[{"author":[{"last_name":"Chang","full_name":"Chang, Seok Jun","first_name":"Seok Jun"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"Charlotte","full_name":"Mason, Charlotte","last_name":"Mason"}],"issue":"4","_id":"21038","external_id":{"arxiv":["2508.08768"]},"volume":545,"intvolume":"       545","article_processing_charge":"Yes","date_published":"2026-02-01T00:00:00Z","year":"2026","article_number":"staf2131","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"Oxford University Press","ddc":["520"],"has_accepted_license":"1","oa":1,"article_type":"original","OA_place":"publisher","title":"Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"gold","file_date_updated":"2026-02-12T12:44:33Z","PlanS_conform":"1","DOAJ_listed":"1","type":"journal_article","date_updated":"2026-02-12T12:56:33Z","abstract":[{"text":"Little Red Dots (LRDs) are compact sources at z > 5 discovered through James Webb Space Telescope spectroscopy. Their spectra exhibit broad Balmer emission lines (>~1000 km s^−1), alongside absorption features and a pronounced Balmer break – evidence for a dense, neutral hydrogen medium, in which the n = 2 state is significantly populated. When interpreted as arising\r\nfrom active galactic nucleus broad-line regions, inferred black hole masses from local scaling relations exceed expectations given their stellar masses, challenging models of early black hole–galaxy co-evolution. However, radiative transfer effects in dense media may also impact the formation of hydrogen emission lines. We model three scattering processes shaping hydrogen\r\nline profiles: resonance scattering by hydrogen in the n = 2 state, Raman scattering of ultraviolet (UV) radiation by ground-state hydrogen, and Thomson scattering by free electrons. Using 3D Monte Carlo radiative transfer simulations, we examine their imprint on line shapes and ratios. Resonance scattering produces strong deviations from Case B flux ratios, clear differences\r\nbetween Hα and Hβ, and encodes gas kinematics in line profiles but cannot broaden Hβ due to conversion to Paα. While Raman scattering can yield broad wings, scattering of the UV continuum is disfavoured given the absence of strong full width at half-maximum variations across transitions. Raman scattering of higher Lyman-series emission can produce Hα/Hβ wing\r\nwidth ratios of  >~1.28, agreeing with observations. Thomson scattering can reproduce the observed >~ 1000 km s^−1 wings under plausible conditions – e.g. Te ∼ 10^4 K and Ne ∼ 10^24 cm^−2 – and lead to black hole mass overestimates by factors  10. Our results provide a framework for interpreting hydrogen lines in LRDs and similar systems.","lang":"eng"}],"date_created":"2026-01-25T23:01:39Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"arxiv":1,"language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","month":"02","publication_status":"published","department":[{"_id":"JoMa"}],"doi":"10.1093/mnras/staf2131","day":"01","scopus_import":"1","acknowledgement":"The authorsthank the anonymousreferee for constructive comments, which improved the clarity of this paper. SJC acknowledges support from the ERC synergy grant 101166930 – RECAP. MG thanks the Max Planck Society for support through the Max Planck Research Group, and the European Union forsupport through ERC-2024-STG 101165038 (ReMMU). JM acknowledges funding by the European Union (ERC, AGENTS, 101076224). CAM acknowledges support\r\nby the European Union ERC grant RISES (101163035), Carlsberg Foundation (CF22-1322), and VILLUM FONDEN (37459). Computations were performed on HPC systems Freya and Orion at the Max Planck Computing and Data Facility.","status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"ama":"Chang SJ, Gronke M, Matthee JJ, Mason C. Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. <i>Monthly Notices of the Royal Astronomical Society</i>. 2026;545(4). doi:<a href=\"https://doi.org/10.1093/mnras/staf2131\">10.1093/mnras/staf2131</a>","apa":"Chang, S. J., Gronke, M., Matthee, J. J., &#38; Mason, C. (2026). Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf2131\">https://doi.org/10.1093/mnras/staf2131</a>","ieee":"S. J. Chang, M. Gronke, J. J. Matthee, and C. Mason, “Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 4. Oxford University Press, 2026.","ista":"Chang SJ, Gronke M, Matthee JJ, Mason C. 2026. Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. Monthly Notices of the Royal Astronomical Society. 545(4), staf2131.","mla":"Chang, Seok Jun, et al. “Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 4, staf2131, Oxford University Press, 2026, doi:<a href=\"https://doi.org/10.1093/mnras/staf2131\">10.1093/mnras/staf2131</a>.","chicago":"Chang, Seok Jun, Max Gronke, Jorryt J Matthee, and Charlotte Mason. “Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2026. <a href=\"https://doi.org/10.1093/mnras/staf2131\">https://doi.org/10.1093/mnras/staf2131</a>.","short":"S.J. Chang, M. Gronke, J.J. Matthee, C. Mason, Monthly Notices of the Royal Astronomical Society 545 (2026)."},"file":[{"creator":"dernst","file_size":5600366,"date_updated":"2026-02-12T12:44:33Z","file_name":"2026_MonthNoticesRAS_Chang.pdf","date_created":"2026-02-12T12:44:33Z","file_id":"21220","checksum":"52ba7d7b5b80af0c50f57e4c2acc3930","relation":"main_file","content_type":"application/pdf","access_level":"open_access","success":1}]},{"volume":705,"intvolume":"       705","author":[{"orcid":"0000-0001-5586-6950","first_name":"Alberto","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"first_name":"Tanya","last_name":"Urrutia","full_name":"Urrutia, Tanya"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia","first_name":"Sara"},{"full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio","first_name":"Francesco"},{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia"},{"first_name":"Anna Christina","full_name":"Eilers, Anna Christina","last_name":"Eilers"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"orcid":"0000-0001-8386-3546","first_name":"Edoardo","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani"},{"first_name":"Yuzo","last_name":"Ishikawa","full_name":"Ishikawa, Yuzo"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín"},{"last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","first_name":"Gauri"}],"_id":"21045","external_id":{"arxiv":["2505.09542"]},"year":"2026","article_number":"A147","ddc":["520"],"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"EDP Sciences","article_processing_charge":"No","date_published":"2026-01-14T00:00:00Z","type":"journal_article","date_updated":"2026-02-16T07:46:53Z","file_date_updated":"2026-02-16T07:35:03Z","PlanS_conform":"1","publication":"Astronomy and Astrophysics","date_created":"2026-01-25T23:01:41Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"abstract":[{"lang":"eng","text":"The abundant population of little red dots (LRDs), compact objects with red UV to optical colors and broad Balmer lines at high redshift, is revealing new insights into the properties of early active galactic nuclei (AGN). Perhaps the most surprising features of this population are the presence of Balmer absorption and ubiquitous strong Balmer breaks. Recent models link these features to an active supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We present a stringent test of such models using VLT/MUSE observations of A2744-45924, the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744 lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula (h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc. The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα) compared to Lyα nebulae typically observed around quasars of similar luminosity. We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered by star formation. In the environment of A2744-45924, we identified four extended Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations based on Hα emission, and show no evidence for radiation from A2744-45924 affecting its surroundings. The lack of strong, compact, and broad Lyα and the absence of a luminous extended halo, suggest that the UV AGN light is obscured by dense gas cloaking the SMBH with a covering factor close to unity."}],"has_accepted_license":"1","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","OA_type":"diamond","article_type":"original","OA_place":"publisher","acknowledgement":"We thank the anonymous referee for constructive and useful comments. We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge funding from JWST program GO-3516. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #3516. MG thanks the Max Planck Society for support through the MPRG. FDE acknowledges support by the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.","scopus_import":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy and Astrophysics. 705, A147.","mla":"Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy and Astrophysics</i>, vol. 705, A147, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>.","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke, S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa, R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy and Astrophysics 705 (2026).","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” <i>Astronomy and Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy and Astrophysics</i>. 2026;705. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke, M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. <i>Astronomy and Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>","ieee":"A. Torralba Torregrosa <i>et al.</i>, “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” <i>Astronomy and Astrophysics</i>, vol. 705. EDP Sciences, 2026."},"file":[{"file_id":"21224","date_created":"2026-02-16T07:35:03Z","file_name":"2026_AstronomyAstrophysics_Torralba.pdf","date_updated":"2026-02-16T07:35:03Z","file_size":2259914,"creator":"dernst","success":1,"access_level":"open_access","content_type":"application/pdf","relation":"main_file","checksum":"3782e03bc0843438aae8487f6af779c5"}],"status":"public","oa_version":"Published Version","quality_controlled":"1","language":[{"iso":"eng"}],"arxiv":1,"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication_status":"published","day":"14","doi":"10.1051/0004-6361/202555596","corr_author":"1","month":"01"},{"corr_author":"1","month":"02","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication_status":"published","day":"01","doi":"10.1051/0004-6361/202556597","arxiv":1,"quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"file":[{"file_size":6531719,"creator":"dernst","date_updated":"2026-02-24T07:46:47Z","file_name":"2026_AstronomyAstrophysics_Kotiwale.pdf","date_created":"2026-02-24T07:46:47Z","file_id":"21355","relation":"main_file","checksum":"6f5849d29ad43bee32f90152f6fc0294","content_type":"application/pdf","success":1,"access_level":"open_access"}],"citation":{"short":"G. Kotiwale, J.J. Matthee, D. Kashino, A.P. Vijayan, A. Torralba Torregrosa, C. Di Cesare, E. Iani, R. Bordoloi, J. Leja, M.V. Maseda, S. Tacchella, I. Shivaei, K.E. Heintz, A.L. Danhaive, S. Mascia, I. Kramarenko, B. Navarrete, R. Mackenzie, R.P. Naidu, D. Sobral, Astronomy &#38; Astrophysics 706 (2026).","chicago":"Kotiwale, Gauri, Jorryt J Matthee, Daichi Kashino, Aswin P. Vijayan, Alberto Torralba Torregrosa, Claudia Di Cesare, Edoardo Iani, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>.","mla":"Kotiwale, Gauri, et al. “Rapid, out-of-Equilibrium Metal Enrichment Indicated by a Flat Mass-Metallicity Relation at z ∼ 6 from NIRCam Grism Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 706, A165, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>.","ista":"Kotiwale G, Matthee JJ, Kashino D, Vijayan AP, Torralba Torregrosa A, Di Cesare C, Iani E, Bordoloi R, Leja J, Maseda MV, Tacchella S, Shivaei I, Heintz KE, Danhaive AL, Mascia S, Kramarenko I, Navarrete B, Mackenzie R, Naidu RP, Sobral D. 2026. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. Astronomy &#38; Astrophysics. 706, A165.","ieee":"G. Kotiwale <i>et al.</i>, “Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 706. EDP Sciences, 2026.","apa":"Kotiwale, G., Matthee, J. J., Kashino, D., Vijayan, A. P., Torralba Torregrosa, A., Di Cesare, C., … Sobral, D. (2026). Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202556597\">https://doi.org/10.1051/0004-6361/202556597</a>","ama":"Kotiwale G, Matthee JJ, Kashino D, et al. Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2026;706. doi:<a href=\"https://doi.org/10.1051/0004-6361/202556597\">10.1051/0004-6361/202556597</a>"},"scopus_import":"1","acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations were taken under programmes # 1243, # 1933 and # 3516. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. GK acknowledges support from the Foundation MERAC. APV acknowledge support from the Sussex Astronomy Centre STFC Consolidated Grant (ST/X001040/1).","article_type":"original","OA_place":"publisher","title":"Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"diamond","oa":1,"has_accepted_license":"1","abstract":[{"text":"We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies.","lang":"eng"}],"date_created":"2026-02-22T23:01:35Z","publication":"Astronomy & Astrophysics","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"PlanS_conform":"1","file_date_updated":"2026-02-24T07:46:47Z","DOAJ_listed":"1","type":"journal_article","date_updated":"2026-02-24T07:49:42Z","date_published":"2026-02-01T00:00:00Z","article_processing_charge":"No","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"EDP Sciences","ddc":["520"],"year":"2026","article_number":"A165","_id":"21341","external_id":{"arxiv":["2510.19959"]},"author":[{"last_name":"Kotiwale","full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","first_name":"Gauri"},{"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":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"first_name":"Aswin P.","full_name":"Vijayan, Aswin P.","last_name":"Vijayan"},{"last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","first_name":"Alberto","orcid":"0000-0001-5586-6950"},{"first_name":"Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"orcid":"0000-0001-8386-3546","first_name":"Edoardo","last_name":"Iani","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a"},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"last_name":"Leja","full_name":"Leja, Joel","first_name":"Joel"},{"full_name":"Maseda, Michael V.","last_name":"Maseda","first_name":"Michael V."