[{"date_created":"2024-06-02T22:00:56Z","issue":"6","publication":"Cell Reports","das_tickbox":"1","acknowledgement":"We would like to thank J. Maiwald for her assistance in animal behavior training, experiments, and brain slice preparation; D. Koch for her assistance in recording drive building and brain slicing; K. Kaefer and J. Wallenschus (IST Austria) for their initial technical support; S. Mikulovich for her comments on an early version of the manuscript; C. Reichert for his comments on SVM analyses; and J. Pakan for English proofreading. This project is funded by the DFG (CRC 779 and CRC 1436).","has_accepted_license":"1","volume":43,"dataavailabilitystatement":"Data published in this manuscript are available upon request.\r\n\r\nAll the original code has been deposited at Zenodo: https://zenodo.org/records/11125633. The DOI is listed in the key resources table.\r\n\r\nAny additional information required to reanalyze the data reported in this paper is available upon request.","oa":1,"article_type":"original","file":[{"date_created":"2024-06-03T07:12:45Z","file_name":"2024_CellReports_Ku.pdf","file_id":"17096","date_updated":"2024-06-03T07:12:45Z","checksum":"9b43f8ca5e5a12ae96e3fb9df06385c1","creator":"dernst","relation":"main_file","access_level":"open_access","success":1,"content_type":"application/pdf","file_size":4371015}],"date_updated":"2026-10-15T08:37:28Z","supplementarymaterial":"yes","type":"journal_article","publisher":"Elsevier","publication_identifier":{"eissn":["2211-1247"]},"isi":1,"year":"2024","citation":{"ama":"Ku SP, Atucha E, Alavi N, et al. Phase locking of hippocampal CA3 neurons to distal CA1 theta oscillations selectively predicts memory performance. <i>Cell Reports</i>. 2024;43(6). doi:<a href=\"https://doi.org/10.1016/j.celrep.2024.114276\">10.1016/j.celrep.2024.114276</a>","chicago":"Ku, Shih Pi, Erika Atucha, Nico Alavi, Halla Mulla-Osman, Rukhshona Kayumova, Motoharu Yoshida, Jozsef L Csicsvari, and Magdalena M. Sauvage. “Phase Locking of Hippocampal CA3 Neurons to Distal CA1 Theta Oscillations Selectively Predicts Memory Performance.” <i>Cell Reports</i>. Elsevier, 2024. <a href=\"https://doi.org/10.1016/j.celrep.2024.114276\">https://doi.org/10.1016/j.celrep.2024.114276</a>.","apa":"Ku, S. P., Atucha, E., Alavi, N., Mulla-Osman, H., Kayumova, R., Yoshida, M., … Sauvage, M. M. (2024). Phase locking of hippocampal CA3 neurons to distal CA1 theta oscillations selectively predicts memory performance. <i>Cell Reports</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.celrep.2024.114276\">https://doi.org/10.1016/j.celrep.2024.114276</a>","ieee":"S. P. Ku <i>et al.</i>, “Phase locking of hippocampal CA3 neurons to distal CA1 theta oscillations selectively predicts memory performance,” <i>Cell Reports</i>, vol. 43, no. 6. Elsevier, 2024.","short":"S.P. Ku, E. Atucha, N. Alavi, H. Mulla-Osman, R. Kayumova, M. Yoshida, J.L. Csicsvari, M.M. Sauvage, Cell Reports 43 (2024).","ista":"Ku SP, Atucha E, Alavi N, Mulla-Osman H, Kayumova R, Yoshida M, Csicsvari JL, Sauvage MM. 2024. Phase locking of hippocampal CA3 neurons to distal CA1 theta oscillations selectively predicts memory performance. Cell Reports. 43(6), 114276.","mla":"Ku, Shih Pi, et al. “Phase Locking of Hippocampal CA3 Neurons to Distal CA1 Theta Oscillations Selectively Predicts Memory Performance.” <i>Cell Reports</i>, vol. 43, no. 6, 114276, Elsevier, 2024, doi:<a href=\"https://doi.org/10.1016/j.celrep.2024.114276\">10.1016/j.celrep.2024.114276</a>."},"month":"06","title":"Phase locking of hippocampal CA3 neurons to distal CA1 theta oscillations selectively predicts memory performance","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-06-25T00:00:00Z","abstract":[{"lang":"eng","text":"How the coordination of neuronal spiking and brain rhythms between hippocampal subregions supports memory function remains elusive. We studied the interregional coordination of CA3 neuronal spiking with CA1 theta oscillations by recording electrophysiological signals along the proximodistal axis of the hippocampus in rats that were performing a high-memory-demand recognition memory task adapted from humans. We found that CA3 population spiking occurs preferentially at the peak of distal CA1 theta oscillations when memory was tested but only when previously encountered stimuli were presented. In addition, decoding analyses revealed that only population cell firing of proximal CA3 together with that of distal CA1 can predict performance at test in the present non-spatial task. Overall, our work demonstrates an important role for the synchronization of CA3 neuronal activity with CA1 theta oscillations during memory testing."}],"researchdata_availability":"upon request","language":[{"iso":"eng"}],"day":"25","file_date_updated":"2024-06-03T07:12:45Z","department":[{"_id":"JoCs"}],"publication_status":"published","external_id":{"isi":["001252792600001"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"114276","scopus_import":"1","article_processing_charge":"Yes (in subscription journal)","oa_version":"Published Version","intvolume":"        43","doi":"10.1016/j.celrep.2024.114276","_id":"17089","author":[{"last_name":"Ku","first_name":"Shih Pi","full_name":"Ku, Shih Pi"},{"first_name":"Erika","full_name":"Atucha, Erika","last_name":"Atucha"},{"last_name":"Alavi","first_name":"Nico","full_name":"Alavi, Nico"},{"first_name":"Halla","full_name":"Mulla-Osman, Halla","last_name":"Mulla-Osman"},{"first_name":"Rukhshona","full_name":"Kayumova, Rukhshona","last_name":"Kayumova"},{"full_name":"Yoshida, Motoharu","first_name":"Motoharu","last_name":"Yoshida"},{"last_name":"Csicsvari","id":"3FA14672-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-5193-4036","full_name":"Csicsvari, Jozsef L","first_name":"Jozsef L"},{"last_name":"Sauvage","full_name":"Sauvage, Magdalena M.","first_name":"Magdalena M."}],"quality_controlled":"1","status":"public","fulldoi":"https://doi.org/10.1016/j.celrep.2024.114276","ddc":["570"]},{"department":[{"_id":"JoFi"}],"publication_status":"published","day":"30","language":[{"iso":"eng"}],"title":"Remote sensing of a levitated superconductor with a flux-tunable microwave cavity","citation":{"chicago":"Schmidt, Philip, Remi Claessen, Gerard Higgins, Joachim Hofer, Jannek J. Hansen, Peter Asenbaum, Martin Zemlicka, et al. “Remote Sensing of a Levitated Superconductor with a Flux-Tunable Microwave Cavity.” <i>Physical Review Applied</i>. American Physical Society, 2024. <a href=\"https://doi.org/10.1103/PhysRevApplied.22.014078\">https://doi.org/10.1103/PhysRevApplied.22.014078</a>.","ama":"Schmidt P, Claessen R, Higgins G, et al. Remote sensing of a levitated superconductor with a flux-tunable microwave cavity. <i>Physical Review Applied</i>. 2024;22. doi:<a href=\"https://doi.org/10.1103/PhysRevApplied.22.014078\">10.1103/PhysRevApplied.22.014078</a>","short":"P. Schmidt, R. Claessen, G. Higgins, J. Hofer, J.J. Hansen, P. Asenbaum, M. Zemlicka, K. Uhl, R. Kleiner, R. Gross, H. Huebl, M. Trupke, M. Aspelmeyer, Physical Review Applied 22 (2024).","ieee":"P. Schmidt <i>et al.</i>, “Remote sensing of a levitated superconductor with a flux-tunable microwave cavity,” <i>Physical Review Applied</i>, vol. 22. American Physical Society, 2024.","apa":"Schmidt, P., Claessen, R., Higgins, G., Hofer, J., Hansen, J. J., Asenbaum, P., … Aspelmeyer, M. (2024). Remote sensing of a levitated superconductor with a flux-tunable microwave cavity. <i>Physical Review Applied</i>. American Physical Society. <a href=\"https://doi.org/10.1103/PhysRevApplied.22.014078\">https://doi.org/10.1103/PhysRevApplied.22.014078</a>","mla":"Schmidt, Philip, et al. “Remote Sensing of a Levitated Superconductor with a Flux-Tunable Microwave Cavity.” <i>Physical Review Applied</i>, vol. 22, 014078, American Physical Society, 2024, doi:<a href=\"https://doi.org/10.1103/PhysRevApplied.22.014078\">10.1103/PhysRevApplied.22.014078</a>.","ista":"Schmidt P, Claessen R, Higgins G, Hofer J, Hansen JJ, Asenbaum P, Zemlicka M, Uhl K, Kleiner R, Gross R, Huebl H, Trupke M, Aspelmeyer M. 2024. Remote sensing of a levitated superconductor with a flux-tunable microwave cavity. Physical Review Applied. 22, 014078."},"month":"07","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-07-30T00:00:00Z","abstract":[{"text":"We present a cavity-electromechanical system comprising a superconducting quantum interference device which is embedded in a microwave resonator and coupled via a pickup loop to a 6-μ⁢g magnetically levitated superconducting sphere. The motion of the sphere in the magnetic trap induces a frequency shift in the SQUID-cavity system. We use microwave spectroscopy to characterize the system, and we demonstrate that the electromechanical interaction is tunable. The measured displacement sensitivity of 10−7m/√Hz defines a path towards ground-state cooling of levitated particles with Planck-scale masses at millikelvin environment temperatures.","lang":"eng"}],"researchdata_availability":"yes","year":"2024","fulldoi":"https://doi.org/10.1103/PhysRevApplied.22.014078","oa_version":"Preprint","doi":"10.1103/PhysRevApplied.22.014078","intvolume":"        22","_id":"17410","author":[{"last_name":"Schmidt","first_name":"Philip","full_name":"Schmidt, Philip"},{"last_name":"Claessen","full_name":"Claessen, Remi","first_name":"Remi"},{"last_name":"Higgins","full_name":"Higgins, Gerard","first_name":"Gerard"},{"last_name":"Hofer","full_name":"Hofer, Joachim","first_name":"Joachim"},{"last_name":"Hansen","first_name":"Jannek J.","full_name":"Hansen, Jannek J."},{"full_name":"Asenbaum, Peter","first_name":"Peter","last_name":"Asenbaum"},{"full_name":"Zemlicka, Martin","first_name":"Martin","last_name":"Zemlicka","orcid":"0009-0005-0878-3032","id":"2DCF8DE6-F248-11E8-B48F-1D18A9856A87"},{"first_name":"Kevin","full_name":"Uhl, Kevin","last_name":"Uhl"},{"last_name":"Kleiner","first_name":"Reinhold","full_name":"Kleiner, Reinhold"},{"full_name":"Gross, Rudolf","first_name":"Rudolf","last_name":"Gross"},{"last_name":"Huebl","first_name":"Hans","full_name":"Huebl, Hans"},{"first_name":"Michael","full_name":"Trupke, Michael","last_name":"Trupke"},{"last_name":"Aspelmeyer","first_name":"Markus","full_name":"Aspelmeyer, Markus"}],"status":"public","quality_controlled":"1","scopus_import":"1","article_processing_charge":"No","arxiv":1,"external_id":{"isi":["001284571700002"],"arxiv":["2401.08854"]},"article_number":"014078","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2401.08854"}],"oa":1,"das_tickbox":"0","publication":"Physical Review Applied","acknowledgement":"We gratefully acknowledge valuable discussions with Uros Delic, Lorenzo Magrini, and Corentin Gut. This work was supported by the European Union’s Horizon 2020 research and innovation program under Grant No. 863132 (iQLev) and No. 101080143 (SuperMeQ), the European Research Council under Grant No. 951234 (ERC Synergy QXtreme), the Austrian and Bavarian Academy of Sciences (Topical Team SGQ), the Alexander von Humboldt Foundation through a Feodor Lynen Fellowship (P.S.), the Swedish Research Council under Grant No. 2020-00381 (G.H.), and the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) via Germany’s Excellence Strategy EXC-2111-390814868 (H.H., R.G.).","volume":22,"date_created":"2024-08-11T22:01:12Z","isi":1,"publication_identifier":{"eissn":["2331-7019"]},"type":"journal_article","publisher":"American Physical Society","date_updated":"2026-10-15T09:06:26Z","supplementarymaterial":"yes","article_type":"original"},{"oa":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).","has_accepted_license":"1","publication":"The Astrophysical Journal","das_tickbox":"0","volume":963,"issue":"2","date_created":"2024-03-25T08:54:47Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"isi":1,"publisher":"IOP Publishing","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"related_material":{"link":[{"relation":"press_release","description":"News on ISTA website","url":"https://ista.ac.at/en/news/baby-quasars-growing-supermassive-black-holes/"}]},"date_updated":"2026-10-15T09:15:55Z","supplementarymaterial":"yes","article_type":"original","file":[{"file_name":"2024_AstrophysicalJourn_Matthee.pdf","file_id":"15184","date_updated":"2024-03-25T09:31:58Z","date_created":"2024-03-25T09:31:58Z","success":1,"access_level":"open_access","content_type":"application/pdf","file_size":6047536,"checksum":"dc7af4694f9f94a551417ab49fa43edf","relation":"main_file","creator":"dernst"}],"file_date_updated":"2024-03-25T09:31:58Z","department":[{"_id":"JoMa"}],"publication_status":"published","OA_type":"gold","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"day":"07","language":[{"iso":"eng"}],"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).","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. IOP Publishing, 2024.","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>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad2345\">https://doi.org/10.3847/1538-4357/ad2345</a>","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>","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>. IOP Publishing, 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.","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, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad2345\">10.3847/1538-4357/ad2345</a>."