"N."},{"full_name":"Siana, B.","first_name":"B.","last_name":"Siana"},{"last_name":"Vanzella","first_name":"E.","full_name":"Vanzella, E."},{"full_name":"Vulcani, B.","last_name":"Vulcani","first_name":"B."},{"full_name":"Wang, X.","first_name":"X.","last_name":"Wang"}],"date_created":"2026-01-04T23:01:35Z","external_id":{"arxiv":["2507.11045"]},"article_number":"A328","date_published":"2025-12-01T00:00:00Z","OA_type":"diamond","file_date_updated":"2026-01-05T09:26:17Z","publication":"Astronomy & Astrophysics","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","ddc":["520"],"citation":{"apa":"Liu, Y., Mascia, S., Pentericci, L., Watson, P., Alavi, A., Bergamini, P., … Wang, X. (2025). A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202556410","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. Astronomy & Astrophysics. 2025;704. doi:10.1051/0004-6361/202556410","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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202556410.","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 & Astrophysics. 704, A328.","ieee":"Y. Liu et al., “A Lyman continuum analysis of ∼100 galaxies at z spec∼ 3 in the Abell 2744 cluster field,” Astronomy & Astrophysics, 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 & 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.” Astronomy & Astrophysics, vol. 704, A328, EDP Sciences, 2025, doi:10.1051/0004-6361/202556410."},"quality_controlled":"1","article_processing_charge":"No","oa_version":"Published Version","_id":"20932","day":"01","department":[{"_id":"JoMa"}],"intvolume":" 704","article_type":"original","scopus_import":"1"},{"status":"public","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"OA_place":"publisher","volume":995,"type":"journal_article","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.","DOAJ_listed":"1","arxiv":1,"month":"12","has_accepted_license":"1","PlanS_conform":"1","doi":"10.3847/1538-4357/ae1500","issue":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"language":[{"iso":"eng"}],"file":[{"date_created":"2026-02-09T06:39:23Z","relation":"main_file","file_name":"2025_AstrophysicalJournal_Setton.pdf","date_updated":"2026-02-09T06:39:23Z","checksum":"2a424eb43748a6370ff058c98adb15c6","file_size":1989640,"content_type":"application/pdf","file_id":"21163","access_level":"open_access","creator":"dernst","success":1}],"oa":1,"year":"2025","publisher":"IOP Publishing","ddc":["520"],"citation":{"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.","mla":"Setton, David J., et al. “Little Red Dots at an Inflection Point: Ubiquitous v-Shaped Turnover Consistently Occurs at the Balmer Limit.” The Astrophysical Journal, vol. 995, no. 1, 118, IOP Publishing, 2025, doi:10.3847/1538-4357/ae1500.","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).","ieee":"D. J. Setton et al., “Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit,” The Astrophysical Journal, vol. 995, no. 1. IOP Publishing, 2025.","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. The Astrophysical Journal. 2025;995(1). doi:10.3847/1538-4357/ae1500","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. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae1500","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.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ae1500."},"quality_controlled":"1","oa_version":"Published Version","article_processing_charge":"Yes","_id":"21057","day":"09","department":[{"_id":"JoMa"}],"intvolume":" 995","scopus_import":"1","article_type":"original","abstract":[{"lang":"eng","text":"Among the most puzzling early discoveries of JWST are “little red dots” (LRDs), compact red sources that host broad Balmer emission lines, and in many cases exhibit a “V-shaped” change in slope in the rest-optical. The physical properties of LRDs currently have order-of-magnitude uncertainties, because models to explain the continuum of these sources differ immensely. Here, we leverage the complete selection of red sources in the RUBIES program, supplemented with public PRISM spectra, to study the origin of this V shape. By fitting a broken power law with a flexible inflection point, we find that a large fraction of red Hα emitters at 2 < z < 6 exhibit a strong change in slope, and that all strong inflections appear associated