},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"full_name":"Danhaive, A. Lola","last_name":"Danhaive","first_name":"A. Lola"},{"first_name":"Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete","first_name":"Benjamín"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"}],"intvolume":"       706","volume":706},{"intvolume":"         9","volume":9,"_id":"21342","external_id":{"arxiv":["2505.11263"]},"author":[{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"first_name":"Yijia","full_name":"Li, Yijia","last_name":"Li"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Chisholm","full_name":"Chisholm, John","first_name":"John"},{"last_name":"Pollock","full_name":"Pollock, Clara L.","first_name":"Clara L."},{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"full_name":"Johnson, Benjamin D.","last_name":"Johnson","first_name":"Benjamin D."},{"first_name":"Xuejian","last_name":"Shen","full_name":"Shen, Xuejian"},{"full_name":"Hviding, Raphael E.","last_name":"Hviding","first_name":"Raphael E."},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"},{"last_name":"Ganguly","full_name":"Ganguly, Arpita","first_name":"Arpita"},{"first_name":"Callum","last_name":"Witten","full_name":"Witten, Callum"},{"last_name":"Atek","full_name":"Atek, Hakim","first_name":"Hakim"},{"first_name":"Sirio","full_name":"Belli, Sirio","last_name":"Belli"},{"first_name":"Sownak","last_name":"Bose","full_name":"Bose, Sownak"},{"last_name":"Bouwens","full_name":"Bouwens, Rychard","first_name":"Rychard"},{"first_name":"Pratika","last_name":"Dayal","full_name":"Dayal, Pratika"},{"first_name":"Roberto","last_name":"Decarli","full_name":"Decarli, Roberto"},{"full_name":"De Graaff, Anna","last_name":"De Graaff","first_name":"Anna"},{"last_name":"Fudamoto","full_name":"Fudamoto, Yoshinobu","first_name":"Yoshinobu"},{"first_name":"Emma","last_name":"Giovinazzo","full_name":"Giovinazzo, Emma"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"last_name":"Illingworth","full_name":"Illingworth, Garth","first_name":"Garth"},{"full_name":"Inoue, Akio K.","last_name":"Inoue","first_name":"Akio K."},{"full_name":"Kane, Sarah G.","last_name":"Kane","first_name":"Sarah G."},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"last_name":"Leonova","full_name":"Leonova, Ecaterina","first_name":"Ecaterina"},{"last_name":"Marques-Chaves","full_name":"Marques-Chaves, Rui","first_name":"Rui"},{"last_name":"Meyer","full_name":"Meyer, Romain A.","first_name":"Romain A."},{"last_name":"Nelson","full_name":"Nelson, Erica J.","first_name":"Erica J."},{"first_name":"Guido","last_name":"Roberts-Borsani","full_name":"Roberts-Borsani, Guido"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Mauro","last_name":"Stefanon","full_name":"Stefanon, Mauro"},{"first_name":"Yuma","last_name":"Sugahara","full_name":"Sugahara, Yuma"},{"first_name":"Sune","full_name":"Toft, Sune","last_name":"Toft"},{"first_name":"Arjen","last_name":"Van Der Wel","full_name":"Van Der Wel, Arjen"},{"last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter","first_name":"Pieter"},{"last_name":"Walter","full_name":"Walter, Fabian","first_name":"Fabian"},{"full_name":"Watson, Darach","last_name":"Watson","first_name":"Darach"},{"first_name":"John R.","last_name":"Weaver","full_name":"Weaver, John R."},{"full_name":"Whitaker, Katherine E.","last_name":"Whitaker","first_name":"Katherine E."}],"project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"Maynooth Academic Publishing","ddc":["520"],"year":"2026","date_published":"2026-01-30T00:00:00Z","article_processing_charge":"No","abstract":[{"lang":"eng","text":"JWST has revealed a stunning population of bright galaxies at surprisingly early epochs, z > 10,\r\nwhere few such sources were expected. Here we present the most distant example of this class yet – MoM-z14, a luminous (MUV = −20.2) source in the COSMOS legacy field at zspec = 14.44+0.02−0.02 that expands the observational frontier to a mere 280 million years after the Big Bang. The redshift is confirmed with NIRSpec/prism spectroscopy through a sharp Lyman-α break and ≈ 3σ detections of five rest-UV emission lines. The number density of bright zspec ≈ 14 − 15 sources implied by our “Mirage or Miracle” survey spanning ≈ 350 arcmin2 is > 100× larger (182+329 −105×) than pre-JWST consensus models. The high EWs of UV lines (≈15−35˚A) signal a rising star-formation history, with a ≈10× increase in the last 5 Myr (SFR5Myr/SFR50Myr = 9.9 +3.0 −5.8). The source is extremely compact (circularized re = 74+15\r\n−12 pc), and yet elongated (b/a = 0.25+0.11−0.06), suggesting an AGN is not the dominant source of UV light. The steep UV slope (β = −2.5 +0.2 −0.2) implies negligible dust attenuation\r\nand a young stellar population. The absence of a strong damping wing provides tentative evidence that the immediate surroundings of MoM-z14 may be partially ionized at a redshift where virtually every reionization model predicts a ≈ 100% neutral fraction. The nitrogen emission and highly supersolar [N/C]> 1 hint at an abundance pattern similar to local globular clusters that may have once hosted luminous supermassive stars. Since this abundance pattern is also common among the most ancient stars born in the Milky Way, we may be directly witnessing the formation of such stars in dense clusters, connecting galaxy evolution across the entire sweep of cosmic time. "}],"date_created":"2026-02-22T23:01:35Z","publication":"The Open Journal of Astrophysics","publication_identifier":{"eissn":["2565-6120"]},"PlanS_conform":"1","type":"journal_article","date_updated":"2026-06-16T10:47:41Z","article_type":"original","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST","OA_type":"diamond","oa":1,"has_accepted_license":"1","main_file_link":[{"url":"https://doi.org/10.33232/001c.156033","open_access":"1"}],"status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"short":"R.P. Naidu, P.A. Oesch, G. Brammer, A. Weibel, Y. Li, J.J. Matthee, J. Chisholm, C.L. Pollock, K.E. Heintz, B.D. Johnson, X. Shen, R.E. Hviding, J. Leja, S. Tacchella, A. Ganguly, C. Witten, H. Atek, S. Belli, S. Bose, R. Bouwens, P. Dayal, R. Decarli, A. De Graaff, Y. Fudamoto, E. Giovinazzo, J.E. Greene, G. Illingworth, A.K. Inoue, S.G. Kane, I. Labbe, E. Leonova, R. Marques-Chaves, R.A. Meyer, E.J. Nelson, G. Roberts-Borsani, D. Schaerer, R.A. Simcoe, M. Stefanon, Y. Sugahara, S. Toft, A. Van Der Wel, P. Van Dokkum, F. Walter, D. Watson, J.R. Weaver, K.E. Whitaker, The Open Journal of Astrophysics 9 (2026).","mla":"Naidu, Rohan P., et al. “A Cosmic Miracle: A Remarkably Luminous Galaxy at Zspec = 14.44 Confirmed with JWST.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.156033\">10.33232/001c.156033</a>.","chicago":"Naidu, Rohan P., Pascal A. Oesch, Gabriel Brammer, Andrea Weibel, Yijia Li, Jorryt J Matthee, John Chisholm, et al. “A Cosmic Miracle: A Remarkably Luminous Galaxy at Zspec = 14.44 Confirmed with JWST.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.156033\">https://doi.org/10.33232/001c.156033</a>.","ista":"Naidu RP, Oesch PA, Brammer G, Weibel A, Li Y, Matthee JJ, Chisholm J, Pollock CL, Heintz KE, Johnson BD, Shen X, Hviding RE, Leja J, Tacchella S, Ganguly A, Witten C, Atek H, Belli S, Bose S, Bouwens R, Dayal P, Decarli R, De Graaff A, Fudamoto Y, Giovinazzo E, Greene JE, Illingworth G, Inoue AK, Kane SG, Labbe I, Leonova E, Marques-Chaves R, Meyer RA, Nelson EJ, Roberts-Borsani G, Schaerer D, Simcoe RA, Stefanon M, Sugahara Y, Toft S, Van Der Wel A, Van Dokkum P, Walter F, Watson D, Weaver JR, Whitaker KE. 2026. A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. The Open Journal of Astrophysics. 9.","ieee":"R. P. Naidu <i>et al.</i>, “A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026.","apa":"Naidu, R. P., Oesch, P. A., Brammer, G., Weibel, A., Li, Y., Matthee, J. J., … Whitaker, K. E. (2026). A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.156033\">https://doi.org/10.33232/001c.156033</a>","ama":"Naidu RP, Oesch PA, Brammer G, et al. A cosmic miracle: A remarkably luminous galaxy at zspec = 14.44 confirmed with JWST. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.156033\">10.33232/001c.156033</a>"},"acknowledgement":"We thank the two anonymous referees for their insightful comments that have strengthened this work. “Mirage or Miracle” is but the latest link in a long chain of surveys that have built COSMOS into a premier extragalactic legacy field. We are thankful to all the teams who have contributed to this legacy, particularly those mentioned in §3 for leading recent JWST programs whose imaging\r\nwe have incorporated in our analysis. We are grateful to Vasily Belokurov for help in compiling the Milky Way reference sample featured in Fig 8. We thank Danielle Berg for sharing a highly complete, highly decimalized NUV vacuum line list. We are grateful to our program’s NIRSpec reviewer, Dan Coe, and program coordinator, Allison Vick, for valuable input on our MSA design. We acknowledge illuminating conversations with Risa Wechsler and Chao-Lin Kuo about early reionization. RPN thanks Neil Pappalardo and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships in Physics, and for their enthusiasm and encouragement for seeking galaxies at the highest redshifts. RPN acknowledges funding from JWST program GO5224. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020 207349. Funded by the European Union (ERC, AGENTS, 101076224 and HEAVYMETAL, 101071865). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of\r\nthe European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. This work has also been supported by JSPS KAKENHI Grant Number 23H00131. HA acknowledges support from CNES, focused on the JWST mission, and the Programme National Cosmology and Galaxies (PNCG)\r\nof CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. HA is supported by the French National Research Agency (ANR) under the project FIRSTGAL, grant number ANR-24-CE31-0838. SB is supported by the UK Research and Innovation (UKRI) Future Leaders Fellowship [grant number MR/V023381/1]. R.D. acknowledges support from the INAF GO 2022\r\ngrant “The birth of the giants: JWST sheds light on the build-up of quasars at cosmic dawn” and by the PRIN MUR “2022935STW”, RFF M4.C2.1.1, CUP J53D23001570006 and C53D23000950006. Computations supporting this paper were run on MIT’s Engaging cluster. This publication made use of the NASA Astrophysical Data System for bibliographic information. Some of the data products presented herein were retrieved from the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is funded by the Danish National Research Foundation under grant DNRF140. Software used in developing this work includes: matplotlib (Hunter 2007), jupyter (Kluyver et al. 2016), IPython (P´erez & Granger 2007), numpy (Oliphant 2015), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy Collaboration et al. 2013).This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space\r\nTelescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program # 5224.","scopus_import":"1","month":"01","publication_status":"published","department":[{"_id":"JoMa"}],"day":"30","doi":"10.33232/001c.156033","arxiv":1,"oa_version":"Published Version","quality_controlled":"1","language":[{"iso":"eng"}]},{"volume":391,"intvolume":"       391","author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"}],"issue":"6787","_id":"21371","external_id":{"pmid":["41712710"]},"year":"2026","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"AAAS","article_processing_charge":"No","page":"767-768","date_published":"2026-02-19T00:00:00Z","pmid":1,"type":"journal_article","date_updated":"2026-03-02T09:15:45Z","abstract":[{"text":"There may be a newly identified early phase of supermassive black hole growth","lang":"eng"}],"publication":"Science","date_created":"2026-03-01T23:01:39Z","publication_identifier":{"eissn":["1095-9203"]},"article_type":"comment","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Black holes disguised as little red dots","OA_type":"closed access","scopus_import":"1","acknowledgement":"The author acknowledges the support from the European Union (European Research Council, AGENTS, 101076224).","status":"public","citation":{"chicago":"Matthee, Jorryt J. “Black Holes Disguised as Little Red Dots.” <i>Science</i>. AAAS, 2026. <a href=\"https://doi.org/10.1126/science.adz8603\">https://doi.org/10.1126/science.adz8603</a>.","mla":"Matthee, Jorryt J. “Black Holes Disguised as Little Red Dots.” <i>Science</i>, vol. 391, no. 6787, AAAS, 2026, pp. 767–68, doi:<a href=\"https://doi.org/10.1126/science.adz8603\">10.1126/science.adz8603</a>.","short":"J.J. Matthee, Science 391 (2026) 767–768.","ista":"Matthee JJ. 2026. Black holes disguised as little red dots. Science. 391(6787), 767–768.","ieee":"J. J. Matthee, “Black holes disguised as little red dots,” <i>Science</i>, vol. 391, no. 6787. AAAS, pp. 767–768, 2026.","ama":"Matthee JJ. Black holes disguised as little red dots. <i>Science</i>. 2026;391(6787):767-768. doi:<a href=\"https://doi.org/10.1126/science.adz8603\">10.1126/science.adz8603</a>","apa":"Matthee, J. J. (2026). Black holes disguised as little red dots. <i>Science</i>. AAAS. <a href=\"https://doi.org/10.1126/science.adz8603\">https://doi.org/10.1126/science.adz8603</a>"},"language":[{"iso":"eng"}],"oa_version":"None","quality_controlled":"1","corr_author":"1","month":"02","publication_status":"published","department":[{"_id":"JoMa"}],"day":"19","doi":"10.1126/science.adz8603"},{"article_processing_charge":"No","date_published":"2026-03-01T00:00:00Z","year":"2026","article_number":"A75","ddc":["520"],"project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"EDP Sciences","author":[{"last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","first_name":"Alberto","orcid":"0000-0001-5586-6950"},{"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":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Yuzo","last_name":"Ishikawa","full_name":"Ishikawa, Yuzo"},{"first_name":"Gabriel B.","full_name":"Brammer, Gabriel B.","last_name":"Brammer"},{"full_name":"Chang, Seok Jun","last_name":"Chang","first_name":"Seok Jun"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Anna","full_name":"De Graaff, Anna","last_name":"De Graaff"},{"first_name":"Francesco","full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio"},{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"first_name":"Jenny E.","full_name":"Greene, Jenny E.","last_name":"Greene"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"last_name":"Iani","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"first_name":"Vasily","full_name":"Kokorev, Vasily","last_name":"Kokorev"},{"last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","first_name":"Gauri"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"full_name":"Ma, Yilun","last_name":"Ma","first_name":"Yilun"},{"first_name":"Sara","last_name":"Mascia","full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín","last_name":"Navarrete"},{"first_name":"Erica","last_name":"Nelson","full_name":"Nelson, Erica"},{"last_name":"Oesch","full_name":"Oesch, Pascal","first_name":"Pascal"},{"last_name":"Simcoe","full_name":"Simcoe, Robert A.","first_name":"Robert A."