},"title":"Little Red Dots: An abundant population of faint active galactic nuclei at z ∼ 5 revealed by the EIGER and FRESCO JWST surveys","month":"03","date_published":"2024-03-07T00:00:00Z","abstract":[{"lang":"eng","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."}],"researchdata_availability":"no","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","fulldoi":"https://doi.org/10.3847/1538-4357/ad2345","ddc":["550"],"APC_amount":"5666,27 EUR","oa_version":"Published Version","corr_author":"1","_id":"15180","author":[{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"full_name":"Chisholm, John","first_name":"John","last_name":"Chisholm"},{"first_name":"Anna-Christina","full_name":"Eilers, Anna-Christina","last_name":"Eilers"},{"last_name":"Goulding","full_name":"Goulding, Andy","first_name":"Andy"},{"first_name":"Jenny","full_name":"Greene, Jenny","last_name":"Greene"},{"full_name":"Kashino, Daichi","first_name":"Daichi","last_name":"Kashino"},{"first_name":"Ivo","full_name":"Labbe, Ivo","last_name":"Labbe"},{"full_name":"Lilly, Simon J.","first_name":"Simon J.","last_name":"Lilly"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"last_name":"Wuyts","first_name":"Stijn","full_name":"Wuyts, Stijn"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"},{"full_name":"Bordoloi, Rongmon","first_name":"Rongmon","last_name":"Bordoloi"},{"last_name":"Bouwens","full_name":"Bouwens, Rychard","first_name":"Rychard"},{"last_name":"van Dokkum","full_name":"van Dokkum, Pieter","first_name":"Pieter"},{"first_name":"Garth","full_name":"Illingworth, Garth","last_name":"Illingworth"},{"full_name":"Kramarenko, Ivan","first_name":"Ivan","last_name":"Kramarenko"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"first_name":"Charlotte","full_name":"Mason, Charlotte","last_name":"Mason"},{"last_name":"Meyer","first_name":"Romain A.","full_name":"Meyer, Romain A."},{"first_name":"Erica J.","full_name":"Nelson, Erica J.","last_name":"Nelson"},{"last_name":"Reddy","full_name":"Reddy, Naveen A.","first_name":"Naveen A."},{"last_name":"Shivaei","first_name":"Irene","full_name":"Shivaei, Irene"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Minghao","full_name":"Yue, Minghao","last_name":"Yue"}],"quality_controlled":"1","status":"public","doi":"10.3847/1538-4357/ad2345","intvolume":"       963","scopus_import":"1","OA_place":"publisher","article_processing_charge":"Yes","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"129","external_id":{"isi":["001184703600001"]}},{"citation":{"ama":"Greene JE, Labbe I, Goulding AD, et al. UNCOVER spectroscopy confirms the surprising ubiquity of active galactic nuclei in red sources at z &#62; 5. <i>Astrophysical Journal</i>. 2024;964. doi:<a href=\"https://doi.org/10.3847/1538-4357/ad1e5f\">10.3847/1538-4357/ad1e5f</a>","chicago":"Greene, Jenny E., Ivo Labbe, Andy D. Goulding, Lukas J. Furtak, Iryna Chemerynska, Vasily Kokorev, Pratika Dayal, et al. “UNCOVER Spectroscopy Confirms the Surprising Ubiquity of Active Galactic Nuclei in Red Sources at z &#62; 5.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad1e5f\">https://doi.org/10.3847/1538-4357/ad1e5f</a>.","apa":"Greene, J. E., Labbe, I., Goulding, A. D., Furtak, L. J., Chemerynska, I., Kokorev, V., … Zitrin, A. (2024). UNCOVER spectroscopy confirms the surprising ubiquity of active galactic nuclei in red sources at z &#62; 5. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad1e5f\">https://doi.org/10.3847/1538-4357/ad1e5f</a>","short":"J.E. Greene, I. Labbe, A.D. Goulding, L.J. Furtak, I. Chemerynska, V. Kokorev, P. Dayal, M. Volonteri, C.C. Williams, B. Wang, D.J. Setton, A.J. Burgasser, R. Bezanson, H. Atek, G. Brammer, S.E. Cutler, R. Feldmann, S. Fujimoto, K. Glazebrook, A. De Graaff, G. Khullar, J. Leja, D. Marchesini, M.V. Maseda, J.J. Matthee, T.B. Miller, R.P. Naidu, T. Nanayakkara, P.A. Oesch, R. Pan, C. Papovich, S.H. Price, P. Van Dokkum, J.R. Weaver, K.E. Whitaker, A. Zitrin, Astrophysical Journal 964 (2024).","ieee":"J. E. Greene <i>et al.</i>, “UNCOVER spectroscopy confirms the surprising ubiquity of active galactic nuclei in red sources at z &#62; 5,” <i>Astrophysical Journal</i>, vol. 964. IOP Publishing, 2024.","ista":"Greene JE, Labbe I, Goulding AD, Furtak LJ, Chemerynska I, Kokorev V, Dayal P, Volonteri M, Williams CC, Wang B, Setton DJ, Burgasser AJ, Bezanson R, Atek H, Brammer G, Cutler SE, Feldmann R, Fujimoto S, Glazebrook K, De Graaff A, Khullar G, Leja J, Marchesini D, Maseda MV, Matthee JJ, Miller TB, Naidu RP, Nanayakkara T, Oesch PA, Pan R, Papovich C, Price SH, Van Dokkum P, Weaver JR, Whitaker KE, Zitrin A. 2024. UNCOVER spectroscopy confirms the surprising ubiquity of active galactic nuclei in red sources at z &#62; 5. Astrophysical Journal. 964, 39.","mla":"Greene, Jenny E., et al. “UNCOVER Spectroscopy Confirms the Surprising Ubiquity of Active Galactic Nuclei in Red Sources at z &#62; 5.” <i>Astrophysical Journal</i>, vol. 964, 39, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad1e5f\">10.3847/1538-4357/ad1e5f</a>."},"month":"03","title":"UNCOVER spectroscopy confirms the surprising ubiquity of active galactic nuclei in red sources at z > 5","researchdata_availability":"no","abstract":[{"text":"The James Webb Space Telescope is revealing a new population of dust-reddened broad-line active galactic nuclei (AGN) at redshifts z ≳ 5. Here we present deep NIRSpec/Prism spectroscopy from the Cycle 1 Treasury program Ultradeep NIRSpec and NIRCam ObserVations before the Epoch of Reionization (UNCOVER) of 15 AGN candidates selected to be compact, with red continua in the rest-frame optical but with blue slopes in the UV. From NIRCam photometry alone, they could have been dominated by dusty star formation or an AGN. Here we show that the majority of the compact red sources in UNCOVER are dust-reddened AGN: 60% show definitive evidence for broad-line Hα with a FWHM > 2000 km s −1, 20% of the current data are inconclusive, and 20% are brown dwarf stars. We propose an updated photometric criterion to select red z > 5 AGN that excludes brown dwarfs and is expected to yield >80% AGN. Remarkably, among all zphot > 5 galaxies with F277W – F444W > 1 in UNCOVER at least 33% are AGN regardless of compactness, climbing to at least 80% AGN for sources with F277W – F444W > 1.6. The confirmed AGN have black hole masses of 107–109M⊙. While their UV luminosities (−16 > MUV > −20 AB mag) are low compared to UV-selected AGN at these epochs, consistent with percent-level scattered AGN light or low levels of unobscured star formation, the inferred bolometric luminosities are typical of 107–109M⊙ black holes radiating at ∼10%–40% the Eddington limit. The number densities are surprisingly high at ∼10−5 Mpc−3 mag−1, 100 times more common than the faintest UV-selected quasars, while accounting for ∼1% of the UV-selected galaxies. While their UV faintness suggests they may not contribute strongly to reionization, their ubiquity poses challenges to models of black hole growth.","lang":"eng"}],"date_published":"2024-03-01T00:00:00Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","department":[{"_id":"JoMa"}],"file_date_updated":"2024-03-25T08:02:43Z","publication_status":"published","day":"01","language":[{"iso":"eng"}],"scopus_import":"1","arxiv":1,"article_processing_charge":"Yes","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"39","external_id":{"isi":["001184746500001"],"arxiv":["2309.05714"]},"fulldoi":"https://doi.org/10.3847/1538-4357/ad1e5f","ddc":["550"],"oa_version":"Published Version","DOAJ_listed":"1","quality_controlled":"1","_id":"15170","author":[{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"first_name":"Ivo","full_name":"Labbe, Ivo","last_name":"Labbe"},{"last_name":"Goulding","first_name":"Andy D.","full_name":"Goulding, Andy D."},{"full_name":"Furtak, Lukas J.","first_name":"Lukas J.","last_name":"Furtak"},{"full_name":"Chemerynska, Iryna","first_name":"Iryna","last_name":"Chemerynska"},{"last_name":"Kokorev","full_name":"Kokorev, Vasily","first_name":"Vasily"},{"full_name":"Dayal, Pratika","first_name":"Pratika","last_name":"Dayal"},{"first_name":"Marta","full_name":"Volonteri, Marta","last_name":"Volonteri"},{"full_name":"Williams, Christina C.","first_name":"Christina C.","last_name":"Williams"},{"first_name":"Bingjie","full_name":"Wang, Bingjie","last_name":"Wang"},{"full_name":"Setton, David J.","first_name":"David J.","last_name":"Setton"},{"full_name":"Burgasser, Adam J.","first_name":"Adam J.","last_name":"Burgasser"},{"full_name":"Bezanson, Rachel","first_name":"Rachel","last_name":"Bezanson"},{"full_name":"Atek, Hakim","first_name":"Hakim","last_name":"Atek"},{"last_name":"Brammer","full_name":"Brammer, Gabriel","first_name":"Gabriel"},{"first_name":"Sam E.","full_name":"Cutler, Sam E.","last_name":"Cutler"},{"first_name":"Robert","full_name":"Feldmann, Robert","last_name":"Feldmann"},{"last_name":"Fujimoto","first_name":"Seiji","full_name":"Fujimoto, Seiji"},{"last_name":"Glazebrook","full_name":"Glazebrook, Karl","first_name":"Karl"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"last_name":"Khullar","first_name":"Gourav","full_name":"Khullar, Gourav"},{"last_name":"Leja","full_name":"Leja, Joel","first_name":"Joel"},{"full_name":"Marchesini, Danilo","first_name":"Danilo","last_name":"Marchesini"},{"first_name":"Michael V.","full_name":"Maseda, Michael V.","last_name":"Maseda"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"Tim B.","full_name":"Miller, Tim B.","last_name":"Miller"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"full_name":"Pan, Richard","first_name":"Richard","last_name":"Pan"},{"last_name":"Papovich","first_name":"Casey","full_name":"Papovich, Casey"},{"full_name":"Price, Sedona H.","first_name":"Sedona H.","last_name":"Price"},{"last_name":"Van Dokkum","first_name":"Pieter","full_name":"Van Dokkum, Pieter"},{"last_name":"Weaver","full_name":"Weaver, John R.","first_name":"John R."},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."},{"last_name":"Zitrin","full_name":"Zitrin, Adi","first_name":"Adi"}],"status":"public","doi":"10.3847/1538-4357/ad1e5f","intvolume":"       964","has_accepted_license":"1","acknowledgement":"J.E.G. and A.D.G acknowledge support from NSF/AAG grant No. 1007094, and J.E.G. also acknowledges support from NSF/AAG grant No. 1007052. A.Z. acknowledges support by grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF), and by the Ministry of Science & Technology of Israel. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant No. 140. 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. P.D. acknowledges support from the NWO grant 016.VIDI.189.162 (\"ODIN\") and from the European Commission's and University of Groningen's CO-FUND Rosalind Franklin program. K.G. and T.N. acknowledge support from Australian Research Council Laureate Fellowship FL180100060. H.A. and I.C. acknowledge support from CNES, focused on the JWST mission, and the Programme National Cosmology and Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, cofunded by CEA and CNES. R.P.N. acknowledges funding from JWST programs GO-1933 and GO-2279. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The research of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. B.W. acknowledges support from JWST-GO-02561.022-A. A.J.B. acknowledges funding support from NASA/ADAP grant 21-ADAP21-0187. Support for this work was provided by The Brinson Foundation through a Brinson Prize Fellowship grant. R.P.N. acknowledges support for this work 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. C.P. thanks Marsha and Ralph Schilling for the generous support of this research.","das_tickbox":"0","publication":"Astrophysical Journal","volume":964,"date_created":"2024-03-24T23:00:59Z","oa":1,"date_updated":"2026-10-15T09:15:28Z","supplementarymaterial":"no","article_type":"original","file":[{"file_id":"15176","file_name":"2024_AstrophysicalJourn_Greene.pdf","date_updated":"2024-03-25T08:02:43Z","date_created":"2024-03-25T08:02:43Z","success":1,"access_level":"open_access","file_size":2700137,"content_type":"application/pdf","checksum":"389a880e176799d5c062ea7cb82d08c9","relation":"main_file","creator":"dernst"}],"isi":1,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publisher":"IOP Publishing","type":"journal_article"},{"file_date_updated":"2024-07-16T06:24:29Z","department":[{"_id":"JoMa"}],"publication_status":"published","language":[{"iso":"eng"}],"day":"01","month":"07","citation":{"chicago":"Wang, Bingjie, Joel Leja, Anna De Graaff, Gabriel B. Brammer, Andrea Weibel, Pieter Van Dokkum, Josephine F.W. Baggen, et al. “RUBIES: Evolved Stellar Populations with Extended Formation Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified with JWST/NIRSpec.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">https://doi.org/10.3847/2041-8213/ad55f7</a>.","ama":"Wang B, Leja J, De Graaff A, et al. RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. <i>Astrophysical Journal Letters</i>. 2024;969(1). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">10.3847/2041-8213/ad55f7</a>","apa":"Wang, B., Leja, J., De Graaff, A., Brammer, G. B., Weibel, A., Van Dokkum, P., … Williams, C. C. (2024). RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">https://doi.org/10.3847/2041-8213/ad55f7</a>","short":"B. Wang, J. Leja, A. De Graaff, G.B. Brammer, A. Weibel, P. Van Dokkum, J.F.W. Baggen, K.A. Suess, J.E. Greene, R. Bezanson, N.J. Cleri, M. Hirschmann, I. Labbé, J.J. Matthee, I. Mcconachie, R.P. Naidu, E. Nelson, P.A. Oesch, D.J. Setton, C.C. Williams, Astrophysical Journal Letters 969 (2024).","ieee":"B. Wang <i>et al.</i>, “RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec,” <i>Astrophysical Journal Letters</i>, vol. 969, no. 1. IOP Publishing, 2024.","ista":"Wang B, Leja J, De Graaff A, Brammer GB, Weibel A, Van Dokkum P, Baggen JFW, Suess KA, Greene JE, Bezanson R, Cleri NJ, Hirschmann M, Labbé I, Matthee JJ, Mcconachie I, Naidu RP, Nelson E, Oesch PA, Setton DJ, Williams CC. 2024. RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec. Astrophysical Journal Letters. 969(1), L13.","mla":"Wang, Bingjie, et al. “RUBIES: Evolved Stellar Populations with Extended Formation Histories at z ∼ 7-8 in Candidate Massive Galaxies Identified with JWST/NIRSpec.” <i>Astrophysical Journal Letters</i>, vol. 969, no. 1, L13, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad55f7\">10.3847/2041-8213/ad55f7</a>."},"title":"RUBIES: Evolved stellar populations with extended formation histories at z ∼ 7-8 in candidate massive galaxies identified with JWST/NIRSpec","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-07-01T00:00:00Z","researchdata_availability":"yes","abstract":[{"text":"The identification of red, apparently massive galaxies at z > 7 in early James Webb Space Telescope (JWST) photometry suggests a strongly accelerated time line compared to standard models of galaxy growth. A major uncertainty in the interpretation is whether the red colors are caused by evolved stellar populations, dust, or other effects such as emission lines or active galactic nuclei (AGNs). Here we show that three of the massive galaxy candidates at z = 6.7–8.4 have prominent Balmer breaks in JWST/NIRSpec spectroscopy from the RUBIES program. The Balmer breaks demonstrate unambiguously that stellar emission dominates at λrest = 0.4 μm and require formation histories extending hundreds of millions of years into the past in galaxies only 600–800 Myr after the big bang. Two of the three galaxies also show broad Balmer lines, with Hβ FWHM > 2500 km s−1, suggesting that dust-reddened AGNs contribute to, or even dominate, the spectral energy distributions of these galaxies at λrest ≳ 0.6 μm. All three galaxies have relatively narrow [O iii] lines, seemingly ruling out a high-mass interpretation if the lines arise in dynamically relaxed, inclined disks. Yet the inferred masses also remain highly uncertain. We model the high-quality spectra using Prospector to decompose the continuum into stellar and AGN components and explore limiting cases in stellar/AGN contribution. This produces a wide range of possible stellar masses, spanning M⋆ ∼ 109−1011M⊙. Nevertheless, all fits suggest a very early and rapid formation, most of which follow with a truncation in star formation. Potential origins and evolutionary tracks for these objects are discussed, from the cores of massive galaxies to low-mass galaxies with overmassive black holes. Intriguingly, we find all of these explanations to be incomplete; deeper and redder data are needed to understand the physics of these systems.","lang":"eng"}],"year":"2024","fulldoi":"https://doi.org/10.3847/2041-8213/ad55f7","ddc":["520"],"DOAJ_listed":"1","oa_version":"Published Version","doi":"10.3847/2041-8213/ad55f7","intvolume":"       969","status":"public","_id":"17234","author":[{"last_name":"Wang","first_name":"Bingjie","full_name":"Wang, Bingjie"},{"last_name":"Leja","full_name":"Leja, Joel","first_name":"Joel"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"full_name":"Brammer, Gabriel B.","first_name":"Gabriel B.","last_name":"Brammer"},{"first_name":"Andrea","full_name":"Weibel, Andrea","last_name":"Weibel"},{"first_name":"Pieter","full_name":"Van Dokkum, Pieter","last_name":"Van Dokkum"},{"full_name":"Baggen, Josephine F.W.","first_name":"Josephine F.W.","last_name":"Baggen"},{"last_name":"Suess","full_name":"Suess, Katherine A.","first_name":"Katherine A."},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"last_name":"Bezanson","first_name":"Rachel","full_name":"Bezanson, Rachel"},{"first_name":"Nikko J.","full_name":"Cleri, Nikko J.","last_name":"Cleri"},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"last_name":"Labbé","first_name":"Ivo","full_name":"Labbé, Ivo"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Mcconachie, Ian","first_name":"Ian","last_name":"Mcconachie"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"first_name":"Erica","full_name":"Nelson, Erica","last_name":"Nelson"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"last_name":"Setton","full_name":"Setton, David J.","first_name":"David J."},{"last_name":"Williams","first_name":"Christina C.","full_name":"Williams, Christina C."}],"quality_controlled":"1","scopus_import":"1","article_processing_charge":"Yes","arxiv":1,"external_id":{"arxiv":["2405.01473"],"isi":["001257903200001"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"L13","oa":1,"publication":"Astrophysical Journal Letters","das_tickbox":"0","acknowledgement":"We thank the anonymous referee for the helpful comments. B.W. and J.L. acknowledge support from JWST-GO04233.009-A. The Cosmic Dawn Center is funded by the Danish National Research Foundation (DNRF) under grant No. 140. This research was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project No. 562 (First Light at Cosmic Dawn: Exploiting the James Webb Space Telescope Revolution). This work is based in part on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. The JWST 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:10.17909/3a4n-9p88. Computations for this research were performed on the Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar supercomputer. This publication made use of the NASA Astrophysical Data System for bibliographic information. \r\nFacilities: HST (ACS, WFC3), JWST (NIRCam, NIRSpec). Software: Astropy (Astropy Collaboration et al. 2013, 2018, 2022), dynesty (Speagle 2020), EAzY (Brammer et al. 2008),\r\nemcee (Foreman-Mackey et al. 2013), Matplotlib (Hunter 2007), msaexp (Brammer 2023b), msafit (de Graaff et al. 2024a), NumPy (Harris et al. 2020), Prospector (Johnson et al. 2021), Python-FSPS (Johnson et al. 2023).","has_accepted_license":"1","volume":969,"date_created":"2024-07-14T22:01:11Z","issue":"1","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"isi":1,"type":"journal_article","publisher":"IOP Publishing","date_updated":"2026-10-15T09:10:55Z","supplementarymaterial":"yes","article_type":"original","file":[{"date_created":"2024-07-16T06:24:29Z","file_id":"17243","file_name":"2024_AstrophysicalJourn_Wang.pdf","date_updated":"2024-07-16T06:24:29Z","checksum":"bb1a6725586df12e745d091b5778bb2b","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_size":3273303,"content_type":"application/pdf"}]},{"isi":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"publisher":"EDP Sciences","type":"journal_article","date_updated":"2026-10-15T09:15:07Z","supplementarymaterial":"yes","article_type":"original","file":[{"checksum":"a6c0df287c75e8929db9f42badeac859","creator":"dernst","relation":"main_file","access_level":"open_access","success":1,"file_size":6225413,"content_type":"application/pdf","date_created":"2024-09-11T07:35:00Z","file_id":"18055","file_name":"2024_AstronomyAstrophysics_TorralbaTorregrosa.pdf","date_updated":"2024-09-11T07:35:00Z"}],"oa":1,"acknowledgement":"The authors acknowledge the financial support from the MICIU with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022) Project (VAL-JPAS), reference ASFAE/2022/025. This work has been funded by project PID2019-109592GBI00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación (MCIN)-Agencia Estatal de Investigación, by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Innovació Universitats, Ciència i Societat Digital de la Generalitat Valenciana. It has also be funded by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Educació, Universitats, i Ocupació de la Generalitat Valenciana. 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. ST acknowledges support by the Royal Society Research Grant G125142. AH acknowledges support by the VILLUM FONDEN under grant 37459. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. We acknowledge funding from JWST program GO-1933. 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. 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 # 1933. The specific observations analyzed can be accessed via https://doi.org/10.17909/s9ht-7n34.","has_accepted_license":"1","publication":"Astronomy & Astrophysics","das_tickbox":"0","volume":689,"date_created":"2024-09-08T22:01:11Z","fulldoi":"https://doi.org/10.1051/0004-6361/202450318","ddc":["520"],"oa_version":"Published Version","quality_controlled":"1","_id":"17889","status":"public","author":[{"first_name":"Alberto","full_name":"Torralba-Torregrosa, Alberto","last_name":"Torralba-Torregrosa"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"last_name":"Hutter","first_name":"Anne","full_name":"Hutter, Anne"},{"last_name":"Arnalte-Mur","full_name":"Arnalte-Mur, Pablo","first_name":"Pablo"},{"last_name":"Gurung-López","first_name":"Siddhartha","full_name":"Gurung-López, Siddhartha"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"last_name":"Oesch","full_name":"Oesch, Pascal","first_name":"Pascal"},{"first_name":"Daichi","full_name":"Kashino, Daichi","last_name":"Kashino"},{"last_name":"Conroy","full_name":"Conroy, Charlie","first_name":"Charlie"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"}],"doi":"10.1051/0004-6361/202450318","intvolume":"       689","scopus_import":"1","arxiv":1,"article_processing_charge":"Yes (in subscription journal)","article_number":"A44","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2404.10040"],"isi":["001303205700016"]},"file_date_updated":"2024-09-11T07:35:00Z","department":[{"_id":"JoMa"}],"publication_status":"published","language":[{"iso":"eng"}],"day":"01","title":"Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment","citation":{"chicago":"Torralba-Torregrosa, Alberto, Jorryt J Matthee, Rohan P. Naidu, Ruari Mackenzie, Gabriele Pezzulli, Anne Hutter, Pablo Arnalte-Mur, et al. “Anatomy of an Ionized Bubble: NIRCam Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman- α Emitter COLA1 and Its Environment.