with the Balmer limit (0.3645 μm). Using a simple model of a reddened active galactic nucleus (AGN) with an unobscured scattered-light component, we demonstrate that the observed V shape in LRDs is unlikely to occur at any specific wavelength if the entire continuum is dominated by light from a power-law AGN continuum. In contrast, models with an intrinsic feature at the Balmer limit, such as those that are dominated by an evolved stellar population, can produce the observed spectral shapes, provided that a reddened component picks up sufficiently redward of the break. While no model can comfortably explain the full LRD spectral energy distribution, the common inflection location suggests that a single component consistently dominates the rest-frame UV optical in LRDs, and that this component is associated with T ∼ 10^4 K hydrogen."}],"date_updated":"2026-02-09T06:41:48Z","title":"Little Red Dots at an inflection point: Ubiquitous v-shaped turnover consistently occurs at the Balmer limit","author":[{"first_name":"David J.","last_name":"Setton","full_name":"Setton, David J."},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"first_name":"Anna","last_name":"de Graaff","full_name":"de Graaff, Anna"},{"full_name":"Ma, Yilun 逸伦","first_name":"Yilun 逸伦","last_name":"Ma"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"last_name":"Boogaard","first_name":"Leindert A.","full_name":"Boogaard, Leindert A."},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"full_name":"Katz, Harley","last_name":"Katz","first_name":"Harley"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"full_name":"McConachie, Ian","first_name":"Ian","last_name":"McConachie"},{"first_name":"Tim B.","last_name":"Miller","full_name":"Miller, Tim B."},{"last_name":"Price","first_name":"Sedona H.","full_name":"Price, Sedona H."},{"first_name":"Katherine A.","last_name":"Suess","full_name":"Suess, Katherine A."},{"full_name":"van Dokkum, Pieter","first_name":"Pieter","last_name":"van Dokkum"},{"first_name":"Bingjie 冰洁","last_name":"Wang 王","full_name":"Wang 王, Bingjie 冰洁"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."},{"first_name":"Christina C.","last_name":"Williams","full_name":"Williams, Christina C."}],"date_created":"2026-01-28T15:21:47Z","external_id":{"arxiv":["2411.03424"]},"article_number":"118","date_published":"2025-12-09T00:00:00Z","OA_type":"gold","file_date_updated":"2026-02-09T06:39:23Z","publication":"The Astrophysical Journal","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"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","volume":991,"OA_place":"publisher","status":"public","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"file":[{"date_created":"2026-02-09T07:10:29Z","relation":"main_file","content_type":"application/pdf","checksum":"799518db92ded4e166df4234195af998","file_size":1394204,"date_updated":"2026-02-09T07:10:29Z","file_name":"2025_AstrophysicalJournalLetters_Setton.pdf","file_id":"21165","access_level":"open_access","success":1,"creator":"dernst"}],"language":[{"iso":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"doi":"10.3847/2041-8213/ade78b","PlanS_conform":"1","has_accepted_license":"1","month":"09","DOAJ_listed":"1","arxiv":1,"intvolume":" 991","department":[{"_id":"JoMa"}],"article_type":"original","scopus_import":"1","_id":"21058","article_processing_charge":"Yes","oa_version":"Published Version","day":"12","ddc":["520"],"citation":{"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. The Astrophysical Journal Letters. 2025;991. doi:10.3847/2041-8213/ade78b","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. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ade78b","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.” The Astrophysical Journal Letters. IOP Publishing, 2025. https://doi.org/10.3847/2041-8213/ade78b.","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.","mla":"Setton, David J., et al. “A Confirmed Deficit of Hot and Cold Dust Emission in the Most Luminous Little Red Dots.” The Astrophysical Journal Letters, vol. 991, L10, IOP Publishing, 2025, doi:10.3847/2041-8213/ade78b.","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 et al., “A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots,” The Astrophysical Journal Letters, vol. 991. IOP Publishing, 2025."