},{"first_name":"Stijn","last_name":"Wuyts","full_name":"Wuyts, Stijn"}],"_id":"21451","external_id":{"arxiv":["2510.00103"]},"volume":707,"intvolume":"       707","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"arxiv":1,"department":[{"_id":"JoMa"}],"publication_status":"published","day":"01","doi":"10.1051/0004-6361/202557537","corr_author":"1","month":"03","scopus_import":"1","acknowledgement":"We thank the scientific referee for useful and constructive comments. We thank Ylva Götberg and Zoltan Haiman for insightful discussions about the physics of gaseous envelopes and accretion into black holes. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #5664. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Naidu RP, Ishikawa Y, Brammer GB, Chang SJ, Chisholm J, De Graaff A, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Gronke M, Iani E, Kokorev V, Kotiwale G, Kramarenko I, Ma Y, Mascia S, Navarrete B, Nelson E, Oesch P, Simcoe RA, Wuyts S. 2026. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. Astronomy &#38; Astrophysics. 707, A75.","short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, R.P. Naidu, Y. Ishikawa, G.B. Brammer, S.J. Chang, J. Chisholm, A. De Graaff, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, M. Gronke, E. Iani, V. Kokorev, G. Kotiwale, I. Kramarenko, Y. Ma, S. Mascia, B. Navarrete, E. Nelson, P. Oesch, R.A. Simcoe, S. Wuyts, Astronomy &#38; Astrophysics 707 (2026).","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Rohan P. Naidu, Yuzo Ishikawa, Gabriel B. Brammer, Seok Jun Chang, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>.","mla":"Torralba Torregrosa, Alberto, et al. “The Warm Outer Layer of a Little Red Dot as the Source of [Fe Ii] and Collisional Balmer Lines with Scattering Wings.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A75, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557537\">10.1051/0004-6361/202557537</a>","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Naidu, R. P., Ishikawa, Y., Brammer, G. B., … Wuyts, S. (2026). The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557537\">https://doi.org/10.1051/0004-6361/202557537</a>","ieee":"A. Torralba Torregrosa <i>et al.</i>, “The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026."},"file":[{"file_name":"2026_AstronomyAstrophysics_Torralba2.pdf","file_id":"21460","date_created":"2026-03-16T10:57:49Z","creator":"dernst","file_size":2510157,"date_updated":"2026-03-16T10:57:49Z","access_level":"open_access","success":1,"checksum":"fcab9cb3dcf1d68612e1fdc8191643c1","relation":"main_file","content_type":"application/pdf"}],"status":"public","has_accepted_license":"1","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"The warm outer layer of a little red dot as the source of [Fe ii] and collisional Balmer lines with scattering wings","OA_type":"diamond","article_type":"original","OA_place":"publisher","type":"journal_article","DOAJ_listed":"1","date_updated":"2026-03-16T10:59:16Z","PlanS_conform":"1","file_date_updated":"2026-03-16T10:57:49Z","date_created":"2026-03-15T23:01:36Z","publication":"Astronomy & Astrophysics","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"abstract":[{"text":"The population of the little red dots (LRDs) may represent a key phase of supermassive black hole (SMBH) growth. A cocoon of dense excited gas is emerging as a key component to explain the most striking properties of LRDs, such as strong Balmer breaks and Balmer absorption, as well as the weak IR emission. To dissect the structure of LRDs, we analyzed new deep JWST/NIRSpec PRISM and G395H spectra of FRESCO-GN-9771, one of the most luminous known LRDs at z = 5.5. These spectra reveal a strong Balmer break, broad Balmer lines, and very narrow [O III] emission. We revealed a forest of optical [Fe II] lines, which we argue are emerging from a dense (nH = 109 − 10 cm−3) warm layer with electron temperature Te ≈ 7000 K. The broad wings of Hα and Hβ have an exponential profile due to electron scattering in this same layer. The high Hα : Hβ : Hγ flux ratio of ≈10.4 : 1 : 0.14 is an indicator of collisional excitation and resonant scattering dominating the Balmer line emission. A narrow Hγ component, unseen in the other two Balmer lines due to outshining by the broad components, could trace the ISM of a normal host galaxy with a star formation rate of ∼5 M⊙ yr−1. The warm layer is mostly opaque to Balmer transitions, producing a characteristic P Cygni profile in the line centers suggesting outflowing motions. This same layer is responsible for shaping the Balmer break. The broadband spectrum can be reasonably matched by a simple photoionized slab model that dominates the λ > 1500 Å continuum and a low-mass (∼108 M⊙) galaxy that could explain the narrow [O III], with only a subdominant contribution to the UV continuum. Our findings indicate that Balmer lines are not directly tracing the gas kinematics near the SMBH and that the BH mass scale is likely much lower than virial indicators suggest.","lang":"eng"}]},{"date_created":"2026-03-15T23:01:36Z","publication":"Astronomy & Astrophysics","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"abstract":[{"text":"Galaxies exhibit a tight correlation between their star formation rate (SFR) and stellar mass over a wide redshift range known as the star-forming main sequence (SFMS). With JWST, the SFMS can now be investigated at high redshifts down to masses of ∼106 M⊙, using sensitive star formation rate tracers such as the Hα emission, which allow us to probe the variability in the star formation histories. We present inferences of the SFMS based on 316 Hα-selected galaxies at z ∼ 4 − 5 with log(M★/M⊙) = 6.4 − 10.6. These galaxies were identified behind the Abell 2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M★α, with α = 0.45). After we corrected this for the Hα-flux limited nature of our survey using a Bayesian framework, the slope steepened to α = 0.59+0.10−0.09, whereas current data on their own are inconclusive on the mass dependence of the scatter. These slopes differ significantly from the slope of ∼1 that is expected from the observed evolution of the galaxy stellar mass function and from simulations. When we fixed the slope to α = 1, we found evidence for a decreasing intrinsic scatter with stellar mass (from ∼0.5 dex at M★ = 108 M⊙ to 0.4 dex at M★ = 1010 M⊙). This difference might be explained by a (combination of) luminosity-dependent SFR(Hα) calibration, a population of (mini)-quenched low-mass galaxies, or underestimated dust attenuation in high-mass galaxies. Future deep observations with different facilities can quantify these processes, which will enable us to achieve better insights into the variability of the star formation histories.","lang":"eng"}],"type":"journal_article","DOAJ_listed":"1","date_updated":"2026-03-16T10:52:44Z","PlanS_conform":"1","file_date_updated":"2026-03-16T10:48:07Z","title":"The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"diamond","article_type":"original","OA_place":"publisher","oa":1,"has_accepted_license":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"file":[{"date_created":"2026-03-16T10:48:07Z","file_id":"21459","file_name":"2026_AstronomyAstrophysics_DiCesare.pdf","date_updated":"2026-03-16T10:48:07Z","creator":"dernst","file_size":1821411,"access_level":"open_access","success":1,"content_type":"application/pdf","checksum":"c056b00ce7324849754521fde10fb7ca","relation":"main_file"}],"citation":{"mla":"Di Cesare, Claudia, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A129, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>.","chicago":"Di Cesare, Claudia, Jorryt J Matthee, Rohan P. Naidu, Alberto Torralba, Gauri Kotiwale, Ivan Kramarenko, Jeremy Blaizot, et al. “The Slope and Scatter of the Star-Forming Main Sequence at z ∼ 5: Reconciling Observations with Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>.","short":"C. Di Cesare, J.J. Matthee, R.P. Naidu, A. Torralba, G. Kotiwale, I. Kramarenko, J. Blaizot, J. Rosdahl, J. Leja, E. Iani, A. Adamo, A. Covelo-Paz, L.J. Furtak, K.E. Heintz, S. Mascia, B. Navarrete, P.A. Oesch, M. Romano, I. Shivaei, S. Tacchella, Astronomy &#38; Astrophysics 707 (2026).","ista":"Di Cesare C, Matthee JJ, Naidu RP, Torralba A, Kotiwale G, Kramarenko I, Blaizot J, Rosdahl J, Leja J, Iani E, Adamo A, Covelo-Paz A, Furtak LJ, Heintz KE, Mascia S, Navarrete B, Oesch PA, Romano M, Shivaei I, Tacchella S. 2026. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. Astronomy &#38; Astrophysics. 707, A129.","ieee":"C. Di Cesare <i>et al.</i>, “The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","ama":"Di Cesare C, Matthee JJ, Naidu RP, et al. The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557790\">10.1051/0004-6361/202557790</a>","apa":"Di Cesare, C., Matthee, J. J., Naidu, R. P., Torralba, A., Kotiwale, G., Kramarenko, I., … Tacchella, S. (2026). The slope and scatter of the star-forming main sequence at z ∼ 5: Reconciling observations with simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557790\">https://doi.org/10.1051/0004-6361/202557790</a>"},"status":"public","scopus_import":"1","acknowledgement":"We thank the anonymous referee for the insightful comments that helped improving the manuscript. We thank Romain. A. Meyer for valuable discussion, Pierluigi Rinaldi for his help with data handling and Luca Graziani and William McClymont for providing the dustyGadget and\r\nTHESAN-ZOOM data, respectively. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program # 3516. We acknowledge funding from JWST program GO-3516. Software used in developing this work includes: matplotlib (Hunter 2007), numpy (Oliphant 2007), scipy (Virtanen et al. 2020), TOPCAT (Taylor 2005), and Astropy (Astropy Collaboration 2013).","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication_status":"published","day":"01","doi":"10.1051/0004-6361/202557790","month":"03","corr_author":"1","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"arxiv":1,"intvolume":"       707","volume":707,"external_id":{"arxiv":["2510.19044"]},"_id":"21452","author":[{"last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."},{"last_name":"Torralba","full_name":"Torralba, Alberto","first_name":"Alberto"},{"first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri","last_name":"Kotiwale"},{"first_name":"Ivan","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko"},{"first_name":"Jeremy","full_name":"Blaizot, Jeremy","last_name":"Blaizot"},{"first_name":"Joakim","last_name":"Rosdahl","full_name":"Rosdahl, Joakim"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","full_name":"Iani, Edoardo","last_name":"Iani","first_name":"Edoardo","orcid":"0000-0001-8386-3546"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"first_name":"Alba","full_name":"Covelo-Paz, Alba","last_name":"Covelo-Paz"},{"full_name":"Furtak, Lukas J.","last_name":"Furtak","first_name":"Lukas J."},{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"first_name":"Sara","full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia"},{"last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","first_name":"Benjamín"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"first_name":"Michael","full_name":"Romano, Michael","last_name":"Romano"},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"}],"ddc":["520"],"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"EDP Sciences","year":"2026","article_number":"A129","date_published":"2026-03-01T00:00:00Z","article_processing_charge":"No"},{"author":[{"first_name":"Ivan","orcid":"0000-0001-5346-6048","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan"},{"first_name":"J.","last_name":"Rosdahl","full_name":"Rosdahl, J."},{"last_name":"Blaizot","full_name":"Blaizot, J.","first_name":"J."},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Katz, H.","last_name":"Katz","first_name":"H."},{"full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia"}],"_id":"21481","external_id":{"arxiv":["2509.05403"]},"volume":707,"intvolume":"       707","article_processing_charge":"No","date_published":"2026-03-05T00:00:00Z","article_number":"A184","year":"2026","ddc":["520"],"publisher":"EDP Sciences","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"has_accepted_license":"1","oa":1,"OA_type":"diamond","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"H α as a tracer of star formation in the SPHINX cosmological simulations","OA_place":"publisher","article_type":"original","date_updated":"2026-03-23T15:46:31Z","DOAJ_listed":"1","type":"journal_article","file_date_updated":"2026-03-23T15:44:09Z","PlanS_conform":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_created":"2026-03-23T14:58:03Z","publication":"Astronomy & Astrophysics","abstract":[{"text":"The Hα emission line in galaxies is a powerful tracer of their recent star formation activity. With the advent of JWST, we are now able to routinely observe Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs leads to biased results because high-redshift galaxies are commonly characterized by low metallicities and bursty star formation histories, affecting the conversion factor between the Hα luminosity (LHα) and the SFR. We developed a set of new SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3 with very little error. We used the SPHINX cosmological simulations to select a sample of star-forming galaxies representative of the Hα-emitter population observed with JWST. We then derived linear corrections to the classical SFR(Hα) calibrations that took variations in the physical properties (e.g., stellar metallicities) among individual galaxies into account. We obtained two new SFR(Hα) calibrations that compared to the classical calibrations reduce the root mean squared error (RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively. Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show that the new calibrations affect the high-redshift galaxy population statistics: (i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.","lang":"eng"}],"quality_controlled":"1","language":[{"iso":"eng"}],"oa_version":"Published Version","arxiv":1,"doi":"10.1051/0004-6361/202557114","day":"05","publication_status":"published","department":[{"_id":"JoMa"}],"corr_author":"1","month":"03","acknowledgement":"We thank the anonymous referee for the insightful comments that helped improve the manuscript. We also thank Thibault Garel, Pascal Oesch, Irene Shivaei, Charlotte Simmonds, Andrew Hopkins, Daniel Schaerer, and Rashmi Gottumukkala for useful comments and productive discussions. We gratefully acknowledge support from the CBPsmn (PSMN, Pôle Scientifique de Modélisation Numérique) of the ENS de Lyon for the computing resources.\r\nFunded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work made extensive use of several open-source software packages, and we gratefully acknowledge the efforts of their authors: numpy (Harris et al. 2020), astropy (Astropy Collaboration 2022), matplotlib (Hunter 2007), ipython (Perez & Granger 2007), and scikit-learn (Pedregosa et al. 2011).","citation":{"chicago":"Kramarenko, Ivan, J. Rosdahl, J. Blaizot, Jorryt J Matthee, H. Katz, and Claudia Di Cesare. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>.","mla":"Kramarenko, Ivan, et al. “H α as a Tracer of Star Formation in the SPHINX Cosmological Simulations.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A184, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>.","short":"I. Kramarenko, J. Rosdahl, J. Blaizot, J.J. Matthee, H. Katz, C. Di Cesare, Astronomy &#38; Astrophysics 707 (2026).","ista":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. 2026. H α as a tracer of star formation in the SPHINX cosmological simulations. Astronomy &#38; Astrophysics. 707, A184.","ieee":"I. Kramarenko, J. Rosdahl, J. Blaizot, J. J. Matthee, H. Katz, and C. Di Cesare, “H α as a tracer of star formation in the SPHINX cosmological simulations,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","apa":"Kramarenko, I., Rosdahl, J., Blaizot, J., Matthee, J. J., Katz, H., &#38; Di Cesare, C. (2026). H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202557114\">https://doi.org/10.1051/0004-6361/202557114</a>","ama":"Kramarenko I, Rosdahl J, Blaizot J, Matthee JJ, Katz H, Di Cesare C. H α as a tracer of star formation in the SPHINX cosmological simulations. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202557114\">10.1051/0004-6361/202557114</a>"},"file":[{"creator":"dernst","file_size":904565,"date_updated":"2026-03-23T15:44:09Z","file_name":"2026_AstronomyAstrophysics_Kramarenko.pdf","file_id":"21492","date_created":"2026-03-23T15:44:09Z","checksum":"7429076b381dd498084f40ffd199e714","relation":"main_file","content_type":"application/pdf","access_level":"open_access","success":1}],"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"status":"public"},{"article_number":"129","year":"2026","publisher":"IOP Publishing","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"ddc":["520"],"article_processing_charge":"Yes","date_published":"2026-01-10T00:00:00Z","volume":996,"intvolume":"       996","author":[{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"first_name":"David J.","full_name":"Setton, David J.","last_name":"Setton"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Volonteri","full_name":"Volonteri, Marta","first_name":"Marta"},{"first_name":"Pratika","full_name":"Dayal, Pratika","last_name":"Dayal"},{"full_name":"Labbe, Ivo","last_name":"Labbe","first_name":"Ivo"},{"first_name":"Pieter","full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum"},{"full_name":"Bezanson, Rachel","last_name":"Bezanson","first_name":"Rachel"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"last_name":"Cutler","full_name":"Cutler, Sam E.","first_name":"Sam E."},{"first_name":"Karl","full_name":"Glazebrook, Karl","last_name":"Glazebrook"},{"first_name":"Anna","last_name":"De Graaff","full_name":"De Graaff, Anna"},{"first_name":"Michaela","last_name":"Hirschmann","full_name":"Hirschmann, Michaela"},{"full_name":"Hviding, Raphael E.","last_name":"Hviding","first_name":"Raphael E."},{"last_name":"Kokorev","full_name":"Kokorev, Vasily","first_name":"Vasily"},{"first_name":"Joel","last_name":"Leja","full_name":"Leja, Joel"},{"first_name":"Hanpu","full_name":"Liu, Hanpu","last_name":"Liu"},{"first_name":"Yilun","last_name":"Ma","full_name":"Ma, Yilun"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"first_name":"Richard","full_name":"Pan, Richard","last_name":"Pan"},{"full_name":"Price, Sedona H.","last_name":"Price","first_name":"Sedona H."},{"first_name":"Justin S.","full_name":"Spilker, Justin S.","last_name":"Spilker"},{"full_name":"Wang, Bingjie","last_name":"Wang","first_name":"Bingjie"},{"first_name":"John R.","full_name":"Weaver, John R.","last_name":"Weaver"},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"},{"last_name":"Zitrin","full_name":"Zitrin, Adi","first_name":"Adi"}],"_id":"21715","issue":"2","external_id":{"arxiv":["2509.05434"]},"acknowledgement":"We benefit from the following JWST programs: UNCOVER (JWST/GO #2561; Labbé & Bezanson); ALT (JWST-GO #3516; Naidu & Matthee); MegaScience (JWST-GO #4111; Suess); RUBIES (JWST-GO #4233; de Graaff & Brammer); PRIMER (JWST/GO #1837; Dunlop).\r\n\r\nWe acknowledge funding from NSF/AAG #2306950, JWST-GO-02561, JWST-GO-03516, and JWST-GO-04111, provided through a grant from the STScI under NASA contract NAS5-03127. I.L. acknowledges support from Australian Research Council Future Fellowship FT220100798. K.G. and T.N. acknowledge support from Australian Research Council Laureate Fellowship FL180100060. A.Z. acknowledges support by grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF); by the Ministry of Science & Technology, Israel; and by the Israel Science Foundation grant No. 864/23. J.M. and I.K. are funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are, however, those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Y.F. acknowledges support from JSPS KAKENHI grant No. JSPS KAKENHI grant Nos. JP22K21349 and JP23K13149. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. Support for this work for RPN was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. J.M. acknowledges funding by the European Union (ERC, AGENTS, 101076224). R.E.H. acknowledges support by the German Aerospace Center (DLR) and the Federal Ministry for Economic Affairs and Energy (BMWi) through program 50OR2403 “RUBIES.”","scopus_import":"1","status":"public","file":[{"file_size":684400,"creator":"dernst","date_updated":"2026-05-04T11:19:48Z","file_name":"2026_AstrophysicalJour_Greene.pdf","file_id":"21792","date_created":"2026-05-04T11:19:48Z","relation":"main_file","checksum":"7b3cb025d4bcaa35c6e52bd0c8fb6cf4","content_type":"application/pdf","success":1,"access_level":"open_access"}],"citation":{"ista":"Greene JE, Setton DJ, Furtak LJ, Naidu RP, Volonteri M, Dayal P, Labbe I, Van Dokkum P, Bezanson R, Brammer G, Cutler SE, Glazebrook K, De Graaff A, Hirschmann M, Hviding RE, Kokorev V, Leja J, Liu H, Ma Y, Matthee JJ, Nanayakkara T, Oesch PA, Pan R, Price SH, Spilker JS, Wang B, Weaver JR, Whitaker KE, Williams CC, Zitrin A. 2026. What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. The Astrophysical Journal. 996(2), 129.","short":"J.E. Greene, D.J. Setton, L.J. Furtak, R.P. Naidu, M. Volonteri, P. Dayal, I. Labbe, P. Van Dokkum, R. Bezanson, G. Brammer, S.E. Cutler, K. Glazebrook, A. De Graaff, M. Hirschmann, R.E. Hviding, V. Kokorev, J. Leja, H. Liu, Y. Ma, J.J. Matthee, T. Nanayakkara, P.A. Oesch, R. Pan, S.H. Price, J.S. Spilker, B. Wang, J.R. Weaver, K.E. Whitaker, C.C. Williams, A. Zitrin, The Astrophysical Journal 996 (2026).","mla":"Greene, Jenny E., et al. “What You See Is What You Get: Empirically Measured Bolometric Luminosities of Little Red Dots.” <i>The Astrophysical Journal</i>, vol. 996, no. 2, 129, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1836\">10.3847/1538-4357/ae1836</a>.","chicago":"Greene, Jenny E., David J. Setton, Lukas J. Furtak, Rohan P. Naidu, Marta Volonteri, Pratika Dayal, Ivo Labbe, et al. “What You See Is What You Get: Empirically Measured Bolometric Luminosities of Little Red Dots.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae1836\">https://doi.org/10.3847/1538-4357/ae1836</a>.","apa":"Greene, J. E., Setton, D. J., Furtak, L. J., Naidu, R. P., Volonteri, M., Dayal, P., … Zitrin, A. (2026). What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae1836\">https://doi.org/10.3847/1538-4357/ae1836</a>","ama":"Greene JE, Setton DJ, Furtak LJ, et al. What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots. <i>The Astrophysical Journal</i>. 2026;996(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae1836\">10.3847/1538-4357/ae1836</a>","ieee":"J. E. Greene <i>et al.</i>, “What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots,” <i>The Astrophysical Journal</i>, vol. 996, no. 2. IOP Publishing, 2026."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"arxiv":1,"language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","month":"01","day":"10","doi":"10.3847/1538-4357/ae1836","publication_status":"published","department":[{"_id":"JoMa"}],"file_date_updated":"2026-05-04T11:19:48Z","PlanS_conform":"1","date_updated":"2026-05-04T11:20:42Z","DOAJ_listed":"1","type":"journal_article","abstract":[{"lang":"eng","text":"New populations of red active galactic nuclei (known as “little red dots”) discovered by JWST exhibit remarkable spectral energy distributions. Leveraging X-ray through far-infrared observations of two of the most luminous known little red dots, we directly measure their bolometric luminosities. We find evidence that more than half of the bolometric luminosity likely emerges in the rest-frame optical, with Lbol/L5100 = 5, roughly half the value for “standard” active galactic nuclei. Meanwhile, the X-ray emitting corona, UV-emitting blackbody, and reprocessed mid to far-infrared emission are all considerably subdominant, assuming that the far-infrared luminosity is well below current measured limits. We present new bolometric corrections that dramatically lower inferred bolometric luminosities by a factor of 10 compared to published values in the literature. These bolometric corrections are in accord with expectations from models in which gas absorption and reprocessing are responsible for the red rest-frame optical colors of little red dots. We discuss how this lowered luminosity scale suggests a lower mass scale for the population by at least an order of magnitude (e.g., ∼105–107 M⊙ black holes, and ∼108 M⊙ galaxies), alleviating tensions with clustering, overmassive black holes, and the integrated black hole mass density in the Universe."}],"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"date_created":"2026-04-12T22:01:50Z","publication":"The Astrophysical Journal","oa":1,"has_accepted_license":"1","OA_place":"publisher","article_type":"original","OA_type":"gold","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"What you see is what you get: Empirically measured bolometric luminosities of Little Red Dots"},{"language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","arxiv":1,"doi":"10.3847/2041-8213/ae58a5","day":"10","department":[{"_id":"ZoHa"},{"_id":"JoMa"}],"publication_status":"published","month":"04","acknowledgement":"We thank Earl Bellinger, Fabio Pacucci, Andrea Ferrara, and Dale Kocevski for useful discussions. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These imaging observations are associated with programs 1345, 1180, 1181, 1243, 6882, 2561, 1324, 4111, and 1895. The compiled dataset can be accessed at doi:10.17909/1m8f-9c47. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. J.M. and A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). This work was performed in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-2210452. This work used the following Python packages: Matplotlib (J. D. Hunter 2007), SciPy (P. Virtanen et al. 2020), NumPy (S. van der Walt et al. 2011), AstroPy (Astropy Collaboration et al. 2022), colossus (B. Diemer 2018), and photutils (L. Bradley et al. 2025).","scopus_import":"1","file":[{"checksum":"8c31d8603cd6ad39c772a72d136dc3f8","relation":"main_file","content_type":"application/pdf","access_level":"open_access","success":1,"creator":"dernst","file_size":13359642,"date_updated":"2026-05-11T06:44:37Z","file_name":"2026_AstrophysicalJourLetters_Baggen.pdf","file_id":"21851","date_created":"2026-05-11T06:44:37Z"}],"citation":{"short":"J.F.W. Baggen, M.T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, J.J. Matthee, The Astrophysical Journal Letters 1002 (2026).","chicago":"Baggen, Josephine F.W., Matthew T. Scoggins, Pieter Van Dokkum, Zoltán Haiman, Alberto Torralba Torregrosa, and Jorryt J Matthee. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">https://doi.org/10.3847/2041-8213/ae58a5</a>.","mla":"Baggen, Josephine F. W., et al. “Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman–Werner Sources Enabling Direct-Collapse Black Hole Formation.” <i>The Astrophysical Journal Letters</i>, vol. 1002, no. 1, L4, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">10.3847/2041-8213/ae58a5</a>.","ista":"Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. 2026. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. The Astrophysical Journal Letters. 1002(1), L4.","ieee":"J. F. W. Baggen, M. T. Scoggins, P. Van Dokkum, Z. Haiman, A. Torralba Torregrosa, and J. J. Matthee, “Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation,” <i>The Astrophysical Journal Letters</i>, vol. 1002, no. 1. IOP Publishing, 2026.","ama":"Baggen JFW, Scoggins MT, Van Dokkum P, Haiman Z, Torralba Torregrosa A, Matthee JJ. Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. <i>The Astrophysical Journal Letters</i>. 2026;1002(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">10.3847/2041-8213/ae58a5</a>","apa":"Baggen, J. F. W., Scoggins, M. T., Van Dokkum, P., Haiman, Z., Torralba Torregrosa, A., &#38; Matthee, J. J. (2026). Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae58a5\">https://doi.org/10.3847/2041-8213/ae58a5</a>"},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"status":"public","oa":1,"has_accepted_license":"1","OA_type":"gold","title":"Connecting the dots: UV-bright companions of Little Red Dots as Lyman–Werner sources enabling direct-collapse Black Hole formation","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_place":"publisher","article_type":"original","date_updated":"2026-05-11T06:48:33Z","DOAJ_listed":"1","type":"journal_article","PlanS_conform":"1","file_date_updated":"2026-05-11T06:44:37Z","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"publication":"The Astrophysical Journal Letters","date_created":"2026-05-10T22:02:15Z","abstract":[{"lang":"eng","text":"We compile a sample of 83 little red dots (LRDs) with JWST imaging and find that a substantial fraction (∼43%, rising to ≳80% for the most luminous LRDs) host one or more spatially offset, UV-bright companions at projected separations of 0.5 kpc ≲ d ≲ 5 kpc, with median 〈d〉 = 1.0 kpc. This fraction is even higher when smaller spatial scales are probed at high signal-to-noise ratio: the two most strongly lensed LRDs, A383-LRD1 and the newly discovered A68-LRD1, both have UV-bright companions at separations of only d ∼ 0.3 kpc, below the resolution limit of most unlensed JWST samples. We explore whether these ubiquitous red/blue configurations may be physically linked to the formation of LRDs, in analogy with the “synchronized pair” scenario originally proposed for direct-collapse black hole formation. In this picture, UV radiation from the companions, with typically modest stellar masses (M∗ ∼ 108−109 M⊙), suppresses molecular hydrogen cooling in nearby gas, allowing nearly isothermal collapse and the formation of extremely compact objects, such as massive black holes, supermassive stars, or quasi-stars. Using component-resolved photometry and spectral energy distribution modeling, we infer Lyman–Werner radiation fields of J21,LW ∼ 102.5–105 at the locations of the red components, comparable to those required in direct-collapse models, suggesting that the necessary photodissociation conditions are realized in many LRD systems. This framework provides a simple and self-consistent explanation for the extreme compactness and distinctive spectral properties of LRDs and links long-standing theoretical models for early compact object formation directly to a population now observed with JWST in the early Universe."}],"article_processing_charge":"Yes","date_published":"2026-04-10T00:00:00Z","article_number":"L4","year":"2026","ddc":["520"],"publisher":"IOP Publishing","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"author":[{"first_name":"Josephine F.W.","last_name":"Baggen","full_name":"Baggen, Josephine F.W."},{"full_name":"Scoggins, Matthew T.","last_name":"Scoggins","first_name":"Matthew T."},{"last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter","first_name":"Pieter"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","first_name":"Zoltán"},{"first_name":"Alberto","orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","last_name":"Torralba Torregrosa"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"}],"issue":"1","_id":"21846","external_id":{"arxiv":["2602.02702"]},"volume":1002,"intvolume":"      1002"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot","OA_type":"diamond","article_type":"original","OA_place":"publisher","oa":1,"has_accepted_license":"1","date_created":"2026-06-07T22:01:36Z","publication":"The Open Journal of Astrophysics","publication_identifier":{"eissn":["2565-6120"]},"abstract":[{"lang":"eng","text":"The central engines of Little Red Dots (LRDs) may be “black hole stars” (BH*s), early stages of\r\nblack hole growth characterized by dense gas envelopes. So far, the most direct evidence for BH*s\r\ncomes from a handful of sources where the host galaxy is completely outshone as suggested by their\r\nremarkably steep Balmer breaks. Here we present a novel scheme to disentangle BH*s from their\r\nhost galaxies assuming that the [O III]5008˚A line arises exclusively from the host. Using a sample\r\nof 98 LRDs (z ≈ 2 − 9) with high quality NIRSpec/PRISM spectra, we demonstrate that the hostsubtracted median stack displays a Balmer break > 2× stronger than massive quiescent galaxies,\r\nwith the rest-optical continuum resembling a blackbody-like SED (Teff ≈ 4050 K, log(Lbol) ≈ 43.9\r\nerg s−1\r\n, Reff ≈ 1300 au). We measure a steep Balmer decrement (Hα/Hβ > 10) and numerous\r\ndensity-sensitive features (e.g., Fe II, He I, O I). These are hallmark signatures of dense gas envelopes,\r\nproviding population-level evidence that BH*s indeed power LRDs. In the median LRD, BH*s account\r\nfor ∼ 20% of the UV emission, ∼ 50% at the Balmer break, and ∼ 90% at wavelengths longer\r\nthan Hα with the remainder arising from the host. BH*s preferentially reside in low-mass galaxies\r\n(M⋆ ≈ 108 M⊙) undergoing recent starbursts, as evidenced by extreme emission line EWs (e.g.,\r\n[O III]5008˚A≈ 1100˚A, C III]≈ 12˚A), thereby favoring BH* origins linked to star-formation. We show\r\nV-shaped LRD selections are biased to high BH*/host fractions (≳ 60% at 5500˚A) – less dominant\r\nBH*s may be powering JWST’s blue broad-line AGN. We find BH*s are so commonplace and transient\r\n(duty cycle ∼ 1%, lifetime ∼ 10 Myrs) that every massive black hole may have once shone as a BH*.\r\n"}],"type":"journal_article","DOAJ_listed":"1","date_updated":"2026-06-08T08:25:40Z","file_date_updated":"2026-06-08T08:23:37Z","PlanS_conform":"1","department":[{"_id":"JoMa"}],"publication_status":"published","day":"25","doi":"10.33232/001c.162505","month":"05","quality_controlled":"1","language":[{"iso":"eng"}],"oa_version":"Published Version","arxiv":1,"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"file":[{"success":1,"access_level":"open_access","relation":"main_file","checksum":"33c4a444f7c37b3f47ecbd53eb187c1b","content_type":"application/pdf","file_name":"2026_OpenJourAstrophysics_Sun.pdf","file_id":"21952","date_created":"2026-06-08T08:23:37Z","file_size":7591188,"creator":"dernst","date_updated":"2026-06-08T08:23:37Z"}],"citation":{"ieee":"W. Q. Sun <i>et al.</i>, “Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026.","apa":"Sun, W. Q., Naidu, R. P., Matthee, J. J., De Graaff, A., Chisholm, J., Greene, J. E., … Williams, C. C. (2026). Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.162505\">https://doi.org/10.33232/001c.162505</a>","ama":"Sun WQ, Naidu RP, Matthee JJ, et al. Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.162505\">10.33232/001c.162505</a>","chicago":"Sun, Wendy Q., Rohan P. Naidu, Jorryt J Matthee, Anna De Graaff, John Chisholm, Jenny E. Greene, Pascal A. Oesch, et al. “Little Red Dot - Host Galaxy = Black Hole Star: A Gas-Enshrouded Heart at the Center of Every Little Red Dot.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.162505\">https://doi.org/10.33232/001c.162505</a>.","short":"W.Q. Sun, R.P. Naidu, J.J. Matthee, A. De Graaff, J. Chisholm, J.E. Greene, P.A. Oesch, A. Torralba Torregrosa, R.E. Hviding, G. Brammer, R.A. Simcoe, S. Bose, R. Bouwens, P. Dayal, A.C. Eilers, Q. Fei, L.J. Furtak, R. Gottumukkala, A. Goulding, K.E. Heintz, M. Hirschmann, V. Kokorev, J. Leja, Z. Liu, P. Natarajan, A.D. Santarelli, D.J. Setton, A. Smith, S. Tacchella, M. Volonteri, F. Walter, A. Weibel, C.C. Williams, The Open Journal of Astrophysics 9 (2026).","mla":"Sun, Wendy Q., et al. “Little Red Dot - Host Galaxy = Black Hole Star: A Gas-Enshrouded Heart at the Center of Every Little Red Dot.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.162505\">10.33232/001c.162505</a>.","ista":"Sun WQ, Naidu RP, Matthee JJ, De Graaff A, Chisholm J, Greene JE, Oesch PA, Torralba Torregrosa A, Hviding RE, Brammer G, Simcoe RA, Bose S, Bouwens R, Dayal P, Eilers AC, Fei Q, Furtak LJ, Gottumukkala R, Goulding A, Heintz KE, Hirschmann M, Kokorev V, Leja J, Liu Z, Natarajan P, Santarelli AD, Setton DJ, Smith A, Tacchella S, Volonteri M, Walter F, Weibel A, Williams CC. 2026. Little Red Dot - Host Galaxy = Black Hole Star: A gas-enshrouded heart at the center of every Little Red Dot. The Open Journal of Astrophysics. 9."},"status":"public","acknowledgement":"We thank the two anonymous referees for their insightful comments that have strengthened this work.\r\nWQS and RPN acknowledge funding from JWST programs GO-3516, GO-5224, and the MIT Undergraduate\r\nResearch Opportunities Program (UROP). Support for\r\nthis work was provided by NASA through the NASA\r\nHubble Fellowship grant HST-HF2-51515.001-A awarded\r\nby the Space Telescope Science Institute, which is operated by the Association of Universities for Research in\r\nAstronomy, Incorporated, under NASA contract NAS5-\r\n26555. RPN thanks Neil Pappalardo and Jane Pappalardo for their generous support of the MIT Pappalardo Fellowships in Physics, and for their enthusiasm\r\nand encouragement for pursuing the earliest galaxies and\r\nblack holes. JM and AT acknowledge funding from the\r\nEuropean Union (ERC, AGENTS, 101076224). KEH\r\nacknowledges support from the Independent Research Fund Denmark (DFF) under grant 5251-00009B and cofunding by the European Union (ERC, HEAVYMETAL,\r\n101071865). Views and opinions expressed are, however,\r\nthose of the authors only and do not necessarily reflect\r\nthose of the European Union or the European Research\r\nCouncil. Neither the European Union nor the granting\r\nauthority can be held responsible for them. REH acknowledges support by the German Aerospace Center\r\n(DLR) and the Federal Ministry for Economic Affairs\r\nand Energy (BMWi) through program 50OR2403 ‘RUBIES’.\r\nThe data products presented herein were retrieved\r\nfrom the Dawn JWST Archive (DJA). DJA is an initiative of the Cosmic Dawn Center (DAWN), which is\r\nfunded by the Danish National Research Foundation under grant DNRF140. This work is based on observations\r\nmade with the NASA/ESA/CSA James Webb Space\r\nTelescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope\r\nScience Institute, which is operated by the Association\r\nof Universities for Research in Astronomy, Inc., under\r\nNASA contract NAS 5-03127 for JWST. Support for\r\nprograms #3516, #5224, #5664 was provided by NASA\r\nthrough grants from the Space Telescope Science Institute, which is operated by the Association of Universities\r\nfor Research in Astronomy, Inc., under NASA contract\r\nNAS 5-03127.\r\nThe spectra used in this paper are associated with programs 1180 (D’Eugenio et al. 2025d), 1181 (PI: D. Eisenstein), 1208 (Willott et al. 2022), 1210 (PI: N. Luetzgendorf), 1211 (Maseda et al. 2024), 1212 - 1215 (PI: N.\r\nLuetzgendorf), 1228 (Luhman et al. 2024b), 1229 (Luhman et al. 2024a), 1286 (PI: N. Luetzgendorf), 1287 (PI:\r\nK. Isaak), 1345 (Finkelstein et al. 2023), 1433 (Hsiao\r\net al. 2024), 1747 (PI: G. Roberts-Borsani), 2028 (Wang\r\net al. 2024c), 2073 (PI: J. Hennawi), 2198 (Barrufet\r\net al. 2025), 2282 (Bradley et al. 2023), 2561 (Bezanson\r\net al. 2024), 2565 (Nanayakkara et al. 2025), 2640 (PI:\r\nW. Best), 2750 (Arrabal Haro et al. 2023), 2756 (Mascia et al. 2024), 2767 (Williams et al. 2023b), 2770 (PI:\r\nM. McCaughrean), 3073 (Castellano et al. 2024), 3215\r\n(Eisenstein et al. 2025), 4106 (PI: E. Nelson), 4233 (de\r\nGraaff et al. 2025c), 4446 (Frye et al. 2024), 4557 (PI: H.\r\nYan), 5105 (Shen et al. 2024), 5224 (PIs: P.A. Oesch &\r\nR.P. Naidu), 6368 (PI: M. Dickinson), 6541 (DeCoursey\r\net al. 2025), 6585 (PI: D. Coulter), 6642 (PI: J. Muzerolle\r\nPage), and FRESCO IFU (Matthee et al. 2024; Torralba\r\net al. 2025b).\r\nSoftware used in developing this work includes:\r\nmatplotlib (Hunter 2007), jupyter (Kluyver et al.\r\n2016), IPython (P´erez & Granger 2007), numpy\r\n(Oliphant 2015), scipy (Virtanen et al. 2020), TOPCAT\r\n(Taylor 2005), Astropy (Astropy Collaboration et al.\r\n2013), msaexp (Brammer 2023).","scopus_import":"1","external_id":{"arxiv":["2601.20929"]},"_id":"21951","author":[{"last_name":"Sun","full_name":"Sun, Wendy Q.","first_name":"Wendy Q."},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"full_name":"De Graaff, Anna","last_name":"De Graaff","first_name":"Anna"},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"first_name":"Jenny E.","last_name":"Greene","full_name":"Greene, Jenny E."},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"orcid":"0000-0001-5586-6950","first_name":"Alberto","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa"},{"first_name":"Raphael E.","full_name":"Hviding, Raphael E.","last_name":"Hviding"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"full_name":"Simcoe, Robert A.","last_name":"Simcoe","first_name":"Robert A."},{"full_name":"Bose, Sownak","last_name":"Bose","first_name":"Sownak"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"full_name":"Dayal, Pratika","last_name":"Dayal","first_name":"Pratika"},{"last_name":"Eilers","full_name":"Eilers, Anna Christina","first_name":"Anna Christina"},{"last_name":"Fei","full_name":"Fei, Qinyue","first_name":"Qinyue"},{"first_name":"Lukas J.","full_name":"Furtak, Lukas J.","last_name":"Furtak"},{"last_name":"Gottumukkala","full_name":"Gottumukkala, Rashmi","first_name":"Rashmi"},{"full_name":"Goulding, Andy","last_name":"Goulding","first_name":"Andy"},{"first_name":"Kasper E.","full_name":"Heintz, Kasper E.","last_name":"Heintz"},{"first_name":"Michaela","last_name":"Hirschmann","full_name":"Hirschmann, Michaela"},{"full_name":"Kokorev, Vasily","last_name":"Kokorev","first_name":"Vasily"},{"first_name":"Joel","full_name":"Leja, Joel","last_name":"Leja"},{"first_name":"Zhaoran","full_name":"Liu, Zhaoran","last_name":"Liu"},{"full_name":"Natarajan, Priyamvada","last_name":"Natarajan","first_name":"Priyamvada"},{"full_name":"Santarelli, Andrew D.","last_name":"Santarelli","first_name":"Andrew D."},{"full_name":"Setton, David J.","last_name":"Setton","first_name":"David J."},{"first_name":"Aaron","last_name":"Smith","full_name":"Smith, Aaron"},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"},{"full_name":"Volonteri, Marta","last_name":"Volonteri","first_name":"Marta"},{"first_name":"Fabian","full_name":"Walter, Fabian","last_name":"Walter"},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."}],"intvolume":"         9","volume":9,"date_published":"2026-05-25T00:00:00Z","article_processing_charge":"No","ddc":["520"],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"Maynooth Academic Publishing","year":"2026"},{"publisher":"Taylor & Francis","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"year":"2025","date_published":"2025-12-04T00:00:00Z","page":"116-151","article_processing_charge":"No","intvolume":"        66","volume":66,"external_id":{"arxiv":["2511.04843"]},"_id":"20864","issue":"1-4","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"}],"citation":{"ieee":"J. J. Matthee, “JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies,” <i>Contemporary Physics</i>, vol. 66, no. 1–4. Taylor &#38; Francis, pp. 116–151, 2025.","apa":"Matthee, J. J. (2025). JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. <i>Contemporary Physics</i>. Taylor &#38; Francis. <a href=\"https://doi.org/10.1080/00107514.2025.2586370\">https://doi.org/10.1080/00107514.2025.2586370</a>","ama":"Matthee JJ. JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. <i>Contemporary Physics</i>. 