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450318\">https://doi.org/10.1051/0004-6361/202450318</a>.","ama":"Torralba-Torregrosa A, Matthee JJ, Naidu RP, et al. Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. <i>Astronomy &#38; Astrophysics</i>. 2024;689. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450318\">10.1051/0004-6361/202450318</a>","apa":"Torralba-Torregrosa, A., Matthee, J. J., Naidu, R. P., Mackenzie, R., Pezzulli, G., Hutter, A., … Sobral, D. (2024). Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450318\">https://doi.org/10.1051/0004-6361/202450318</a>","ieee":"A. Torralba-Torregrosa <i>et al.</i>, “Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment,” <i>Astronomy &#38; Astrophysics</i>, vol. 689. EDP Sciences, 2024.","short":"A. Torralba-Torregrosa, J.J. Matthee, R.P. Naidu, R. Mackenzie, G. Pezzulli, A. Hutter, P. Arnalte-Mur, S. Gurung-López, S. Tacchella, P. Oesch, D. Kashino, C. Conroy, D. Sobral, Astronomy &#38; Astrophysics 689 (2024).","ista":"Torralba-Torregrosa A, Matthee JJ, Naidu RP, Mackenzie R, Pezzulli G, Hutter A, Arnalte-Mur P, Gurung-López S, Tacchella S, Oesch P, Kashino D, Conroy C, Sobral D. 2024. Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. Astronomy &#38; Astrophysics. 689, A44.","mla":"Torralba-Torregrosa, Alberto, et al. “Anatomy of an Ionized Bubble: NIRCam Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman- α Emitter COLA1 and Its Environment.” <i>Astronomy &#38; Astrophysics</i>, vol. 689, A44, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450318\">10.1051/0004-6361/202450318</a>."},"month":"09","date_published":"2024-09-01T00:00:00Z","researchdata_availability":"no","abstract":[{"text":"The increasingly neutral intergalactic gas at z > 6 impacts the Lyman-α (Lyα) flux observed from galaxies. One luminous galaxy, COLA1, stands out because of its unique double-peaked Lyα line at z = 6.6, unseen in any simulation of reionization. Here, we present JWST/NIRCam wide-field slitless spectroscopy in a 21 arcmin2 field centered on COLA1. We find 141 galaxies spectroscopically selected through the [O III] doublet at 5.35 < z < 6.95, with 40 of these sources showing Hβ. For COLA1, we additionally detect [O III]4363 as well as Hγ. We measure a systemic redshift of z = 6.5917 for COLA1, confirming the classical double-peak nature of the Lyα profile. This implies that it resides in a highly ionized bubble and that it is leaking ionizing photons with a high escape fraction of fesc(LyC) = 20–50%, making it a prime laboratory to study Lyman continuum escape in the Epoch of Reionization. COLA1 shows all the signs of a prolific ionizer with a Lyα escape fraction of 81 ± 5%, Balmer decrement indicating no dust, a steep UV slope (βUV = −3.2 ± 0.4), and a star-formation surface density ≳10× that of typical galaxies at similar redshift. We detect five galaxies in COLA1’s close environment (Δz < 0.02). Exploiting the high spectroscopic completeness inherent to grism surveys, and using mock simulations that fully mimic the selection function, we show that the number of detected companions is very typical for a normal similarly UV-bright (MUV ∼ −21.3) galaxy – that is, the ionized bubble around COLA1 is unlikely to be due to an excessively large over-density. Instead, the measured ionizing properties suggest that COLA1 by itself might be powering the bubble required to explain its double-peaked Lyα profile (Rion ≈ 0.7 pMpc), with only minor contributions from detected neighbors (−19.5 ≲ MUV ≲ −17.5).","lang":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024"},{"OA_type":"green","language":[{"iso":"eng"}],"day":"24","department":[{"_id":"JoMa"}],"publication_status":"published","year":"2024","citation":{"ama":"Heintz KE, Watson D, Brammer G, et al. Strong damped Lyman-a absorption in young star-forming galaxies at redshifts 9 to 11. <i>Science</i>. 2024;384(6698):890-894. doi:<a href=\"https://doi.org/10.1126/science.adj0343\">10.1126/science.adj0343</a>","chicago":"Heintz, Kasper E., Darach Watson, Gabriel Brammer, Simone Vejlgaard, Anne Hutter, Victoria B. Strait, Jorryt J Matthee, et al. “Strong Damped Lyman-a Absorption in Young Star-Forming Galaxies at Redshifts 9 to 11.” <i>Science</i>. AAAS, 2024. <a href=\"https://doi.org/10.1126/science.adj0343\">https://doi.org/10.1126/science.adj0343</a>.","short":"K.E. Heintz, D. Watson, G. Brammer, S. Vejlgaard, A. Hutter, V.B. Strait, J.J. Matthee, P.A. Oesch, P. Jakobsson, N.R. Tanvir, P. Laursen, R.P. Naidu, C.A. Mason, M. Killi, I. Jung, T.Y.Y. Hsiao, U. Abdurro’Uf, D. Coe, P.A. Haro, S.L. Finkelstein, S. Toft, Science 384 (2024) 890–894.","ieee":"K. E. Heintz <i>et al.</i>, “Strong damped Lyman-a absorption in young star-forming galaxies at redshifts 9 to 11,” <i>Science</i>, vol. 384, no. 6698. AAAS, pp. 890–894, 2024.","apa":"Heintz, K. E., Watson, D., Brammer, G., Vejlgaard, S., Hutter, A., Strait, V. B., … Toft, S. (2024). Strong damped Lyman-a absorption in young star-forming galaxies at redshifts 9 to 11. <i>Science</i>. AAAS. <a href=\"https://doi.org/10.1126/science.adj0343\">https://doi.org/10.1126/science.adj0343</a>","mla":"Heintz, Kasper E., et al. “Strong Damped Lyman-a Absorption in Young Star-Forming Galaxies at Redshifts 9 to 11.” <i>Science</i>, vol. 384, no. 6698, AAAS, 2024, pp. 890–94, doi:<a href=\"https://doi.org/10.1126/science.adj0343\">10.1126/science.adj0343</a>.","ista":"Heintz KE, Watson D, Brammer G, Vejlgaard S, Hutter A, Strait VB, Matthee JJ, Oesch PA, Jakobsson P, Tanvir NR, Laursen P, Naidu RP, Mason CA, Killi M, Jung I, Hsiao TYY, Abdurro’Uf U, Coe D, Haro PA, Finkelstein SL, Toft S. 2024. Strong damped Lyman-a absorption in young star-forming galaxies at redshifts 9 to 11. Science. 384(6698), 890–894."},"title":"Strong damped Lyman-a absorption in young star-forming galaxies at redshifts 9 to 11","month":"05","researchdata_availability":"yes","date_published":"2024-05-24T00:00:00Z","abstract":[{"lang":"eng","text":"Primordial neutral atomic gas, mostly composed of hydrogen, is the raw material for star formation in galaxies. However, there are few direct constraints on the amount of neutral atomic hydrogen (H i) in galaxies at early cosmic times. We analyzed James Webb Space Telescope (JWST) near-infrared spectroscopy of distant galaxies, at redshifts ≳8. From a sample of 12 galaxies, we identified three that show strong damped Lyman-α absorption due to H i in their local surroundings. The galaxies are located at spectroscopic redshifts of 8.8, 10.2, and 11.4, corresponding to 400 to 600 million years after the Big Bang. They have H i column densities ≳1022 cm−2, which is an order of magnitude higher than expected for a fully neutral intergalactic medium, and constitute a gas-rich population of young star-forming galaxies."}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Submitted Version","_id":"17090","status":"public","quality_controlled":"1","author":[{"last_name":"Heintz","full_name":"Heintz, Kasper E.","first_name":"Kasper E."},{"last_name":"Watson","full_name":"Watson, Darach","first_name":"Darach"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"full_name":"Vejlgaard, Simone","first_name":"Simone","last_name":"Vejlgaard"},{"full_name":"Hutter, Anne","first_name":"Anne","last_name":"Hutter"},{"full_name":"Strait, Victoria B.","first_name":"Victoria B.","last_name":"Strait"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"full_name":"Jakobsson, Páll","first_name":"Páll","last_name":"Jakobsson"},{"last_name":"Tanvir","full_name":"Tanvir, Nial R.","first_name":"Nial R."},{"full_name":"Laursen, Peter","first_name":"Peter","last_name":"Laursen"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Mason, Charlotte A.","first_name":"Charlotte A.","last_name":"Mason"},{"last_name":"Killi","first_name":"Meghana","full_name":"Killi, Meghana"},{"last_name":"Jung","first_name":"Intae","full_name":"Jung, Intae"},{"last_name":"Hsiao","first_name":"Tiger Yu Yang","full_name":"Hsiao, Tiger Yu Yang"},{"first_name":"Unknown","full_name":"Abdurro’Uf, Unknown","last_name":"Abdurro’Uf"},{"full_name":"Coe, Dan","first_name":"Dan","last_name":"Coe"},{"full_name":"Haro, Pablo Arrabal","first_name":"Pablo Arrabal","last_name":"Haro"},{"full_name":"Finkelstein, Steven L.","first_name":"Steven L.","last_name":"Finkelstein"},{"last_name":"Toft","full_name":"Toft, Sune","first_name":"Sune"}],"doi":"10.1126/science.adj0343","intvolume":"       384","fulldoi":"https://doi.org/10.1126/science.adj0343","external_id":{"pmid":["38781391"],"isi":["001230029500001"]},"scopus_import":"1","OA_place":"repository","article_processing_charge":"No","dataavailabilitystatement":"The JWST spectroscopic data are available at the Mikulski Archive for Space Telescopes (MAST) (https://mast.stsci.edu) under program IDs DD-2750 and GO-1433 for the three selected galaxies; the IDs for the other galaxies we searched are listed in table S1. Our data analysis codes are archived at Zenodo (19, 20). The reduced spectroscopic data are available through the DAWN JWST Archive (DJA): https://s3.amazonaws.com/msaexp-nirspec/extractions/nirspec_graded.html under file names ceers-ddt-v1_prism-clear_2750_28.spec.fits for CEERS-43833, macsj0647-v1_prism-clear_1433_3593.spec.fits for MACS0647-JD, and ceers-ddt-v1_prism-clear_2750_1.spec.fits for CEERS-16943. The photometry is available at https://dawn-cph.github.io/dja/imaging/v7/. Our derived physical parameters are provided in Table 1, and measured line fluxes are provided in table S2.","oa":1,"main_file_link":[{"url":"https://figshare.com/articles/journal_contribution/Strong_damped_Lyman-_absorption_in_young_star-forming_galaxies_at_redshifts_9_to_11/26069122?file=47174584","open_access":"1"}],"issue":"6698","date_created":"2024-06-02T22:00:56Z","acknowledgement":"K.E.H. acknowledges support from Carlsberg Foundation Reintegration Fellowship grant CF21-0103. A.H. acknowledges support from the VILLUM FONDEN under grant 37459. C.A.M. acknowledges support from the VILLUM FONDEN under grant 37459 and the Carlsberg Foundation under grant CF22-1322. N.R.T. was funded through Science and Technology Facilities Council (STFC) consolidated grant ST/W000857/1. R.P.N. acknowledges funding from JWST programs GO-1933 and GO-2279. R.P.N. was supported by 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 under NASA contract NAS5-26555. P.A.O. received funding from the Swiss State Secretariat for Education, Research, and Innovation (SERI) under contract number MB22.00072 and from the Swiss National Science Foundation (SNSF) through project grant 200020_207349.","das_tickbox":"1","publication":"Science","volume":384,"publisher":"AAAS","type":"journal_article","page":"890-894","publication_identifier":{"eissn":["1095-9203"],"issn":["0036-8075"]},"isi":1,"pmid":1,"article_type":"original","date_updated":"2026-10-15T09:10:20Z","supplementarymaterial":"yes"},{"scopus_import":"1","OA_place":"publisher","article_processing_charge":"Yes","arxiv":1,"external_id":{"arxiv":["2305.15346"],"isi":["001188770300019"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"fulldoi":"https://doi.org/10.1093/mnras/stae673","ddc":["520"],"corr_author":"1","oa_version":"Published Version","DOAJ_listed":"1","doi":"10.1093/mnras/stae673","intvolume":"       529","author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Golling, Christopher","first_name":"Christopher","last_name":"Golling"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Lilly","full_name":"Lilly, Simon","first_name":"Simon"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"first_name":"Tanya","full_name":"Urrutia, Tanya","last_name":"Urrutia"},{"full_name":"Boogaard, Leindert","first_name":"Leindert","last_name":"Boogaard"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"first_name":"Thibault","full_name":"Garel, Thibault","last_name":"Garel"},{"full_name":"Bouché, Nicolas F.","first_name":"Nicolas F.","last_name":"Bouché"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"_id":"15249","status":"public","quality_controlled":"1","citation":{"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>.","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>","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.","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.","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>","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>.","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."