},"quality_controlled":"1","publisher":"IOP Publishing","file_date_updated":"2026-02-09T07:10:29Z","publication":"The Astrophysical Journal Letters","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","article_number":"L10","OA_type":"gold","date_published":"2025-09-12T00:00:00Z","external_id":{"arxiv":["2503.02059"]},"date_created":"2026-01-28T15:23:00Z","title":"A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots","author":[{"full_name":"Setton, David J.","first_name":"David J.","last_name":"Setton"},{"last_name":"Greene","first_name":"Jenny E.","full_name":"Greene, Jenny E."},{"last_name":"Spilker","first_name":"Justin S.","full_name":"Spilker, Justin S."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."},{"first_name":"Ivo","last_name":"Labbé","full_name":"Labbé, Ivo"},{"first_name":"Yilun 逸伦","last_name":"Ma","full_name":"Ma, Yilun 逸伦"},{"full_name":"Wang, Bingjie 冰洁","last_name":"Wang","first_name":"Bingjie 冰洁"},{"full_name":"Whitaker, Katherine E.","first_name":"Katherine E.","last_name":"Whitaker"},{"full_name":"Leja, Joel","first_name":"Joel","last_name":"Leja"},{"last_name":"de Graaff","first_name":"Anna","full_name":"de Graaff, Anna"},{"full_name":"Alberts, Stacey","first_name":"Stacey","last_name":"Alberts"},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"full_name":"Boogaard, Leindert A.","first_name":"Leindert A.","last_name":"Boogaard"},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"first_name":"Sam E.","last_name":"Cutler","full_name":"Cutler, Sam E."},{"last_name":"Cleri","first_name":"Nikko J.","full_name":"Cleri, Nikko J."},{"last_name":"Cooper","first_name":"Olivia R.","full_name":"Cooper, Olivia R."},{"last_name":"Dayal","first_name":"Pratika","full_name":"Dayal, Pratika"},{"first_name":"Seiji","last_name":"Fujimoto","full_name":"Fujimoto, Seiji"},{"last_name":"Furtak","first_name":"Lukas J.","full_name":"Furtak, Lukas J."},{"full_name":"Goulding, Andy D.","last_name":"Goulding","first_name":"Andy D."},{"full_name":"Hirschmann, Michaela","first_name":"Michaela","last_name":"Hirschmann"},{"first_name":"Vasily","last_name":"Kokorev","full_name":"Kokorev, Vasily"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"first_name":"Ian","last_name":"McConachie","full_name":"McConachie, Ian"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Tim B.","last_name":"Miller","full_name":"Miller, Tim B."},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"full_name":"Pan, Richard","last_name":"Pan","first_name":"Richard"},{"full_name":"Price, Sedona H.","last_name":"Price","first_name":"Sedona H."},{"last_name":"Suess","first_name":"Katherine A.","full_name":"Suess, Katherine A."},{"full_name":"Weaver, John R.","last_name":"Weaver","first_name":"John R."},{"full_name":"Xiao, Mengyuan","first_name":"Mengyuan","last_name":"Xiao"},{"full_name":"Zhang, Yunchong","first_name":"Yunchong","last_name":"Zhang"},{"last_name":"Zitrin","first_name":"Adi","full_name":"Zitrin, Adi"}],"abstract":[{"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.","lang":"eng"}],"date_updated":"2026-02-09T07:14:08Z"},{"_id":"21060","oa_version":"Published Version","article_processing_charge":"No","day":"01","intvolume":" 701","department":[{"_id":"JoMa"}],"scopus_import":"1","article_type":"original","publisher":"EDP Sciences","ddc":["520"],"quality_controlled":"1","citation":{"ieee":"S. Mascia et al., “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” Astronomy & Astrophysics, vol. 701. EDP Sciences, 2025.","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 & 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.” Astronomy & Astrophysics, vol. 701, A122, EDP Sciences, 2025, doi:10.1051/0004-6361/202553760.","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 & Astrophysics. 701, A122.","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.” Astronomy & Astrophysics. EDP Sciences, 2025. https://doi.org/10.1051/0004-6361/202553760.","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. Astronomy & Astrophysics. 2025;701. doi:10.1051/0004-6361/202553760","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. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202553760"},"article_number":"A122","corr_author":"1","OA_type":"diamond","date_published":"2025-09-01T00:00:00Z","publication":"Astronomy & Astrophysics","file_date_updated":"2026-02-09T07:28:08Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","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"}],"date_updated":"2026-02-09T07:33:46Z","date_created":"2026-01-28T15:24:24Z","external_id":{"arxiv":["2501.08268"]},"author":[{"first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"first_name":"L.","last_name":"Pentericci","full_name":"Pentericci, L."},{"full_name":"Llerena, M.","first_name":"M.","last_name":"Llerena"},{"first_name":"A.","last_name":"Calabrò","full_name":"Calabrò, A."},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"S.","last_name":"Flury","full_name":"Flury, S."},{"full_name":"Pacucci, F.","first_name":"F.","last_name":"Pacucci"},{"last_name":"Jaskot","first_name":"A.","full_name":"Jaskot, A."},{"first_name":"R. O.","last_name":"Amorín","full_name":"Amorín, R. O."},{"full_name":"Bhatawdekar, R.","first_name":"R.","last_name":"Bhatawdekar"},{"full_name":"Castellano, M.","first_name":"M.","last_name":"Castellano"},{"full_name":"Cleri, N.","first_name":"N.","last_name":"Cleri"},{"first_name":"L.","last_name":"Costantin","full_name":"Costantin, L."},{"full_name":"Davis, K.","first_name":"K.","last_name":"Davis"},{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"full_name":"Dickinson, M.","first_name":"M.","last_name":"Dickinson"},{"first_name":"A.","last_name":"Fontana","full_name":"Fontana, A."},{"last_name":"Guo","first_name":"Y.","full_name":"Guo, Y."},{"first_name":"M.","last_name":"Giavalisco","full_name":"Giavalisco, M."},{"full_name":"Holwerda, B. W.","first_name":"B. W.","last_name":"Holwerda"},{"full_name":"Hu, W.","first_name":"W.","last_name":"Hu"},{"full_name":"Huertas-Company, M.","first_name":"M.","last_name":"Huertas-Company"},{"full_name":"Jung, Intae","last_name":"Jung","first_name":"Intae"},{"full_name":"Kartaltepe, J.","first_name":"J.","last_name":"Kartaltepe"},{"full_name":"Kashino, D.","last_name":"Kashino","first_name":"D."},{"last_name":"Koekemoer","first_name":"A. M.","full_name":"Koekemoer, A. M."},{"first_name":"R. A.","last_name":"Lucas","full_name":"Lucas, R. A."},{"last_name":"Lotz","first_name":"J.","full_name":"Lotz, J."},{"first_name":"L.","last_name":"Napolitano","full_name":"Napolitano, L."},{"full_name":"Jogee, S.","first_name":"S.","last_name":"Jogee"},{"first_name":"S.","last_name":"Wilkins","full_name":"Wilkins, S."}],"title":"Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"type":"journal_article","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”.","status":"public","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"volume":701,"OA_place":"publisher","doi":"10.1051/0004-6361/202553760","has_accepted_license":"1","PlanS_conform":"1","language":[{"iso":"eng"}],"file":[{"file_id":"21166","access_level":"open_access","success":1,"creator":"dernst","date_created":"2026-02-09T07:28:08Z","relation":"main_file","content_type":"application/pdf","checksum":"990e384ca19e14b35296712d3b9e2919","file_size":9994234,"date_updated":"2026-02-09T07:28:08Z","file_name":"2025_AstronomyAstrophysics_Mascia.pdf"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"DOAJ_listed":"1","arxiv":1,"month":"09"},{"year":"2025","oa":1,"language":[{"iso":"eng"}],"file":[{"relation":"main_file","date_created":"2026-02-09T07:57:01Z","checksum":"9e08e77ce6d818fafd074e2b6c30bc43","content_type":"application/pdf","file_size":14405059,"file_name":"2025_AstrophysicalJournal_Fujimoto.pdf","date_updated":"2026-02-09T07:57:01Z","file_id":"21167","success":1,"creator":"dernst","access_level":"open_access"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"doi":"10.3847/1538-4357/ade9a1","PlanS_conform":"1","has_accepted_license":"1","month":"08","DOAJ_listed":"1","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).","type":"journal_article","volume":989,"OA_place":"publisher","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","file_date_updated":"2026-02-09T07:57:01Z","publication":"The Astrophysical Journal","OA_type":"gold","date_published":"2025-08-04T00:00:00Z","article_number":"46","date_created":"2026-01-28T15:25:17Z","author":[{"last_name":"Fujimoto","first_name":"Seiji","full_name":"Fujimoto, Seiji"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"last_name":"Atek","first_name":"Hakim","full_name":"Atek, Hakim"},{"first_name":"Ryan","last_name":"Endsley","full_name":"Endsley, Ryan"},{"full_name":"Kokorev, Vasily","first_name":"Vasily","last_name":"Kokorev"},{"full_name":"Furtak, Lukas