2025;66(1-4):116-151. doi:<a href=\"https://doi.org/10.1080/00107514.2025.2586370\">10.1080/00107514.2025.2586370</a>","mla":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” <i>Contemporary Physics</i>, vol. 66, no. 1–4, Taylor &#38; Francis, 2025, pp. 116–51, doi:<a href=\"https://doi.org/10.1080/00107514.2025.2586370\">10.1080/00107514.2025.2586370</a>.","chicago":"Matthee, Jorryt J. “JWST Provides a New View of Cosmic Dawn: Latest Developments in Studies of Early Galaxies.” <i>Contemporary Physics</i>. Taylor &#38; Francis, 2025. <a href=\"https://doi.org/10.1080/00107514.2025.2586370\">https://doi.org/10.1080/00107514.2025.2586370</a>.","short":"J.J. Matthee, Contemporary Physics 66 (2025) 116–151.","ista":"Matthee JJ. 2025. JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies. Contemporary Physics. 66(1–4), 116–151."},"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2511.04843","open_access":"1"}],"status":"public","scopus_import":"1","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).","day":"04","doi":"10.1080/00107514.2025.2586370","publication_status":"published","department":[{"_id":"JoMa"}],"month":"12","corr_author":"1","language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Preprint","arxiv":1,"publication_identifier":{"issn":["0010-7514"],"eissn":["1366-5812"]},"date_created":"2025-12-29T12:05:25Z","publication":"Contemporary Physics","abstract":[{"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.","lang":"eng"}],"date_updated":"2026-04-07T08:44:00Z","type":"journal_article","OA_type":"green","title":"JWST provides a new view of cosmic dawn: Latest developments in studies of early galaxies","user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","OA_place":"repository","article_type":"original","oa":1},{"author":[{"first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia"},{"first_name":"L.","full_name":"Pentericci, L.","last_name":"Pentericci"},{"last_name":"Llerena","full_name":"Llerena, M.","first_name":"M."},{"full_name":"Calabrò, A.","last_name":"Calabrò","first_name":"A."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"S.","last_name":"Flury","full_name":"Flury, S."},{"full_name":"Pacucci, F.","last_name":"Pacucci","first_name":"F."},{"full_name":"Jaskot, A.","last_name":"Jaskot","first_name":"A."},{"first_name":"R. O.","last_name":"Amorín","full_name":"Amorín, R. O."},{"last_name":"Bhatawdekar","full_name":"Bhatawdekar, R.","first_name":"R."},{"first_name":"M.","full_name":"Castellano, M.","last_name":"Castellano"},{"first_name":"N.","full_name":"Cleri, N.","last_name":"Cleri"},{"full_name":"Costantin, L.","last_name":"Costantin","first_name":"L."},{"first_name":"K.","last_name":"Davis","full_name":"Davis, K."},{"first_name":"Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"first_name":"M.","full_name":"Dickinson, M.","last_name":"Dickinson"},{"first_name":"A.","last_name":"Fontana","full_name":"Fontana, A."},{"last_name":"Guo","full_name":"Guo, Y.","first_name":"Y."},{"first_name":"M.","full_name":"Giavalisco, M.","last_name":"Giavalisco"},{"first_name":"B. W.","last_name":"Holwerda","full_name":"Holwerda, B. W."},{"full_name":"Hu, W.","last_name":"Hu","first_name":"W."},{"last_name":"Huertas-Company","full_name":"Huertas-Company, M.","first_name":"M."},{"last_name":"Jung","full_name":"Jung, Intae","first_name":"Intae"},{"first_name":"J.","last_name":"Kartaltepe","full_name":"Kartaltepe, J."},{"last_name":"Kashino","full_name":"Kashino, D.","first_name":"D."},{"first_name":"A. M.","last_name":"Koekemoer","full_name":"Koekemoer, A. M."},{"full_name":"Lucas, R. A.","last_name":"Lucas","first_name":"R. A."},{"full_name":"Lotz, J.","last_name":"Lotz","first_name":"J."},{"last_name":"Napolitano","full_name":"Napolitano, L.","first_name":"L."},{"first_name":"S.","last_name":"Jogee","full_name":"Jogee, S."},{"first_name":"S.","last_name":"Wilkins","full_name":"Wilkins, S."}],"external_id":{"arxiv":["2501.08268"]},"_id":"21060","volume":701,"intvolume":"       701","article_processing_charge":"No","date_published":"2025-09-01T00:00:00Z","year":"2025","article_number":"A122","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"publisher":"EDP Sciences","ddc":["520"],"has_accepted_license":"1","oa":1,"article_type":"original","OA_place":"publisher","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe","OA_type":"diamond","file_date_updated":"2026-02-09T07:28:08Z","PlanS_conform":"1","DOAJ_listed":"1","type":"journal_article","date_updated":"2026-02-09T07:33:46Z","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_created":"2026-01-28T15:24:24Z","publication":"Astronomy & Astrophysics","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"arxiv":1,"oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","month":"09","corr_author":"1","publication_status":"published","department":[{"_id":"JoMa"}],"doi":"10.1051/0004-6361/202553760","day":"01","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”.","scopus_import":"1","status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"ama":"Mascia S, Pentericci L, Llerena M, et al. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. 2025;701. doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>","apa":"Mascia, S., Pentericci, L., Llerena, M., Calabrò, A., Matthee, J. J., Flury, S., … Wilkins, S. (2025). Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>","ieee":"S. Mascia <i>et al.</i>, “Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 701. EDP Sciences, 2025.","ista":"Mascia S, Pentericci L, Llerena M, Calabrò A, Matthee JJ, Flury S, Pacucci F, Jaskot A, Amorín RO, Bhatawdekar R, Castellano M, Cleri N, Costantin L, Davis K, Di Cesare C, Dickinson M, Fontana A, Guo Y, Giavalisco M, Holwerda BW, Hu W, Huertas-Company M, Jung I, Kartaltepe J, Kashino D, Koekemoer AM, Lucas RA, Lotz J, Napolitano L, Jogee S, Wilkins S. 2025. Little impact of mergers and galaxy morphology on the production and escape of ionizing photons in the early Universe. Astronomy &#38; Astrophysics. 701, A122.","short":"S. Mascia, L. Pentericci, M. Llerena, A. Calabrò, J.J. Matthee, S. Flury, F. Pacucci, A. Jaskot, R.O. Amorín, R. Bhatawdekar, M. Castellano, N. Cleri, L. Costantin, K. Davis, C. Di Cesare, M. Dickinson, A. Fontana, Y. Guo, M. Giavalisco, B.W. Holwerda, W. Hu, M. Huertas-Company, I. Jung, J. Kartaltepe, D. Kashino, A.M. Koekemoer, R.A. Lucas, J. Lotz, L. Napolitano, S. Jogee, S. Wilkins, Astronomy &#38; Astrophysics 701 (2025).","mla":"Mascia, Sara, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 701, A122, EDP Sciences, 2025, doi:<a href=\"https://doi.org/10.1051/0004-6361/202553760\">10.1051/0004-6361/202553760</a>.","chicago":"Mascia, Sara, L. Pentericci, M. Llerena, A. Calabrò, Jorryt J Matthee, S. Flury, F. Pacucci, et al. “Little Impact of Mergers and Galaxy Morphology on the Production and Escape of Ionizing Photons in the Early Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2025. <a href=\"https://doi.org/10.1051/0004-6361/202553760\">https://doi.org/10.1051/0004-6361/202553760</a>."},"file":[{"checksum":"990e384ca19e14b35296712d3b9e2919","relation":"main_file","content_type":"application/pdf","access_level":"open_access","success":1,"creator":"dernst","file_size":9994234,"date_updated":"2026-02-09T07:28:08Z","file_name":"2025_AstronomyAstrophysics_Mascia.pdf","file_id":"21166","date_created":"2026-02-09T07:28:08Z"}]},{"OA_type":"gold","title":"Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_place":"publisher","article_type":"original","oa":1,"has_accepted_license":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_created":"2026-01-28T15:25:42Z","publication":"The Astrophysical Journal","abstract":[{"text":"JWST observations have unveiled faint active galactic nuclei (AGNs) at high redshift that provide insights into the formation of supermassive black holes (SMBHs). However, disentangling their stellar from AGN light is challenging. Here, we use an empirical approach to infer the average stellar mass of five faint broad-line (BL) Hα emitters at z = 4–5 with BH masses ≈6 × 10^6 M⊙, with a method independent of their spectral energy distribution (SED). We use the deep JWST/NIRcam grism survey “All the Little Things” to measure the overdensities around BL-Hα emitters and around a spectroscopic reference sample of ∼300 galaxies. In our reference sample, we find that megaparsec-scale overdensity correlates with stellar mass. Their large-scale environments suggest that BL-Hα emitters are hosted by galaxies with stellar masses ≈5 × 10^7 M⊙, ≈40 times lower than those inferred from galaxy-only SED fits. Adding measurements around more luminous z ≈ 6 AGNs, we find tentative correlations between line width, BH mass, and the overdensity, suggestive of a steep BH to halo mass relation. The main implications are (1) when BH masses are taken at face value, we confirm extremely high BH to stellar mass ratios of ≈10%, (2) the galaxies of low stellar mass that host growing SMBHs are in tension with typical hydrodynamical simulations, except those without feedback, (3) a 1% duty cycle implied by the host mass hints at super-Eddington accretion, (4) the masses are at odds with an interpretation of the line broadening in terms of high stellar density, (5) our results imply a luminosity-dependent diversity of galaxy masses, environments, and SEDs among AGN samples.","lang":"eng"}],"date_updated":"2026-02-09T08:22:01Z","DOAJ_listed":"1","type":"journal_article","PlanS_conform":"1","file_date_updated":"2026-02-09T08:20:14Z","doi":"10.3847/1538-4357/ade886","day":"29","department":[{"_id":"JoMa"}],"publication_status":"published","corr_author":"1","month":"07","language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","arxiv":1,"file":[{"relation":"main_file","checksum":"a49fbed72f2ff9c0b13129acb6f44f9d","content_type":"application/pdf","success":1,"access_level":"open_access","file_size":6237415,"creator":"dernst","date_updated":"2026-02-09T08:20:14Z","file_name":"2025_AstrophysicalJournal_Matthee.pdf","file_id":"21168","date_created":"2026-02-09T08:20:14Z"}],"citation":{"chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gauri Kotiwale, Lukas J. Furtak, Ivan Kramarenko, Ruari Mackenzie, Jenny Greene, et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>.","mla":"Matthee, Jorryt J., et al. “Environmental Evidence for Overly Massive Black Holes in Low-Mass Galaxies and a Black Hole–Halo Mass Relation at z ∼ 5.” <i>The Astrophysical Journal</i>, vol. 988, no. 2, 246, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>.","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.","ieee":"J. J. Matthee <i>et al.</i>, “Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5,” <i>The Astrophysical Journal</i>, vol. 988, no. 2. IOP Publishing, 2025.","ama":"Matthee JJ, Naidu RP, Kotiwale G, et al. Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. 2025;988(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ade886\">10.3847/1538-4357/ade886</a>","apa":"Matthee, J. J., Naidu, R. P., Kotiwale, G., Furtak, L. J., Kramarenko, I., Mackenzie, R., … Torralba Torregrosa, A. (2025). Environmental evidence for overly massive Black Holes in low-mass galaxies and a Black Hole–Halo mass relation at z ∼ 5. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ade886\">https://doi.org/10.3847/1538-4357/ade886</a>"},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"status":"public","scopus_import":"1","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).","_id":"21062","issue":"2","external_id":{"arxiv":["2412.02846"]},"author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"full_name":"Kotiwale, Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale","first_name":"Gauri"},{"last_name":"Furtak","full_name":"Furtak, Lukas J.","first_name":"Lukas J."},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","first_name":"Ivan"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"full_name":"Greene, Jenny","last_name":"Greene","first_name":"Jenny"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"last_name":"Bouwens","full_name":"Bouwens, Rychard J.","first_name":"Rychard J."},{"id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","last_name":"Di Cesare","first_name":"Claudia"},{"first_name":"Anna-Christina","last_name":"Eilers","full_name":"Eilers, Anna-Christina"},{"first_name":"Anna","full_name":"de Graaff, Anna","last_name":"de Graaff"},{"first_name":"Kasper E.","last_name":"Heintz","full_name":"Heintz, Kasper E."},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"full_name":"Tacchella, Sandro","last_name":"Tacchella","first_name":"Sandro"},{"last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","orcid":"0000-0001-5586-6950","first_name":"Alberto"}],"intvolume":"       988","volume":988,"date_published":"2025-07-29T00:00:00Z","article_processing_charge":"Yes","ddc":["520"],"publisher":"IOP Publishing","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"article_number":"246","year":"2025"},{"_id":"19066","issue":"3","external_id":{"isi":["001420026000001"],"arxiv":["2410.10974"]},"isi":1,"author":[{"last_name":"Claeyssens","full_name":"Claeyssens, Adélaïde","first_name":"Adélaïde"},{"full_name":"Adamo, Angela","last_name":"Adamo","first_name":"Angela"},{"full_name":"Messa, Matteo","last_name":"Messa","first_name":"Matteo"},{"last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava","first_name":"Miroslava"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."}],"intvolume":"       537","volume":537,"date_published":"2025-03-01T00:00:00Z","article_processing_charge":"No","page":"2535-2558","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"Oxford University Press","ddc":["520"],"year":"2025","article_type":"original","OA_place":"publisher","title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"gold","oa":1,"has_accepted_license":"1","abstract":[{"lang":"eng","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. "}],"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2025-02-23T23:01:55Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"file_date_updated":"2025-02-25T06:38:43Z","DOAJ_listed":"1","type":"journal_article","date_updated":"2026-02-16T11:51:48Z","month":"03","publication_status":"published","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"doi":"10.1093/mnras/staf058","day":"01","arxiv":1,"language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"apa":"Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J., Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>","ama":"Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(3):2535-2558. doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>","ieee":"A. Claeyssens <i>et al.