},"title":"Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field","month":"04","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-04-01T00:00:00Z","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"}],"researchdata_availability":"yes","year":"2024","file_date_updated":"2024-04-02T08:42:17Z","department":[{"_id":"JoMa"}],"publication_status":"published","OA_type":"gold","language":[{"iso":"eng"}],"day":"01","project":[{"grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"date_updated":"2026-10-15T09:19:25Z","supplementarymaterial":"yes","article_type":"original","file":[{"access_level":"open_access","success":1,"content_type":"application/pdf","file_size":2626735,"checksum":"1e65c40a71e565eebdc4c5ff11822ba2","creator":"dernst","relation":"main_file","file_name":"2024_MonthlyNRoyalAstronSoc_Matthee.pdf","file_id":"15255","date_updated":"2024-04-02T08:42:17Z","date_created":"2024-04-02T08:42:17Z"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"isi":1,"type":"journal_article","publisher":"Oxford University Press","page":"2794-2806","publication":"Monthly Notices of the Royal Astronomical Society","das_tickbox":"1","has_accepted_license":"1","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’.","volume":529,"date_created":"2024-03-31T22:01:12Z","issue":"3","dataavailabilitystatement":"The MUSE data in the UDF-MXDF region underlying this work is available through the website https://amused.univ-lyon1.fr/. The catalogue of galaxies in the MUSE Wide region is available through https://musewide.aip.de/. The transmission spectrum measured in this paper will be available online through the publisher.","oa":1},{"year":"2024","month":"10","title":"EIGER. VI. The correlation function, host halo mass, and duty cycle of luminous quasars at z ≳ 6","citation":{"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.","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).","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>","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>.","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>.","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."},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_published":"2024-10-01T00:00:00Z","researchdata_availability":"no","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."}],"OA_type":"gold","day":"01","language":[{"iso":"eng"}],"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"file_date_updated":"2024-11-04T08:42:23Z","department":[{"_id":"JoMa"}],"publication_status":"published","external_id":{"isi":["001338877100001"]},"article_number":"275","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"scopus_import":"1","OA_place":"publisher","article_processing_charge":"Yes","oa_version":"Published Version","DOAJ_listed":"1","doi":"10.3847/1538-4357/ad778b","intvolume":"       974","author":[{"last_name":"Eilers","full_name":"Eilers, Anna Christina","first_name":"Anna Christina"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"first_name":"Elia","full_name":"Pizzati, Elia","last_name":"Pizzati"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Hennawi, Joseph F.","first_name":"Joseph F.","last_name":"Hennawi"},{"first_name":"Haowen","full_name":"Zhang, Haowen","last_name":"Zhang"},{"last_name":"Bordoloi","full_name":"Bordoloi, Rongmon","first_name":"Rongmon"},{"first_name":"Daichi","full_name":"Kashino, Daichi","last_name":"Kashino"},{"full_name":"Lilly, Simon J.","first_name":"Simon J.","last_name":"Lilly"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"last_name":"Yue","full_name":"Yue, Minghao","first_name":"Minghao"},{"full_name":"Frenk, Carlos S.","first_name":"Carlos S.","last_name":"Frenk"},{"last_name":"Helly","first_name":"John C.","full_name":"Helly, John C."},{"last_name":"Schaller","first_name":"Matthieu","full_name":"Schaller, Matthieu"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"}],"_id":"18494","quality_controlled":"1","status":"public","fulldoi":"https://doi.org/10.3847/1538-4357/ad778b","ddc":["520"],"date_created":"2024-11-03T23:01:45Z","issue":"2","publication":"Astrophysical Journal","das_tickbox":"0","has_accepted_license":"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).","volume":974,"oa":1,"article_type":"original","file":[{"date_updated":"2024-11-04T08:42:23Z","file_id":"18496","file_name":"2024_AstrophysicalJour_Eilers.pdf","date_created":"2024-11-04T08:42:23Z","content_type":"application/pdf","file_size":1042470,"access_level":"open_access","success":1,"creator":"dernst","relation":"main_file","checksum":"1fcac3d11d01d91cf2bb4963b6e10b22"}],"date_updated":"2026-10-15T09:27:42Z","supplementarymaterial":"no","type":"journal_article","publisher":"IOP Publishing","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"isi":1},{"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"isi":1,"type":"journal_article","publisher":"EDP Sciences","supplementarymaterial":"no","date_updated":"2026-10-15T09:27:12Z","file":[{"date_created":"2024-10-21T11:45:35Z","file_name":"2024_AstronomyAstrophysics_Matharu.pdf","file_id":"18457","date_updated":"2024-10-21T11:45:35Z","checksum":"10ae78291aa9fa9a9e64724c42d91588","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_size":825494,"content_type":"application/pdf"}],"article_type":"original","oa":1,"volume":690,"das_tickbox":"0","publication":"Astronomy & Astrophysics","acknowledgement":"JM is grateful to the Cosmic Dawn Center for the DAWN Fellowship. JM thanks Adam Muzzin, Viola Gelli and Anne Hutter for useful discussions that led to improvements in the analysis presented in this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The raw data were obtained from the Mikulski Archive for\r\nSpace Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The Cosmic Dawn Center  DAWN) is funded by the Danish National Research Foundation under grant DNRF140.\r\nThis 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. RPN thanks the NASA Hubble Fellowshp Program for the Hubble Fellowship. DM acknowledges funding from JWST-GO-01895.013, provided through a grant from the STScI under NASA contract NAS5-03127.","has_accepted_license":"1","date_created":"2024-10-20T22:02:06Z","ddc":["520"],"fulldoi":"https://doi.org/10.1051/0004-6361/202450522","intvolume":"       690","doi":"10.1051/0004-6361/202450522","author":[{"last_name":"Matharu","full_name":"Matharu, Jasleen","first_name":"Jasleen"},{"first_name":"Erica J.","full_name":"Nelson, Erica J.","last_name":"Nelson"},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"full_name":"Oesch, Pascal A.","first_name":"Pascal A.","last_name":"Oesch"},{"last_name":"Allen","first_name":"Natalie","full_name":"Allen, Natalie"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"first_name":"John","full_name":"Chisholm, John","last_name":"Chisholm"},{"last_name":"Covelo-Paz","first_name":"Alba","full_name":"Covelo-Paz, Alba"},{"last_name":"Fudamoto","first_name":"Yoshinobu","full_name":"Fudamoto, Yoshinobu"},{"last_name":"Giovinazzo","first_name":"Emma","full_name":"Giovinazzo, Emma"},{"last_name":"Herard-Demanche","full_name":"Herard-Demanche, Thomas","first_name":"Thomas"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"full_name":"Kramarenko, Ivan","first_name":"Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"last_name":"Marchesini","first_name":"Danilo","full_name":"Marchesini, Danilo"},{"first_name":"Romain A.","full_name":"Meyer, Romain A.","last_name":"Meyer"},{"first_name":"Gonzalo","full_name":"Prieto-Lyon, Gonzalo","last_name":"Prieto-Lyon"},{"first_name":"Naveen","full_name":"Reddy, Naveen","last_name":"Reddy"},{"first_name":"Marko","full_name":"Shuntov, Marko","last_name":"Shuntov"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"last_name":"Wuyts","full_name":"Wuyts, Stijn","first_name":"Stijn"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"}],"_id":"18447","quality_controlled":"1","status":"public","oa_version":"Published Version","OA_place":"publisher","article_processing_charge":"Yes (in subscription journal)","arxiv":1,"scopus_import":"1","external_id":{"arxiv":["2404.17629"],"isi":["001322237700004"]},"article_number":"A64","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"publication_status":"published","file_date_updated":"2024-10-21T11:45:35Z","department":[{"_id":"JoMa"}],"language":[{"iso":"eng"}],"day":"01","OA_type":"hybrid","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","researchdata_availability":"no","abstract":[{"text":"We present the first results on the spatial distribution of star formation in 454 star-forming galaxies just after the epoch of reionisation (4.8 < z < 6.5) using Hα emission-line maps and F444W imaging that traces the stellar continuum from the JWST FRESCO NIRCam Slitless Spectroscopy Survey. The Hα equivalent width profiles of star-forming galaxies across the main sequence at z ∼ 5.3 with stellar masses 6.8≤ log(M*/M⊙) < 11.1 increase with radius, which provides direct evidence for the inside-out growth of star-forming galaxies just after the epoch of reionisation. GALFIT was used to calculate half-light radii, Reff, and central surface densities within 1 kiloparsec, Σ1kpc of Hα and the continuum. At a fixed stellar mass of Log(M*/M⊙) = 9.5, Σ1kpc, Hα is 1.04 ± 0.05 times higher than Σ1kpc, C, Reff, Hα is 1.18 ± 0.03 times larger than Reff, C and both Reff measurements are smaller than 1 kiloparsec. These measurements suggest the rapid build-up of compact bulges via star formation just after the epoch of reionisation. By comparison to analogous work done at lower redshifts with Hubble Space Telescope WFC3 slitless spectroscopy as part of the 3D-HST (z ∼ 1) and CLEAR (z ∼ 0.5) surveys, we find that Reff(z) evolves at the same pace for Hα and the continuum, but Σ1kpc(z) evolves faster for Hα than the stellar continuum. As a function of the Hubble parameter, Reff, Hα/Reff,C = 1.1h(z) and Σ1 kpc, Hα/Σ1 kpc,C = h(z)1.3. These parametrisations suggest that the inside-out growth of the disk starts to dominate the inside-out growth of the bulge towards lower redshifts. This is supported by the redshift evolution in the EW(Hα) profiles from FRESCO, 3D-HST, and CLEAR at fixed stellar mass and when star-forming progenitors are traced, in which in EW(Hα) rapidly increases with radius within the half-light radius at z ∼ 5.3, but EW(Hα) increases only significantly with radius in the outer disk at z ∼ 0.5.","lang":"eng"}],"date_published":"2024-10-01T00:00:00Z","month":"10","citation":{"ieee":"J. Matharu <i>et al.</i>, “A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","short":"J. Matharu, E.J. Nelson, G. Brammer, P.A. Oesch, N. Allen, I. Shivaei, R.P. Naidu, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, E. Giovinazzo, T. Herard-Demanche, J. Kerutt, I. Kramarenko, D. Marchesini, R.A. Meyer, G. Prieto-Lyon, N. Reddy, M. Shuntov, A. Weibel, S. Wuyts, M. Xiao, Astronomy &#38; Astrophysics 690 (2024).","apa":"Matharu, J., Nelson, E. J., Brammer, G., Oesch, P. A., Allen, N., Shivaei, I., … Xiao, M. (2024). A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>","ama":"Matharu J, Nelson EJ, Brammer G, et al. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>","chicago":"Matharu, Jasleen, Erica J. Nelson, Gabriel Brammer, Pascal A. Oesch, Natalie Allen, Irene Shivaei, Rohan P. Naidu, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>.","mla":"Matharu, Jasleen, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A64, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>.","ista":"Matharu J, Nelson EJ, Brammer G, Oesch PA, Allen N, Shivaei I, Naidu RP, Chisholm J, Covelo-Paz A, Fudamoto Y, Giovinazzo E, Herard-Demanche T, Kerutt J, Kramarenko I, Marchesini D, Meyer RA, Prieto-Lyon G, Reddy N, Shuntov M, Weibel A, Wuyts S, Xiao M. 2024. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. Astronomy &#38; Astrophysics. 