J.","first_name":"Lukas J.","last_name":"Furtak"},{"last_name":"Pan","first_name":"Richard","full_name":"Pan, Richard"},{"full_name":"Liu, Boyuan","first_name":"Boyuan","last_name":"Liu"},{"full_name":"Bromm, Volker","last_name":"Bromm","first_name":"Volker"},{"full_name":"Venditti, Alessandra","first_name":"Alessandra","last_name":"Venditti"},{"last_name":"Visbal","first_name":"Eli","full_name":"Visbal, Eli"},{"full_name":"Sarmento, Richard","last_name":"Sarmento","first_name":"Richard"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"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"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"last_name":"Chemerynska","first_name":"Iryna","full_name":"Chemerynska, Iryna"},{"full_name":"Claeyssens, Adélaïde","first_name":"Adélaïde","last_name":"Claeyssens"},{"first_name":"Miroslava","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava"},{"full_name":"Frebel, Anna","first_name":"Anna","last_name":"Frebel"},{"last_name":"Korber","first_name":"Damien","full_name":"Korber, Damien"},{"full_name":"Labbe, Ivo","first_name":"Ivo","last_name":"Labbe"},{"last_name":"Marques-Chaves","first_name":"Rui","full_name":"Marques-Chaves, Rui"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"McQuinn, Kristen B. W.","last_name":"McQuinn","first_name":"Kristen B. W."},{"full_name":"Muñoz, Julian B.","last_name":"Muñoz","first_name":"Julian B."},{"full_name":"Natarajan, Priyamvada","last_name":"Natarajan","first_name":"Priyamvada"},{"full_name":"Saldana-Lopez, Alberto","first_name":"Alberto","last_name":"Saldana-Lopez"},{"full_name":"Suess, Katherine A.","last_name":"Suess","first_name":"Katherine A."},{"full_name":"Volonteri, Marta","first_name":"Marta","last_name":"Volonteri"},{"first_name":"Adi","last_name":"Zitrin","full_name":"Zitrin, Adi"}],"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","date_updated":"2026-02-09T08:11:01Z","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"}],"scopus_import":"1","article_type":"original","intvolume":" 989","department":[{"_id":"JoMa"}],"day":"04","_id":"21061","oa_version":"Published Version","article_processing_charge":"Yes","quality_controlled":"1","citation":{"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.","ieee":"S. Fujimoto 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,” The Astrophysical Journal, vol. 989. IOP Publishing, 2025.","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).","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.” The Astrophysical Journal, vol. 989, 46, IOP Publishing, 2025, doi:10.3847/1538-4357/ade9a1.","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. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ade9a1","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. The Astrophysical Journal. 2025;989. doi:10.3847/1538-4357/ade9a1","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.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ade9a1."},"ddc":["520"],"publisher":"IOP Publishing"},{"citation":{"ieee":"J. J. Matthee et al., “Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” The Astrophysical Journal, vol. 988, no. 2. IOP Publishing, 2025.","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.” The Astrophysical Journal, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:10.3847/1538-4357/ade886.","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).","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.","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.” The Astrophysical Journal. IOP Publishing, 2025. https://doi.org/10.3847/1538-4357/ade886.","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. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ade886","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. The Astrophysical Journal. 2025;988(2). doi:10.3847/1538-4357/ade886"},"quality_controlled":"1","ddc":["520"],"publisher":"IOP Publishing","scopus_import":"1","article_type":"original","intvolume":" 988","department":[{"_id":"JoMa"}],"day":"29","_id":"21062","article_processing_charge":"Yes","oa_version":"Published Version","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"date_created":"2026-01-28T15:25:42Z","external_id":{"arxiv":["2412.02846"]},"title":"Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5","author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri","last_name":"Kotiwale"},{"full_name":"Furtak, Lukas J.","last_name":"Furtak","first_name":"Lukas J."