</i>, “Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3. Oxford University Press, pp. 2535–2558, 2025.","ista":"Claeyssens A, Adamo A, Messa M, Dessauges-Zavadsky M, Richard J, Kramarenko I, Matthee JJ, Naidu RP. 2025. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. 537(3), 2535–2558.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>.","chicago":"Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky, Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>."},"file":[{"content_type":"application/pdf","relation":"main_file","checksum":"431aef05755e6b5472f5e9b4c326cf84","success":1,"access_level":"open_access","date_updated":"2025-02-25T06:38:43Z","file_size":35099276,"creator":"dernst","date_created":"2025-02-25T06:38:43Z","file_id":"19084","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf"}],"scopus_import":"1","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."},{"article_type":"original","OA_place":"publisher","title":"The light echo of a high-redshift quasar mapped with Lyα tomography","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"gold","oa":1,"has_accepted_license":"1","abstract":[{"text":"Ultraviolet (UV) radiation from accreting black holes ionizes the intergalactic gas around early quasars, carving out highly ionized bubbles in their surroundings. Any changes in a quasar’s luminosity are therefore predicted to produce outward-propagating ionization gradients, affecting the Lyα absorption opacity near the quasar’s systemic redshift. This “proximity effect” is well-documented in rest-UV quasar spectra but only provides a one-dimensional probe along our line of sight. Here we present deep spectroscopic observations with the James Webb Space Telescope (JWST) of galaxies in the background of a superluminous quasar at zQSO ≈ 6.3, which reveal the quasar’s “light echo” with Lyα tomography in the transverse direction. This transverse proximity effect is detected for the first time toward multiple galaxy sightlines, allowing us to map the extent and geometry of the quasar’s ionization cone. We obtain constraints on the orientation and inclination of the cone, as well as an upper limit on the obscured solid angle fraction of fobsc < 91%. Additionally, we find a timescale of the quasar’s UV radiation of tqso = 10^5.6+0.1-0.3 yr, which is significantly shorter than would be required to build up the central supermassive black hole (SMBH) with conventional growth models, but is consistent with independent measurements of the quasars’ duty cycle. Our inferred obscured fraction disfavors a scenario where short quasar lifetimes can be explained exclusively by geometric obscuration, and instead supports the idea that radiatively inefficient accretion or growth in initially heavily enshrouded cocoons plays a pivotal role in early SMBH growth. Our results pave the way for novel studies of quasars’ ionizing geometries and radiative histories at early cosmic times.","lang":"eng"}],"publication":"The Astrophysical Journal Letters","date_created":"2025-10-05T22:01:35Z","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"file_date_updated":"2025-10-13T09:25:12Z","PlanS_conform":"1","DOAJ_listed":"1","type":"journal_article","date_updated":"2026-02-16T12:44:42Z","month":"09","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"publication_status":"published","doi":"10.3847/2041-8213/ae057a","day":"25","arxiv":1,"language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","status":"public","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"mla":"Eilers, Anna Christina, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2, L40, IOP Publishing, 2025, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>.","chicago":"Eilers, Anna Christina, Minghao Yue, Jorryt J Matthee, Joseph F. Hennawi, Frederick B. Davies, Robert A. Simcoe, Richard Teague, et al. “The Light Echo of a High-Redshift Quasar Mapped with Lyα Tomography.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2025. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>.","short":"A.C. Eilers, M. Yue, J.J. Matthee, J.F. Hennawi, F.B. Davies, R.A. Simcoe, R. Teague, R. Bordoloi, G. Brammer, Y. Kang, D. Kashino, R. Mackenzie, R.P. Naidu, B. Navarrete, The Astrophysical Journal Letters 991 (2025).","ista":"Eilers AC, Yue M, Matthee JJ, Hennawi JF, Davies FB, Simcoe RA, Teague R, Bordoloi R, Brammer G, Kang Y, Kashino D, Mackenzie R, Naidu RP, Navarrete B. 2025. The light echo of a high-redshift quasar mapped with Lyα tomography. The Astrophysical Journal Letters. 991(2), L40.","ieee":"A. C. Eilers <i>et al.</i>, “The light echo of a high-redshift quasar mapped with Lyα tomography,” <i>The Astrophysical Journal Letters</i>, vol. 991, no. 2. IOP Publishing, 2025.","ama":"Eilers AC, Yue M, Matthee JJ, et al. The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. 2025;991(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae057a\">10.3847/2041-8213/ae057a</a>","apa":"Eilers, A. C., Yue, M., Matthee, J. J., Hennawi, J. F., Davies, F. B., Simcoe, R. A., … Navarrete, B. (2025). The light echo of a high-redshift quasar mapped with Lyα tomography. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae057a\">https://doi.org/10.3847/2041-8213/ae057a</a>"},"file":[{"date_updated":"2025-10-13T09:25:12Z","creator":"dernst","file_size":23585591,"file_id":"20461","date_created":"2025-10-13T09:25:12Z","file_name":"2025_AstrophysicalJour_Eilers.pdf","content_type":"application/pdf","checksum":"3cb8099b9a915755164e5675b33f8a03","relation":"main_file","access_level":"open_access","success":1}],"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 #1243 and #4713.\r\n\r\nAll of the data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/w7hm-qb39.\r\nJ.M. is supported by the European Union (ERC, AGENTS, 101076224).","scopus_import":"1","_id":"20425","external_id":{"arxiv":["2509.05417"],"isi":["001581023000001"]},"issue":"2","isi":1,"author":[{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"last_name":"Yue","full_name":"Yue, Minghao","first_name":"Minghao"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Joseph F.","full_name":"Hennawi, Joseph F.","last_name":"Hennawi"},{"full_name":"Davies, Frederick B.","last_name":"Davies","first_name":"Frederick B."},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"last_name":"Teague","full_name":"Teague, Richard","first_name":"Richard"},{"first_name":"Rongmon","full_name":"Bordoloi, Rongmon","last_name":"Bordoloi"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"first_name":"Yi","full_name":"Kang, Yi","last_name":"Kang"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Benjamín","last_name":"Navarrete","full_name":"Navarrete, Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"}],"intvolume":"       991","volume":991,"date_published":"2025-09-25T00:00:00Z","article_processing_charge":"Yes","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publisher":"IOP Publishing","ddc":["520"],"year":"2025","article_number":"L40"},{"has_accepted_license":"1","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"title":"Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","OA_type":"gold","article_type":"original","APC_amount":"5666,27 EUR","OA_place":"publisher","type":"journal_article","date_updated":"2025-09-04T13:15:26Z","file_date_updated":"2024-03-25T09:31:58Z","publication":"The Astrophysical Journal","date_created":"2024-03-25T08:54:47Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"abstract":[{"text":"Characterizing the prevalence and properties of faint active galactic nuclei (AGNs) in the early Universe is key for understanding the formation of supermassive black holes (SMBHs) and determining their role in cosmic reionization. We perform a spectroscopic search for broad Hα emitters at z ≈ 4–6 using deep JWST/NIRCam imaging and wide field slitless spectroscopy from the EIGER and FRESCO surveys. We identify 20 Hα lines at z = 4.2–5.5 that have broad components with line widths from ∼1200–3700 km s−1, contributing ∼30%–90% of the total line flux. We interpret these broad components as being powered by accretion onto SMBHs with implied masses ∼107–8M⊙. In the UV luminosity range MUV,AGN+host = −21 to −18, we measure number densities of ≈10−5 cMpc−3. This is an order of magnitude higher than expected from extrapolating quasar UV luminosity functions (LFs). Yet, such AGN are found in only <1% of star-forming galaxies at z ∼ 5. The number density discrepancy is much lower when compared to the broad Hα LF. The SMBH mass function agrees with large cosmological simulations. In two objects, we detect complex Hα profiles that we tentatively interpret as caused by absorption signatures from dense gas fueling SMBH growth and outflows. We may be witnessing early AGN feedback that will clear dust-free pathways through which more massive blue quasars are seen. We uncover a strong correlation between reddening and the fraction of total galaxy luminosity arising from faint AGN. This implies that early SMBH growth is highly obscured and that faint AGN are only minor contributors to cosmic reionization.","lang":"eng"}],"quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"publication_status":"published","department":[{"_id":"JoMa"}],"doi":"10.3847/1538-4357/ad2345","day":"07","related_material":{"link":[{"description":"News on ISTA website","relation":"press_release","url":"https://ista.ac.at/en/news/baby-quasars-growing-supermassive-black-holes/"}]},"month":"03","corr_author":"1","acknowledgement":"We thank the anonymous referee for constructive comments that helped improve the manuscript. 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. 1243 and 1895. The specific observations analyzed can be accessed via doi:10.17909/4xx0-zj76. 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. R.P.N. acknowledges funding from JWST programs GO-1933 and GO-2279. 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. Support for this work for G.I. 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. 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 No. 140.\r\nFacility: JWST - James Webb Space Telescope, HST - Hubble Space Telescope satellite\r\nSoftware:​​​​​​​ Python, matplotlib (Hunter 2007), numpy (Harris et al. 2020), scipy (Virtanen et al. 2020), Astropy (Astropy Collaboration et al. 2013, 2018), Imfit (Erwin 2015).","scopus_import":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"file":[{"date_updated":"2024-03-25T09:31:58Z","file_size":6047536,"creator":"dernst","file_id":"15184","date_created":"2024-03-25T09:31:58Z","file_name":"2024_AstrophysicalJourn_Matthee.pdf","content_type":"application/pdf","relation":"main_file","checksum":"dc7af4694f9f94a551417ab49fa43edf","success":1,"access_level":"open_access"}],"citation":{"short":"J.J. Matthee, R.P. Naidu, G. Brammer, J. Chisholm, A.-C. Eilers, A. Goulding, J. Greene, D. Kashino, I. Labbe, S.J. Lilly, R. Mackenzie, P.A. Oesch, A. Weibel, S. Wuyts, M. Xiao, R. Bordoloi, R. Bouwens, P. van Dokkum, G. Illingworth, I. Kramarenko, M.V. Maseda, C. Mason, R.A. Meyer, E.J. Nelson, N.A. Reddy, I. Shivaei, R.A. Simcoe, M. Yue, The Astrophysical Journal 963 (2024).","mla":"Matthee, Jorryt J., et al. “Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z ∼ 5 Revealed by the EIGER and FRESCO JWST Surveys.” <i>The Astrophysical Journal</i>, vol. 963, no. 2, 129, American Astronomical Society, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad2345\">10.3847/1538-4357/ad2345</a>.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriel Brammer, John Chisholm, Anna-Christina Eilers, Andy Goulding, Jenny Greene, et al. “Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z ∼ 5 Revealed by the EIGER and FRESCO JWST Surveys.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad2345\">https://doi.org/10.3847/1538-4357/ad2345</a>.","ista":"Matthee JJ, Naidu RP, Brammer G, Chisholm J, Eilers A-C, Goulding A, Greene J, Kashino D, Labbe I, Lilly SJ, Mackenzie R, Oesch PA, Weibel A, Wuyts S, Xiao M, Bordoloi R, Bouwens R, van Dokkum P, Illingworth G, Kramarenko I, Maseda MV, Mason C, Meyer RA, Nelson EJ, Reddy NA, Shivaei I, Simcoe RA, Yue M. 2024. Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys. The Astrophysical Journal. 963(2), 129.","ieee":"J. J. Matthee <i>et al.</i>, “Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys,” <i>The Astrophysical Journal</i>, vol. 963, no. 2. American Astronomical Society, 2024.","ama":"Matthee JJ, Naidu RP, Brammer G, et al. Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys. <i>The Astrophysical Journal</i>. 2024;963(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad2345\">10.3847/1538-4357/ad2345</a>","apa":"Matthee, J. J., Naidu, R. P., Brammer, G., Chisholm, J., Eilers, A.-C., Goulding, A., … Yue, M. (2024). Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ad2345\">https://doi.org/10.3847/1538-4357/ad2345</a>"},"status":"public","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"first_name":"Anna-Christina","full_name":"Eilers, Anna-Christina","last_name":"Eilers"},{"first_name":"Andy","last_name":"Goulding","full_name":"Goulding, Andy"},{"first_name":"Jenny","last_name":"Greene","full_name":"Greene, Jenny"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"last_name":"Labbe","full_name":"Labbe, Ivo","first_name":"Ivo"},{"first_name":"Simon J.","last_name":"Lilly","full_name":"Lilly, Simon J."},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"first_name":"Stijn","last_name":"Wuyts","full_name":"Wuyts, Stijn"},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"},{"full_name":"Bordoloi, Rongmon","last_name":"Bordoloi","first_name":"Rongmon"},{"first_name":"Rychard","last_name":"Bouwens","full_name":"Bouwens, Rychard"},{"first_name":"Pieter","last_name":"van Dokkum","full_name":"van Dokkum, Pieter"},{"first_name":"Garth","last_name":"Illingworth","full_name":"Illingworth, Garth"},{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","first_name":"Ivan"},{"full_name":"Maseda, Michael V.","last_name":"Maseda","first_name":"Michael V."},{"first_name":"Charlotte","full_name":"Mason, Charlotte","last_name":"Mason"},{"last_name":"Meyer","full_name":"Meyer, Romain A.","first_name":"Romain A."},{"last_name":"Nelson","full_name":"Nelson, Erica J.","first_name":"Erica J."