690, A64."},"title":"A first look at spatially resolved star formation at 4.8 < z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy","year":"2024"},{"date_created":"2024-04-21T22:00:53Z","volume":684,"das_tickbox":"0","publication":"Astronomy & Astrophysics","has_accepted_license":"1","acknowledgement":"We thank the anonymous referee for the careful reading of the paper and useful suggestions which improved the manuscript. We thank Dr. Leindert Boogaard for sharing data and providing support in the data analysis process. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2021.1.00793.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This project was supported by the European Research Council (ERC) Consolidator Grant 864361 (CosmicWeb) and by Fondazione Cariplo grant no. 2020-0902. M.M. was supported in part by grant HST-GO-17065. This research made use of Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), and Statsmodel (Seabold & Perktold 2010).","oa":1,"file":[{"content_type":"application/pdf","file_size":4410627,"access_level":"open_access","success":1,"creator":"dernst","relation":"main_file","checksum":"ab48775b6946cebfa27ddded5a68fdd2","date_updated":"2024-04-23T06:59:18Z","file_id":"15341","file_name":"2024_AstronomyAstrophysics_Pensabene.pdf","date_created":"2024-04-23T06:59:18Z"}],"article_type":"original","supplementarymaterial":"no","date_updated":"2026-10-15T09:19:58Z","type":"journal_article","publisher":"EDP Sciences","isi":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"year":"2024","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","researchdata_availability":"no","date_published":"2024-04-01T00:00:00Z","abstract":[{"text":"Submillimeter surveys toward overdense regions in the early Universe are essential for uncovering the obscured star formation and the cold gas content of assembling galaxies within massive dark matter halos. In this work, we present deep ALMA mosaic observations covering an area of ∼2′×2′ around MUSE Quasar Nebula 01 (MQN01), one of the largest and brightest Ly-α emitting nebulae discovered thus far; it surrounds a radio-quiet quasar at z ≃ 3.25. Our observations target the 1.2 and the 3 mm dust continuum as well as the carbon monoxide CO(4–3) transition in galaxies in the vicinity of the quasar. We identify a robust sample of 11 CO-line-emitting galaxies (including a closely separated quasar companion) that lie within ±4000 km s−1 of the quasar systemic redshift. A fraction of these objects were missed in previous deep rest-frame optical/UV surveys, which highlights the critical role of (sub)millimeter imaging. We also detect a total of 11 sources revealed in the dust continuum at 1.2 mm; six of them have either high-fidelity spectroscopic redshift information from rest-frame UV metal absorptions or the CO(4–3) line that places them in the same narrow redshift range. A comparison of the CO luminosity function and 1.2 mm number count density with those of the general fields points to a galaxy overdensity of δ > 10. We find evidence of a systematic flattening at the bright end of the CO luminosity function with respect to the trend measured in blank fields. Our findings reveal that galaxies in dense regions at z ∼ 3 are more massive and significantly richer in molecular gas than galaxies in fields, which enables a faster and accelerated assembly. This is the first in a series of studies aimed at characterizing one of the densest regions of the Universe found so far at z > 3.","lang":"eng"}],"month":"04","title":"ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters","citation":{"mla":"Pensabene, A., et al. “ALMA Survey of a Massive Node of the Cosmic Web at z ∼ 3: I. Discovery of a Large Overdensity of CO Emitters.” <i>Astronomy &#38; Astrophysics</i>, vol. 684, A119, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202348659\">10.1051/0004-6361/202348659</a>.","ista":"Pensabene A, Cantalupo S, Cicone C, Decarli R, Galbiati M, Ginolfi M, De Beer S, Fossati M, Fumagalli M, Lazeyras T, Pezzulli G, Travascio A, Wang W, Matthee JJ, Maseda MV. 2024. ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. Astronomy &#38; Astrophysics. 684, A119.","ama":"Pensabene A, Cantalupo S, Cicone C, et al. ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. <i>Astronomy &#38; Astrophysics</i>. 2024;684. doi:<a href=\"https://doi.org/10.1051/0004-6361/202348659\">10.1051/0004-6361/202348659</a>","chicago":"Pensabene, A., S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi, S. De Beer, et al. “ALMA Survey of a Massive Node of the Cosmic Web at z ∼ 3: I. Discovery of a Large Overdensity of CO Emitters.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202348659\">https://doi.org/10.1051/0004-6361/202348659</a>.","ieee":"A. Pensabene <i>et al.</i>, “ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters,” <i>Astronomy &#38; Astrophysics</i>, vol. 684. EDP Sciences, 2024.","apa":"Pensabene, A., Cantalupo, S., Cicone, C., Decarli, R., Galbiati, M., Ginolfi, M., … Maseda, M. V. (2024). ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202348659\">https://doi.org/10.1051/0004-6361/202348659</a>","short":"A. Pensabene, S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi, S. De Beer, M. Fossati, M. Fumagalli, T. Lazeyras, G. Pezzulli, A. Travascio, W. Wang, J.J. Matthee, M.V. Maseda, Astronomy &#38; Astrophysics 684 (2024)."},"day":"01","language":[{"iso":"eng"}],"publication_status":"published","file_date_updated":"2024-04-23T06:59:18Z","department":[{"_id":"JoMa"}],"external_id":{"arxiv":["2401.04765"],"isi":["001199982500009"]},"article_number":"A119","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_processing_charge":"Yes (in subscription journal)","arxiv":1,"scopus_import":"1","doi":"10.1051/0004-6361/202348659","intvolume":"       684","_id":"15336","status":"public","quality_controlled":"1","author":[{"full_name":"Pensabene, A.","first_name":"A.","last_name":"Pensabene"},{"first_name":"S.","full_name":"Cantalupo, S.","last_name":"Cantalupo"},{"last_name":"Cicone","full_name":"Cicone, C.","first_name":"C."},{"last_name":"Decarli","full_name":"Decarli, R.","first_name":"R."},{"last_name":"Galbiati","full_name":"Galbiati, M.","first_name":"M."},{"first_name":"M.","full_name":"Ginolfi, M.","last_name":"Ginolfi"},{"first_name":"S.","full_name":"De Beer, S.","last_name":"De Beer"},{"last_name":"Fossati","first_name":"M.","full_name":"Fossati, M."},{"last_name":"Fumagalli","first_name":"M.","full_name":"Fumagalli, M."},{"full_name":"Lazeyras, T.","first_name":"T.","last_name":"Lazeyras"},{"last_name":"Pezzulli","full_name":"Pezzulli, G.","first_name":"G."},{"first_name":"A.","full_name":"Travascio, A.","last_name":"Travascio"},{"last_name":"Wang","full_name":"Wang, W.","first_name":"W."},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Maseda, M. V.","first_name":"M. V.","last_name":"Maseda"}],"oa_version":"Published Version","ddc":["520"],"fulldoi":"https://doi.org/10.1051/0004-6361/202348659"},{"article_type":"original","file":[{"relation":"main_file","creator":"dernst","checksum":"754b58c1d79adb9670ca76fa8c20ab16","file_size":9960685,"content_type":"application/pdf","success":1,"access_level":"open_access","date_created":"2024-09-17T08:23:59Z","date_updated":"2024-09-17T08:23:59Z","file_id":"18082","file_name":"2024_AstrophysicalJourn_Neufeld.pdf"}],"date_updated":"2026-10-15T09:22:54Z","supplementarymaterial":"yes","publisher":"IOP Publishing","type":"journal_article","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"isi":1,"issue":"2","date_created":"2024-09-15T22:01:40Z","has_accepted_license":"1","acknowledgement":"The authors thank the anonymous referee whose comments and suggestions improved the quality of this work.\r\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program No. 1895.\r\nSupport for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.\r\nThis 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\nR.P.N. acknowledges funding from JWST programs GO-1933 and GO-2279. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555\r\nCloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program.\r\nThis paper made use of several publicly available software packages. We thank the respective authors for sharing their work: IPython (Pérez & Granger 2007), matplotlib (Hunter 2007), seaborn (Waskom et al. 2018), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), jupyter (Kluyver et al. 2016), Astropy (Astropy Collaboration et al. 2013, 2018, 2022), grizli (Brammer 2018; Brammer et al. 2022), Prospector (Leja et al. 2019, 2017; Johnson et al. 2021), FSPS (Conroy et al. 2009a, 2010; Conroy & Gunn 2010a, 2010b; Foreman-Mackey et al. 2014), dynesty (Speagle 2020), EAZY (Brammer et al. 2008), Bagpipes (Carnall et al. 2018), and SExtractor (Bertin & Arnouts 1996).","das_tickbox":"1","publication":"Astrophysical Journal","volume":972,"dataavailabilitystatement":"The JWST data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed on the MAST website. 26","oa":1,"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"156","external_id":{"isi":["001305987600001"]},"scopus_import":"1","article_processing_charge":"Yes","oa_version":"Published Version","DOAJ_listed":"1","author":[{"last_name":"Neufeld","first_name":"Chloe","full_name":"Neufeld, Chloe"},{"last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter","first_name":"Pieter"},{"first_name":"Yasmeen","full_name":"Asali, Yasmeen","last_name":"Asali"},{"last_name":"Covelo-Paz","full_name":"Covelo-Paz, Alba","first_name":"Alba"},{"full_name":"Leja, Joel","first_name":"Joel","last_name":"Leja"},{"full_name":"Lin, Jamie","first_name":"Jamie","last_name":"Lin"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"last_name":"Reddy","first_name":"Naveen A.","full_name":"Reddy, Naveen A."},{"last_name":"Shivaei","full_name":"Shivaei, Irene","first_name":"Irene"},{"last_name":"Whitaker","first_name":"Katherine E.","full_name":"Whitaker, Katherine E."},{"full_name":"Wuyts, Stijn","first_name":"Stijn","last_name":"Wuyts"},{"full_name":"Brammer, Gabriel","first_name":"Gabriel","last_name":"Brammer"},{"full_name":"Marchesini, Danilo","first_name":"Danilo","last_name":"Marchesini"},{"last_name":"Maseda","first_name":"Michael V.","full_name":"Maseda, Michael V."},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"full_name":"Nelson, Erica J.","first_name":"Erica J.","last_name":"Nelson"},{"first_name":"Anna","full_name":"Velichko, Anna","last_name":"Velichko"},{"last_name":"Weibel","full_name":"Weibel, Andrea","first_name":"Andrea"},{"full_name":"Xiao, Mengyuan","first_name":"Mengyuan","last_name":"Xiao"}],"_id":"18069","quality_controlled":"1","status":"public","intvolume":"       972","doi":"10.3847/1538-4357/ad6158","fulldoi":"https://doi.org/10.3847/1538-4357/ad6158","ddc":["520"],"year":"2024","citation":{"ista":"Neufeld C, Van Dokkum P, Asali Y, Covelo-Paz A, Leja J, Lin J, Matthee JJ, Oesch PA, Reddy NA, Shivaei I, Whitaker KE, Wuyts S, Brammer G, Marchesini D, Maseda MV, Naidu RP, Nelson EJ, Velichko A, Weibel A, Xiao M. 2024. FRESCO: The Paschen-α star-forming sequence at cosmic noon. Astrophysical Journal. 972(2), 156.","mla":"Neufeld, Chloe, et al. “FRESCO: The Paschen-α Star-Forming Sequence at Cosmic Noon.” <i>Astrophysical Journal</i>, vol. 972, no. 2, 156, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad6158\">10.3847/1538-4357/ad6158</a>.","chicago":"Neufeld, Chloe, Pieter Van Dokkum, Yasmeen Asali, Alba Covelo-Paz, Joel Leja, Jamie Lin, Jorryt J Matthee, et al. “FRESCO: The Paschen-α Star-Forming Sequence at Cosmic Noon.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad6158\">https://doi.org/10.3847/1538-4357/ad6158</a>.","ama":"Neufeld C, Van Dokkum P, Asali Y, et al. FRESCO: The Paschen-α star-forming sequence at cosmic noon. <i>Astrophysical Journal</i>. 2024;972(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad6158\">10.3847/1538-4357/ad6158</a>","ieee":"C. Neufeld <i>et al.</i>, “FRESCO: The Paschen-α star-forming sequence at cosmic noon,” <i>Astrophysical Journal</i>, vol. 972, no. 2. IOP Publishing, 2024.","apa":"Neufeld, C., Van Dokkum, P., Asali, Y., Covelo-Paz, A., Leja, J., Lin, J., … Xiao, M. (2024). FRESCO: The Paschen-α star-forming sequence at cosmic noon. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad6158\">https://doi.org/10.3847/1538-4357/ad6158</a>","short":"C. Neufeld, P. Van Dokkum, Y. Asali, A. Covelo-Paz, J. Leja, J. Lin, J.J. Matthee, P.A. Oesch, N.A. Reddy, I. Shivaei, K.E. Whitaker, S. Wuyts, G. Brammer, D. Marchesini, M.V. Maseda, R.P. Naidu, E.J. Nelson, A. Velichko, A. Weibel, M. Xiao, Astrophysical Journal 972 (2024)."},"title":"FRESCO: The Paschen-α star-forming sequence at cosmic noon","month":"09","date_published":"2024-09-01T00:00:00Z","researchdata_availability":"yes","abstract":[{"text":"We present results from the JWST First Reionization Epoch Spectroscopically Complete Observations survey on the star-forming sequence (SFS) of galaxies at 1.0 < z < 1.7, around the peak of the cosmic star formation history. Star formation rates (SFRs) are measured from the redshifted, relatively dust-insensitive Paschen-α emission line, and stellar mass measurements include the F444W (4.4 μm; rest-frame H) band. We find SFRs of galaxies with log(M*/M⊙) > 9.5 that are lower than found in many earlier studies by up to 0.6 dex, but in good agreement with recent results obtained with the Prospector fitting framework. The difference (log(SFR(Paα)-SFR(Prospector)) is −0.09 ± 0.04 dex at 1010−11M⊙. We also measure the empirical relation between Paschen-α luminosity and rest-frame H-band magnitude and find that the scatter is only 0.04 dex lower than that of the SFR–M* relation and is much lower than the systematic differences among relations in the literature due to various methods of converting observed measurements to physical properties. We additionally identify examples of sources—that, with standard cutoffs via the UVJ diagram, would be deemed quiescent—with significant (log(sSFR)> −11 yr−1), typically extended, Paschen-α emission. Our results may be indicative of the potential unification of methods used to derive the SFS with careful selection of star-forming galaxies and independent SFR and stellar mass indicators.","lang":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","day":"01","language":[{"iso":"eng"}],"file_date_updated":"2024-09-17T08:23:59Z","department":[{"_id":"JoMa"}],"publication_status":"published"},{"file_date_updated":"2024-05-21T11:13:25Z","department":[{"_id":"JoMa"}],"publication_status":"published","language":[{"iso":"eng"}],"day":"01","citation":{"ama":"Yue M, Eilers AC, Simcoe RA, et al. EIGER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6. <i>Astrophysical Journal</i>. 2024;966(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ad3914\">10.3847/1538-4357/ad3914</a>","chicago":"Yue, Minghao, Anna Christina Eilers, Robert A. Simcoe, Ruari Mackenzie, Jorryt J Matthee, Daichi Kashino, Rongmon Bordoloi, Simon J. Lilly, and Rohan P. Naidu. “EIGER. V. Characterizing the Host Galaxies of Luminous Quasars at z ≳ 6.” <i>Astrophysical Journal</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/1538-4357/ad3914\">https://doi.org/10.3847/1538-4357/ad3914</a>.","ieee":"M. Yue <i>et al.</i>, “EIGER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6,” <i>Astrophysical Journal</i>, vol. 966, no. 2. IOP Publishing, 2024.","short":"M. Yue, A.C. Eilers, R.A. Simcoe, R. Mackenzie, J.J. Matthee, D. Kashino, R. Bordoloi, S.J. Lilly, R.P. Naidu, Astrophysical Journal 966 (2024).","apa":"Yue, M., Eilers, A. C., Simcoe, R. A., Mackenzie, R., Matthee, J. J., Kashino, D., … Naidu, R. P. (2024). EIGER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6. <i>Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ad3914\">https://doi.org/10.3847/1538-4357/ad3914</a>","mla":"Yue, Minghao, et al. “EIGER. V. Characterizing the Host Galaxies of Luminous Quasars at z ≳ 6.” <i>Astrophysical Journal</i>, vol. 966, no. 2, 176, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/1538-4357/ad3914\">10.3847/1538-4357/ad3914</a>.","ista":"Yue M, Eilers AC, Simcoe RA, Mackenzie R, Matthee JJ, Kashino D, Bordoloi R, Lilly SJ, Naidu RP. 2024. EIGER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6. Astrophysical Journal. 966(2), 176."},"month":"05","title":"EIGER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6","date_published":"2024-05-01T00:00:00Z","researchdata_availability":"no","abstract":[{"lang":"eng","text":"We report JWST/NIRCam measurements of quasar host galaxy emissions and supermassive black hole (SMBH) masses for six quasars at 5.9 < z < 7.1 in the Emission-line galaxies and Intergalactic Gas in the Epoch of Reionization (EIGER) project. We obtain deep NIRCam imaging in the F115W, F200W, and F356W bands, as well as F356W grism spectroscopy of the quasars. We use bright unsaturated stars to construct models of the point-spread functions (PSFs) and estimate the errors of these PSFs. We then measure or constrain the fluxes and morphology of the quasar host galaxies by fitting the quasar images as a point source plus an exponential disk. We successfully detect the host galaxies of three quasars, which have host-to-quasar-flux ratios of ∼1%–5%. Spectral energy distribution fitting suggests that these quasar host galaxies have stellar masses of M* ≳ 1010M⊙. For quasars with host galaxy nondetections, we estimate the upper limits of their stellar masses. We use the grism spectra to measure the Hβ line profile and the continuum luminosity, then estimate the SMBH masses for the quasars. Our results indicate that the positive relation between SMBH masses and host galaxy stellar masses already exists at redshift z ≳ 6. The quasars in our sample show a high BH-to-stellar-mass ratio of MBH/M* ∼ 0.15, which is about ∼2 dex higher than local relations. We find that selection effects only contribute partially to the high MBH/M* ratios of high-redshift quasars. This result hints at a possible redshift evolution of the MBH–M* relation."}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","fulldoi":"https://doi.org/10.3847/1538-4357/ad3914","ddc":["520"],"DOAJ_listed":"1","oa_version":"Published Version","quality_controlled":"1","_id":"15405","status":"public","author":[{"last_name":"Yue","first_name":"Minghao","full_name":"Yue, Minghao"},{"first_name":"Anna Christina","full_name":"Eilers, Anna Christina","last_name":"Eilers"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"last_name":"Bordoloi","full_name":"Bordoloi, Rongmon","first_name":"Rongmon"},{"last_name":"Lilly","first_name":"Simon J.","full_name":"Lilly, Simon J."},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."}],"doi":"10.3847/1538-4357/ad3914","intvolume":"       966","scopus_import":"1","article_processing_charge":"Yes","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"176","external_id":{"isi":["001214916200001"]},"oa":1,"has_accepted_license":"1","acknowledgement":"We thank the referee for the valuable comments on this paper. We thank John Silverman, Madeline Marshall, MingYang Zhuang, Weizhe Liu, and Jinyi Yang for inspiring discussions and suggestions. D.K. is grateful for the support from JSPS KAKENHI grant No. JP21K13956. 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\r\nScience 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\r\nassociated with program ID #1243. Facility: JWST (NIRCam) Software: astropy (Astropy Collaboration et al. 2013, 2018), psfMC (Mechtley 2014), webbpsf (Perrin et al. 2014), jwst.","publication":"Astrophysical Journal","das_tickbox":"0","volume":966,"issue":"2","date_created":"2024-05-19T22:01:12Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"isi":1,"publisher":"IOP Publishing","type":"journal_article","date_updated":"2026-10-15T09:20:19Z","supplementarymaterial":"yes","article_type":"original","file":[{"date_created":"2024-05-21T11:13:25Z","file_id":"15410","file_name":"2024_AstrophysicalJourn_Yue.pdf","date_updated":"2024-05-21T11:13:25Z","checksum":"47b428f6209d8a6f9869031d9cb8dae6","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_size":4472346,"content_type":"application/pdf"}]},{"type":"journal_article","publisher":"Oxford University Press","page":"1067-1094","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"isi":1,"article_type":"original","file":[{"date_created":"2024-12-03T12:52:13Z","file_id":"18613","file_name":"2024_MonthlyNRoyalAstronSoc_Meyer.pdf","date_updated":"2024-12-03T12:52:13Z","checksum":"efe0ce3580e01459f3be78eb111b35a9","relation":"main_file","creator":"dernst","success":1,"access_level":"open_access","file_size":29476699,"content_type":"application/pdf"}],"date_updated":"2026-10-15T09:36:43Z","supplementarymaterial":"yes","dataavailabilitystatement":"The results presented in this work are mostly based on public JWST GO1 data (Programme #1895), reduced with the publicly-available code GRIZLI (grizli.readthedocs.io). The reduced imaging data is publicly available at https://s3.amazonaws.com/grizli-v2/JwstMosaics/v7/index.html or through MAST: https://archive.stsci.edu/hlsp/fresco (DOI:10.17909/gdyc-7g80). The [\r\n] emitters catalogues presented in this work, as well as subsequent updates, is publicly available at the following link https://github.com/rameyer/fresco/.","oa":1,"date_created":"2024-11-24T23:01:49Z","issue":"1","das_tickbox":"1","publication":"Monthly Notices of the Royal Astronomical Society","acknowledgement":"The authors thank the anonymous referee for comments and suggestions which improved this paper. RAM thanks R. Kannan for sharing emission line luminosities from THESAN and H. Katz for similar data from an early version of the SPHINX20 data release (we use the final data release in this paper). The authors thank the CONGRESS team for proposing and designing their program with a zero exclusive access period.\r\nRAM, PA, ACP, and AW acknowledge support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. PA, AW, EG, and MX acknowledge support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072. YF acknowledges support by JSPS KAKENHI grant number JP22K21349 and JP23K13149. RPN acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the European Research Commission Grant 101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and from project PID2019-109592GB-I00/AEI/10.13039/501100011033 by the Spanish Ministerio de Ciencia e Innovación - Agencia Estatal de Investigación. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. RJB and MS acknowledges support from NWO grant TOP1.16.057.\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The raw data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","has_accepted_license":"1","volume":535,"DOAJ_listed":"1","oa_version":"Published Version","intvolume":"       535","doi":"10.1093/mnras/stae2353","quality_controlled":"1","_id":"18585","author":[{"full_name":"Meyer, R. A.","first_name":"R. A.","last_name":"Meyer"},{"last_name":"Oesch","first_name":"P. A.","full_name":"Oesch, P. A."},{"last_name":"Giovinazzo","full_name":"Giovinazzo, E.","first_name":"E."},{"last_name":"Weibel","full_name":"Weibel, A.","first_name":"A."},{"first_name":"G.","full_name":"Brammer, G.","last_name":"Brammer"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Naidu","first_name":"R. P.","full_name":"Naidu, R. P."},{"full_name":"Bouwens, R. J.","first_name":"R. J.","last_name":"Bouwens"},{"last_name":"Chisholm","first_name":"J.","full_name":"Chisholm, J."},{"last_name":"Covelo-Paz","full_name":"Covelo-Paz, A.","first_name":"A."},{"full_name":"Fudamoto, Y.","first_name":"Y.","last_name":"Fudamoto"},{"last_name":"Maseda","first_name":"M.","full_name":"Maseda, M."},{"full_name":"Nelson, E.","first_name":"E.","last_name":"Nelson"},{"last_name":"Shivaei","first_name":"I.","full_name":"Shivaei, I."},{"full_name":"Xiao, M.","first_name":"M.","last_name":"Xiao"},{"last_name":"Herard-Demanche","first_name":"T.","full_name":"Herard-Demanche, T."},{"full_name":"Illingworth, G. D.","first_name":"G. D.","last_name":"Illingworth"},{"full_name":"Kerutt, J.","first_name":"J.","last_name":"Kerutt"},{"first_name":"Ivan","full_name":"Kramarenko, Ivan","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","last_name":"Kramarenko"},{"full_name":"Labbe, I.","first_name":"I.","last_name":"Labbe"},{"first_name":"E.","full_name":"Leonova, E.","last_name":"Leonova"},{"full_name":"Magee, D.","first_name":"D.","last_name":"Magee"},{"full_name":"Matharu, J.","first_name":"J.","last_name":"Matharu"},{"last_name":"Prieto Lyon","full_name":"Prieto Lyon, G.","first_name":"G."