},{"full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Greene, Jenny","last_name":"Greene","first_name":"Jenny"},{"full_name":"Adamo, Angela","first_name":"Angela","last_name":"Adamo"},{"full_name":"Bouwens, Rychard J.","first_name":"Rychard J.","last_name":"Bouwens"},{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia","last_name":"Di Cesare"},{"first_name":"Anna-Christina","last_name":"Eilers","full_name":"Eilers, Anna-Christina"},{"first_name":"Anna","last_name":"de Graaff","full_name":"de Graaff, Anna"},{"full_name":"Heintz, Kasper E.","first_name":"Kasper E.","last_name":"Heintz"},{"last_name":"Kashino","first_name":"Daichi","full_name":"Kashino, Daichi"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","first_name":"Alberto","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541"}],"date_updated":"2026-02-09T08:22:01Z","abstract":[{"lang":"eng","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."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","file_date_updated":"2026-02-09T08:20:14Z","publication":"The Astrophysical Journal","OA_type":"gold","date_published":"2025-07-29T00:00:00Z","article_number":"246","corr_author":"1","volume":988,"OA_place":"publisher","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"status":"public","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).","type":"journal_article","month":"07","arxiv":1,"DOAJ_listed":"1","year":"2025","oa":1,"language":[{"iso":"eng"}],"file":[{"content_type":"application/pdf","checksum":"a49fbed72f2ff9c0b13129acb6f44f9d","file_size":6237415,"date_updated":"2026-02-09T08:20:14Z","file_name":"2025_AstrophysicalJournal_Matthee.pdf","date_created":"2026-02-09T08:20:14Z","relation":"main_file","access_level":"open_access","success":1,"creator":"dernst","file_id":"21168"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"doi":"10.3847/1538-4357/ade886","issue":"2","has_accepted_license":"1","PlanS_conform":"1"},{"file":[{"date_updated":"2026-02-09T08:39:19Z","file_name":"2025_MonthlyNoticesRAS_HerardDemanche.pdf","file_size":2787493,"content_type":"application/pdf","checksum":"4cbade43244eaa8b60bb05a90ae613da","date_created":"2026-02-09T08:39:19Z","relation":"main_file","access_level":"open_access","creator":"dernst","success":1,"file_id":"21169"}],"language":[{"iso":"eng"}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"year":"2025","oa":1,"doi":"10.1093/mnras/staf030","issue":"2","PlanS_conform":"1","has_accepted_license":"1","page":"788-808","month":"02","DOAJ_listed":"1","arxiv":1,"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).","type":"journal_article","volume":537,"OA_place":"publisher","status":"public","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"file_date_updated":"2026-02-09T08:39:19Z","publication":"Monthly Notices of the Royal Astronomical Society","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","OA_type":"gold","date_published":"2025-02-01T00:00:00Z","date_created":"2026-01-28T15:25:53Z","external_id":{"arxiv":["2309.04525"]},"author":[{"first_name":"Thomas","last_name":"Herard-Demanche","full_name":"Herard-Demanche, Thomas"},{"full_name":"Bouwens, Rychard J","first_name":"Rychard J","last_name":"Bouwens"},{"first_name":"Pascal A","last_name":"Oesch","full_name":"Oesch, Pascal A"},{"last_name":"Naidu","first_name":"Rohan P","full_name":"Naidu, Rohan P"},{"full_name":"Decarli, Roberto","first_name":"Roberto","last_name":"Decarli"},{"full_name":"Nelson, Erica J","first_name":"Erica J","last_name":"Nelson"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"last_name":"Weibel","first_name":"Andrea","full_name":"Weibel, Andrea"},{"full_name":"Xiao, Mengyuan","first_name":"Mengyuan","last_name":"Xiao"},{"last_name":"Stefanon","first_name":"Mauro","full_name":"Stefanon, Mauro"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Meyer","first_name":"Romain A","full_name":"Meyer, Romain A"},{"full_name":"Wuyts, Stijn","last_name":"Wuyts","first_name":"Stijn"},{"first_name":"Naveen","last_name":"Reddy","full_name":"Reddy, Naveen"},{"last_name":"Rowland","first_name":"Lucie","full_name":"Rowland, Lucie"},{"full_name":"van