},{"full_name":"Reddy, Naveen A.","last_name":"Reddy","first_name":"Naveen A."},{"full_name":"Shivaei, Irene","last_name":"Shivaei","first_name":"Irene"},{"first_name":"Robert A.","last_name":"Simcoe","full_name":"Simcoe, Robert A."},{"last_name":"Yue","full_name":"Yue, Minghao","first_name":"Minghao"}],"isi":1,"_id":"15180","external_id":{"isi":["001184703600001"]},"issue":"2","volume":963,"intvolume":"       963","article_processing_charge":"Yes","date_published":"2024-03-07T00:00:00Z","year":"2024","article_number":"129","ddc":["550"],"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"publisher":"American Astronomical Society"},{"abstract":[{"text":"Observationally mapping the relation between galaxies and the intergalactic medium (IGM) is of key interest for studies of cosmic reionization. Diffuse hydrogen gas has typically been observed in H I Lyman-α (Lyα) absorption in the spectra of bright background quasars. However, it is important to extend these measurements to background galaxies as quasars become increasingly rare at high redshift and rarely probe closely separated sight lines. Here, we use deep integral field spectroscopy in the MUSE eXtremely Deep Field to demonstrate the measurement of the Lyα transmission at z ≈ 4 in absorption to a background galaxy at z = 4.77. The H I transmission is consistent with independent quasar sight lines at similar redshifts. Exploiting the high number of spectroscopic redshifts of faint galaxies (500 between z = 4.0–4.7 within a radius of 8 arcmin) that are tracers of the density field, we show that Lyα transmission is inversely correlated with galaxy density, i.e. transparent regions in the Lyα forest mark underdense regions at z ≈ 4. Due to large-scale clustering, galaxies are surrounded by excess H I absorption over the cosmic mean out to 4 cMpc/h70. We also find that redshifts from the peak of the Lyα line are typically offset from the systemic redshift by +170 km s−1. This work extends results from z ≈ 2–3 to higher redshifts and demonstrates the power of deep integral field spectroscopy to simultaneously measure the ionization structure of the IGM and the large-scale density field in the early Universe.","lang":"eng"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_created":"2024-03-31T22:01:12Z","publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2024-04-02T08:42:17Z","date_updated":"2025-09-04T13:18:02Z","DOAJ_listed":"1","type":"journal_article","OA_place":"publisher","article_type":"original","OA_type":"gold","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field","has_accepted_license":"1","oa":1,"status":"public","file":[{"date_created":"2024-04-02T08:42:17Z","file_id":"15255","file_name":"2024_MonthlyNRoyalAstronSoc_Matthee.pdf","date_updated":"2024-04-02T08:42:17Z","creator":"dernst","file_size":2626735,"access_level":"open_access","success":1,"content_type":"application/pdf","checksum":"1e65c40a71e565eebdc4c5ff11822ba2","relation":"main_file"}],"citation":{"ama":"Matthee JJ, Golling C, Mackenzie R, et al. Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;529(3):2794-2806. doi:<a href=\"https://doi.org/10.1093/mnras/stae673\">10.1093/mnras/stae673</a>","apa":"Matthee, J. J., Golling, C., Mackenzie, R., Pezzulli, G., Lilly, S., Schaye, J., … Wisotzki, L. (2024). Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae673\">https://doi.org/10.1093/mnras/stae673</a>","ieee":"J. J. Matthee <i>et al.</i>, “Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 529, no. 3. Oxford University Press, pp. 2794–2806, 2024.","ista":"Matthee JJ, Golling C, Mackenzie R, Pezzulli G, Lilly S, Schaye J, Bacon R, Kusakabe H, Urrutia T, Boogaard L, Brinchmann J, Maseda MV, Garel T, Bouché NF, Wisotzki L. 2024. Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. Monthly Notices of the Royal Astronomical Society. 529(3), 2794–2806.","short":"J.J. Matthee, C. Golling, R. Mackenzie, G. Pezzulli, S. Lilly, J. Schaye, R. Bacon, H. Kusakabe, T. Urrutia, L. Boogaard, J. Brinchmann, M.V. Maseda, T. Garel, N.F. Bouché, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 529 (2024) 2794–2806.","mla":"Matthee, Jorryt J., et al. “Large-Scale Excess H I Absorption around z ≈ 4 Galaxies Detected in a Background Galaxy Spectrum in the MUSE EXtremely Deep Field.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 529, no. 3, Oxford University Press, 2024, pp. 2794–806, doi:<a href=\"https://doi.org/10.1093/mnras/stae673\">10.1093/mnras/stae673</a>.","chicago":"Matthee, Jorryt J, Christopher Golling, Ruari Mackenzie, Gabriele Pezzulli, Simon Lilly, Joop Schaye, Roland Bacon, et al. “Large-Scale Excess H I Absorption around z ≈ 4 Galaxies Detected in a Background Galaxy Spectrum in the MUSE EXtremely Deep Field.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae673\">https://doi.org/10.1093/mnras/stae673</a>."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"acknowledgement":"We thank the referee for constructive comments that helped improving the paper. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. 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. GP acknowledges support from the Netherlands Research School for Astronomy (Nederlandse Onderzoekschool Voor Astronomie, NOVA). JB acknowledges financial support from the Fundação para a Ciência e a Tecnologia (FCT) through national funds PTDC/FIS-AST/4862/2020, work contract 2020.03379.CEECIND, and research grants UIDB/04434/2020 and UIDP/04434/2020. TU and LW acknowledge funding by the European Research Council through ERC-AdG SPECMAP-CGM, GA 101020943. TG is supported by the ERC Starting grant 757258 ‘TRIPLE’.","scopus_import":"1","month":"04","corr_author":"1","doi":"10.1093/mnras/stae673","day":"01","publication_status":"published","department":[{"_id":"JoMa"}],"arxiv":1,"quality_controlled":"1","language":[{"iso":"eng"}],"oa_version":"Published Version","intvolume":"       529","volume":529,"issue":"3","_id":"15249","external_id":{"arxiv":["2305.15346"],"isi":["001188770300019"]},"author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"Christopher","last_name":"Golling","full_name":"Golling, Christopher"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"first_name":"Simon","last_name":"Lilly","full_name":"Lilly, Simon"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"first_name":"Leindert","last_name":"Boogaard","full_name":"Boogaard, Leindert"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"first_name":"Nicolas F.","last_name":"Bouché","full_name":"Bouché, Nicolas F."},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"}],"isi":1,"publisher":"Oxford University Press","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"ddc":["520"],"year":"2024","date_published":"2024-04-01T00:00:00Z","article_processing_charge":"Yes","page":"2794-2806"},{"type":"journal_article","DOAJ_listed":"1","date_updated":"2025-09-08T14:29:05Z","file_date_updated":"2024-11-04T08:42:23Z","date_created":"2024-11-03T23:01:45Z","publication":"Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"abstract":[{"lang":"eng","text":"We expect luminous (M 1450 ≲ −26.5) high-redshift quasars to trace the highest-density peaks in the early Universe. Here, we present observations of four z ≳ 6 quasar fields using JWST/NIRCam in the imaging and wide-field slitless spectroscopy mode and report a wide range in the number of detected [O iii]-emitting galaxies in the quasars’ environments, ranging between a density enhancement of δ ≈ 65 within a 2 cMpc radius—one of the largest protoclusters during the Epoch of Reionization discovered to date—to a density contrast consistent with zero, indicating the presence of a UV-luminous quasar in a region comparable to the average density of the Universe. By measuring the two-point cross-correlation function of quasars and their surrounding galaxies, as well as the galaxy autocorrelation function, we infer a correlation length of quasars at 〈z〉 = 6.25 of r 0 QQ = 22.0 − 2.9 + 3.0 cMpc h − 1 , while we obtain a correlation length of the [O iii]-emitting galaxies of r 0 GG = 4.1 ± 0.3 cMpc h − 1 . By comparing the correlation functions to dark-matter-only simulations we estimate the minimum mass of the quasars’ host dark matter halos to be log 10 ( M halo , min / M ⊙ ) = 12.43 − 0.15 + 0.13 (and log 10 ( M halo , min [ OIII ] / M ⊙ ) = 10.56 − 0.03 + 0.05 for the [O iii] emitters), indicating that (a) luminous quasars do not necessarily reside within the most overdense regions in the early Universe, and that (b) the UV-luminous duty cycle of quasar activity at these redshifts is f duty ≪ 1. Such short quasar activity timescales challenge our understanding of early supermassive black hole growth and provide evidence for highly dust-obscured growth phases or episodic, radiatively inefficient accretion rates."}],"has_accepted_license":"1","oa":1,"title":"EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","OA_type":"gold","article_type":"original","OA_place":"publisher","scopus_import":"1","acknowledgement":"The authors would like to thank the anonymous referee for the thoughtful comments, which significantly improved our manuscript, and Jan-Torge Schindler, Jiamu Huang, and Feige Wang for helpful discussions.\r\n\r\nJ.F.H. and E.P. acknowledge support from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement No. 885301). J.M. acknowledges support from the European Union (ERC, AGENTS, 101076224).\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The JWST data presented in this article 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 are associated with program #1243 and can be accessed via doi:10.17909/m5mp-5v90.\r\n\r\nThis work used the DiRAC Memory Intensive service (Cosma8) at the University of Durham, which is part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). Access to DiRAC resources was granted through a Directors Discretionary Time allocation in 2023/24, under the auspices of the UKRI-funded DiRAC Federation Project. The equipment was funded by BEIS capital funding via STFC capital grants ST/K00042X/1, ST/P002293/1, ST/R002371/1, and ST/S002502/1, Durham University and STFC operations grant ST/R000832/1. DiRAC is part of the National e-Infrastructure.\r\n\r\nWe thank the Instituto de Astrofisica de Andalucia (IAA-CSIC), Centro de Supercomputacion de Galicia (CESGA), and Spanish Academic and Research Network (RedIRIS) in Spain for hosting Uchuu DR1, DR2, and DR3 in the Skies & Universes site for cosmological simulations. The Uchuu simulations were carried out on the Aterui II supercomputer at the Center for Computational Astrophysics, CfCA, of the National Astronomical Observatory of Japan, and the K computer at the RIKEN Advanced Institute for Computational Science. The Uchuu Data Releases efforts have made use of the skunIAA_RedIRIS and skun6IAA computer facilities managed by the IAA-CSIC in Spain (MICINN EU-Feder grant EQC2018-004366-P).","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png"},"citation":{"ista":"Eilers AC, Mackenzie R, Pizzati E, Matthee JJ, Hennawi JF, Zhang H, Bordoloi R, Kashino D, Lilly SJ, Naidu RP, Simcoe RA, Yue M, Frenk CS, Helly JC, Schaller M, Schaye J. 2024. EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6. Astrophysical Journal. 974(2), 275.","chicago":"Eilers, Anna Christina, Ruari Mackenzie, Elia Pizzati, Jorryt J Matthee, Joseph F. Hennawi, Haowen Zhang, Rongmon Bordoloi, et al. “EIGER. VI. The Correlation Function, Host Halo Mass, and Duty Cycle of Luminous Quasars at z ≳ 6.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad778b\">https://doi.org/10.3847/1538-4357/ad778b</a>.","short":"A.C. Eilers, R. Mackenzie, E. Pizzati, J.J. Matthee, J.F. Hennawi, H. Zhang, R. Bordoloi, D. Kashino, S.J. Lilly, R.P. Naidu, R.A. Simcoe, M. Yue, C.S. Frenk, J.C. Helly, M. Schaller, J. Schaye, Astrophysical Journal 974 (2024).","mla":"Eilers, Anna Christina, et al. “EIGER. VI. The Correlation Function, Host Halo Mass, and Duty Cycle of Luminous Quasars at z ≳ 6.” <i>Astrophysical Journal</i>, vol. 974, no. 2, 275, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad778b\">10.3847/1538-4357/ad778b</a>.","apa":"Eilers, A. C., Mackenzie, R., Pizzati, E., Matthee, J. J., Hennawi, J. F., Zhang, H., … Schaye, J. (2024). EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad778b\">https://doi.org/10.3847/1538-4357/ad778b</a>","ama":"Eilers AC, Mackenzie R, Pizzati E, et al. EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6. <i>Astrophysical Journal</i>. 2024;974(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad778b\">10.3847/1538-4357/ad778b</a>","ieee":"A. C. Eilers <i>et al.</i>, “EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6,” <i>Astrophysical Journal</i>, vol. 974, no. 2. IOP Publishing, 2024."},"file":[{"date_updated":"2024-11-04T08:42:23Z","file_size":1042470,"creator":"dernst","file_id":"18496","date_created":"2024-11-04T08:42:23Z","file_name":"2024_AstrophysicalJour_Eilers.pdf","content_type":"application/pdf","relation":"main_file","checksum":"1fcac3d11d01d91cf2bb4963b6e10b22","success":1,"access_level":"open_access"}],"status":"public","language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","department":[{"_id":"JoMa"}],"publication_status":"published","day":"01","doi":"10.3847/1538-4357/ad778b","month":"10","volume":974,"intvolume":"       974","isi":1,"author":[{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"first_name":"Elia","full_name":"Pizzati, Elia","last_name":"Pizzati"},{"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":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"first_name":"Haowen","last_name":"Zhang","full_name":"Zhang, Haowen"},{"full_name":"Bordoloi, Rongmon","last_name":"Bordoloi","first_name":"Rongmon"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"last_name":"Lilly","full_name":"Lilly, Simon J.","first_name":"Simon J."},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Robert A.","last_name":"Simcoe","full_name":"Simcoe, Robert A."},{"full_name":"Yue, Minghao","last_name":"Yue","first_name":"Minghao"},{"first_name":"Carlos S.","full_name":"Frenk, Carlos S.","last_name":"Frenk"},{"first_name":"John C.","last_name":"Helly","full_name":"Helly, John C."},{"first_name":"Matthieu","last_name":"Schaller","full_name":"Schaller, Matthieu"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"}],"_id":"18494","external_id":{"isi":["001338877100001"]},"issue":"2","year":"2024","article_number":"275","ddc":["520"],"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"publisher":"IOP Publishing","article_processing_charge":"Yes","date_published":"2024-10-01T00:00:00Z"}]