Leeuwen, Ivana","first_name":"Ivana","last_name":"van Leeuwen"},{"first_name":"Pablo Arrabal","last_name":"Haro","full_name":"Haro, Pablo Arrabal"},{"last_name":"Dannerbauer","first_name":"Helmut","full_name":"Dannerbauer, Helmut"},{"first_name":"Alice E","last_name":"Shapley","full_name":"Shapley, Alice E"},{"full_name":"Chisholm, John","first_name":"John","last_name":"Chisholm"},{"full_name":"van Dokkum, Pieter","last_name":"van Dokkum","first_name":"Pieter"},{"full_name":"Labbe, Ivo","last_name":"Labbe","first_name":"Ivo"},{"full_name":"Illingworth, Garth","last_name":"Illingworth","first_name":"Garth"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"last_name":"Shivaei","first_name":"Irene","full_name":"Shivaei, Irene"}],"title":"Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures","abstract":[{"lang":"eng","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."}],"date_updated":"2026-02-09T08:50:55Z","intvolume":" 537","department":[{"_id":"JoMa"}],"article_type":"original","_id":"21063","oa_version":"Published Version","article_processing_charge":"Yes","day":"01","ddc":["520"],"citation":{"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 > 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf030.","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 > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf030","ama":"Herard-Demanche T, Bouwens RJ, Oesch PA, et al. Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. 2025;537(2):788-808. doi:10.1093/mnras/staf030","ieee":"T. Herard-Demanche et al., “Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures,” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 2. Oxford University Press, pp. 788–808, 2025.","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.","mla":"Herard-Demanche, Thomas, et al. “Mapping Dusty Galaxy Growth at z > 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 2, Oxford University Press, 2025, pp. 788–808, doi:10.1093/mnras/staf030.","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 > 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."},"quality_controlled":"1","publisher":"Oxford University Press"},{"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).","type":"journal_article","OA_place":"repository","volume":66,"status":"public","publication_identifier":{"eissn":["1366-5812"],"issn":["0010-7514"]},"language":[{"iso":"eng"}],"oa":1,"year":"2025","page":"116-151","issue":"1-4","doi":"10.1080/00107514.2025.2586370","month":"12","arxiv":1,"department":[{"_id":"JoMa"}],"intvolume":" 66","article_type":"original","scopus_import":"1","oa_version":"Preprint","article_processing_charge":"No","_id":"20864","day":"04","quality_controlled":"1","citation":{"apa":"Matthee, J. J. (2025). JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. Contemporary Physics. Taylor & Francis. https://doi.org/10.1080/00107514.2025.2586370","ama":"Matthee JJ. JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. Contemporary Physics. 2025;66(1-4):116-151. doi:10.1080/00107514.2025.2586370","chicago":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” Contemporary Physics. Taylor & Francis, 2025. https://doi.org/10.1080/00107514.2025.2586370.","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.","mla":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” Contemporary Physics, vol. 66, no. 1–4, Taylor & Francis, 2025, pp. 116–51, doi:10.1080/00107514.2025.2586370.","short":"J.J. Matthee, Contemporary Physics 66 (2025) 116–151.","ieee":"J. J. Matthee, “JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies,” Contemporary Physics, vol. 66, no. 1–4. Taylor & Francis, pp. 116–151, 2025."},"publisher":"Taylor & Francis","publication":"Contemporary Physics","publication_status":"published","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","corr_author":"1","date_published":"2025-12-04T00:00:00Z","OA_type":"green","title":"JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}],"date_created":"2025-12-29T12:05:25Z","external_id":{"arxiv":["2511.04843"]},"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"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."}],"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2511.04843","open_access":"1"}],"date_updated":"2026-04-07T08:44:00Z"}]