},{"first_name":"N.","full_name":"Reddy, N.","last_name":"Reddy"},{"full_name":"Schaerer, D.","first_name":"D.","last_name":"Schaerer"},{"last_name":"Shapley","full_name":"Shapley, A.","first_name":"A."},{"full_name":"Stefanon, M.","first_name":"M.","last_name":"Stefanon"},{"first_name":"M. A.","full_name":"Wozniak, M. A.","last_name":"Wozniak"},{"full_name":"Wuyts, S.","first_name":"S.","last_name":"Wuyts"}],"status":"public","fulldoi":"https://doi.org/10.1093/mnras/stae2353","ddc":["520"],"external_id":{"isi":["001348009500001"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"scopus_import":"1","article_processing_charge":"Yes","OA_place":"publisher","OA_type":"gold","language":[{"iso":"eng"}],"day":"01","department":[{"_id":"JoMa"}],"file_date_updated":"2024-12-03T12:52:13Z","publication_status":"published","year":"2024","citation":{"ista":"Meyer RA, Oesch PA, Giovinazzo E, Weibel A, Brammer G, Matthee JJ, Naidu RP, Bouwens RJ, Chisholm J, Covelo-Paz A, Fudamoto Y, Maseda M, Nelson E, Shivaei I, Xiao M, Herard-Demanche T, Illingworth GD, Kerutt J, Kramarenko I, Labbe I, Leonova E, Magee D, Matharu J, Prieto Lyon G, Reddy N, Schaerer D, Shapley A, Stefanon M, Wozniak MA, Wuyts S. 2024. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. Monthly Notices of the Royal Astronomical Society. 535(1), 1067–1094.","mla":"Meyer, R. A., et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1, Oxford University Press, 2024, pp. 1067–94, doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>.","ama":"Meyer RA, Oesch PA, Giovinazzo E, et al. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;535(1):1067-1094. doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>","chicago":"Meyer, R. A., P. A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, Jorryt J Matthee, R. P. Naidu, et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>.","ieee":"R. A. Meyer <i>et al.</i>, “JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1. Oxford University Press, pp. 1067–1094, 2024.","short":"R.A. Meyer, P.A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, J.J. Matthee, R.P. Naidu, R.J. Bouwens, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, M. Maseda, E. Nelson, I. Shivaei, M. Xiao, T. Herard-Demanche, G.D. Illingworth, J. Kerutt, I. Kramarenko, I. Labbe, E. Leonova, D. Magee, J. Matharu, G. Prieto Lyon, N. Reddy, D. Schaerer, A. Shapley, M. Stefanon, M.A. Wozniak, S. Wuyts, Monthly Notices of the Royal Astronomical Society 535 (2024) 1067–1094.","apa":"Meyer, R. A., Oesch, P. A., Giovinazzo, E., Weibel, A., Brammer, G., Matthee, J. J., … Wuyts, S. (2024). JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>"},"month":"11","title":"JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 < z < 9.0 in the GOODS fields","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","abstract":[{"text":"We present the census of Hβ+[OIII] 4960,5008 Åemitters at 6.8<z<9.0 from the JWST FRESCO survey over 124 arcmin2 in the GOODS-North and GOODS-South fields. Our unbiased spectroscopic search results in 137 spectroscopically-confirmed galaxies at 6.8<z<9.0 with observed [OIII] fluxes f[OIII]≳1×10−18 ergs s−1 cm−2. The rest-frame optical line ratios of the median stacked spectrum (median MUV=−19.65+0.59−1.05) indicate negligible dust attenuation, low metallicity (12+log(O/H)=7.2−7.7) and a high ionisation parameter log10U≃−2.5. We find a factor ×1.3 difference in the number density of 6.8<z<9.0 galaxies between GOODS-South and GOODS-North, which is caused by a single overdensity at 7.0<z<7.2 in GOODS-North. The bright end of the UV luminosity function of spectroscopically-confirmed [OIII] emitters is in good agreement with HST dropout-selected samples. Discrepancies between the observed [OIII] LF, [OIII]/UV ratio and [OIII] equivalent widths, and that predicted by theoretical models, suggest burstier star-formation histories and/or more heterogeneous metallicity and ionising conditions in z>7 galaxies. We report a rapid decline of the [OIII] luminosity density at z≳6−7 which cannot be explained by the evolution of the cosmic star-formation rate density. Finally we find that FRESCO detects in only 2h galaxies likely accounting for ∼10−20% of the ionising budget at z=7−8 (assuming an escape fraction of 10%), raising the prospect of directly detecting a significant fraction of the sources of reionisation with JWST.","lang":"eng"}],"researchdata_availability":"yes","date_published":"2024-11-01T00:00:00Z"},{"ddc":["520"],"fulldoi":"https://doi.org/10.1051/0004-6361/202451432","_id":"18493","author":[{"last_name":"Goovaerts","first_name":"I.","full_name":"Goovaerts, I."},{"full_name":"Thai, T. T.","first_name":"T. T.","last_name":"Thai"},{"last_name":"Pello","full_name":"Pello, R.","first_name":"R."},{"first_name":"P.","full_name":"Tuan-Anh, P.","last_name":"Tuan-Anh"},{"first_name":"N.","full_name":"Laporte, N.","last_name":"Laporte"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, T.","first_name":"T."},{"last_name":"Pharo","first_name":"J.","full_name":"Pharo, J."}],"quality_controlled":"1","status":"public","doi":"10.1051/0004-6361/202451432","intvolume":"       690","oa_version":"Published Version","arxiv":1,"OA_place":"publisher","article_processing_charge":"No","scopus_import":"1","article_number":"A302","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"isi":["001339205700015"],"arxiv":["2408.00517"]},"publication_status":"published","department":[{"_id":"JoMa"}],"file_date_updated":"2024-11-04T08:04:44Z","language":[{"iso":"eng"}],"day":"01","OA_type":"diamond","date_published":"2024-10-01T00:00:00Z","researchdata_availability":"no","abstract":[{"text":"Context. The escape of Lyman-α photons at redshifts greater than two is an ongoing subject of study and an important quantity to further understanding of Lyman-α emitters (LAEs), the transmission of Lyman-α photons through the interstellar medium and intergalactic medium, and the impact these LAEs have on cosmic reionisation.\r\n\r\nAims. This study aims to assess the Lyman-α escape fraction, fesc, Lyα, over the redshift range 2.9 < z < 6.7, focusing on Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) selected, gravitationally lensed, intrinsically faint LAEs. These galaxies are of particular interest as the potential drivers of cosmic reionisation.\r\n\r\nMethods. We assessed fesc, Lyα in two ways: through an individual study of 96 LAEs behind the A2744 lensing cluster, with James Webb Space Telescope/Near-Infrared Camera (JWST/NIRCam) and HST data, and through a study of the global evolution of fesc, Lyα using the state-of-the-art luminosity functions for LAEs and the UV-selected ‘parent’ population (dust-corrected). We compared these studies to those in the literature based on brighter samples.\r\n\r\nResults. We find a negligible redshift evolution of fesc, Lyα for our individual galaxies; it is likely that it was washed out by significant intrinsic scatter. We observed a more significant evolution towards higher escape fractions with decreasing UV magnitude and fit this relation. When comparing the two luminosity functions to derive fesc, Lyα in a global sense, we saw agreement with previous literature when integrating the luminosity functions to a bright limit. However, when integrating using a faint limit equivalent to the observational limits of our samples, we observed enhanced values of fesc, Lyα, particularly around z ∼ 6, where fesc, Lyα becomes consistent with 100% escape. This indicates for the faint regimes we sampled that galaxies towards reionisation tend to allow very large fractions of Lyman-α photons to escape. We interpret this as evidence of a lack of any significant dust in these populations; our sample is likely dominated by young, highly star-forming chemically unevolved galaxies. Finally, we assessed the contribution of the LAE population to reionisation using our latest values for fesc, Lyα and the LAE luminosity density. The dependence on the escape fraction of Lyman continuum photons is strong, but for values similar to those observed recently in z ∼ 3 LAEs and high-redshift analogues, LAEs could provide all the ionising emissivity necessary for reionisation.","lang":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Charting the Lyman-α escape fraction in the range 2.9 < z < 6.7 and consequences for the LAE reionisation contribution","citation":{"ama":"Goovaerts I, Thai TT, Pello R, et al. Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451432\">10.1051/0004-6361/202451432</a>","chicago":"Goovaerts, I., T. T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, Jorryt J Matthee, T. Nanayakkara, and J. Pharo. “Charting the Lyman-α Escape Fraction in the Range 2.9 &#60; z &#60; 6.7 and Consequences for the LAE Reionisation Contribution.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202451432\">https://doi.org/10.1051/0004-6361/202451432</a>.","apa":"Goovaerts, I., Thai, T. T., Pello, R., Tuan-Anh, P., Laporte, N., Matthee, J. J., … Pharo, J. (2024). Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451432\">https://doi.org/10.1051/0004-6361/202451432</a>","short":"I. Goovaerts, T.T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, J.J. Matthee, T. Nanayakkara, J. Pharo, Astronomy &#38; Astrophysics 690 (2024).","ieee":"I. Goovaerts <i>et al.</i>, “Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","mla":"Goovaerts, I., et al. “Charting the Lyman-α Escape Fraction in the Range 2.9 &#60; z &#60; 6.7 and Consequences for the LAE Reionisation Contribution.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A302, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451432\">10.1051/0004-6361/202451432</a>.","ista":"Goovaerts I, Thai TT, Pello R, Tuan-Anh P, Laporte N, Matthee JJ, Nanayakkara T, Pharo J. 2024. Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. Astronomy &#38; Astrophysics. 690, A302."},"month":"10","year":"2024","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"isi":1,"publisher":"EDP Sciences","type":"journal_article","supplementarymaterial":"yes","date_updated":"2026-10-15T09:40:49Z","file":[{"creator":"dernst","relation":"main_file","checksum":"4007e2b0fadf93bea61c5bec3fc97e87","content_type":"application/pdf","file_size":2008461,"access_level":"open_access","success":1,"date_created":"2024-11-04T08:04:44Z","date_updated":"2024-11-04T08:04:44Z","file_id":"18495","file_name":"2024_AstronomyAstrophysics_Goovaerts.pdf"}],"article_type":"original","oa":1,"volume":690,"acknowledgement":"This work is done based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345, 092.A-0472, 094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also based on observations obtained with the\r\nNASA/ESA Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. All plots in this paper were created using Matplotlib (Hunter 2007). Part of this work was supported by the French CNRS, the Aix-Marseille University, the French Programme National de Cosmologie et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This work also received support from the French government under the France 2030 investment plan, as part of the Excellence Initiative of Aix-Marseille University - A*MIDEX (AMX-19-IET-008 - IPhU).\r\nFinancial support from the World Laboratory, the Odon Vallet Foundation and VNSC is gratefully acknowledged. Tran Thi Thai was funded by Vingroup JSC and supported by the Master, PhD Scholarship Programme of Vingroup Innovation Foundation (VINIF), Institute of Big Data, code VINIF.2023.TS.108. This research was funded by Vingroup Innovation Foundation under project code VINIF.2023.DA.057.","has_accepted_license":"1","das_tickbox":"0","publication":"Astronomy & Astrophysics","date_created":"2024-11-03T23:01:45Z"},{"year":"2024","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","researchdata_availability":"upon request","abstract":[{"lang":"eng","text":"Recent observations from the EIGER JWST program have measured for the first time the quasar–galaxy cross-correlation function at z ≈ 6. The autocorrelation function of faint z ≈ 6 quasars was also recently estimated. These measurements provide key insights into the properties of quasars and galaxies at high redshift and their relation with the host dark matter haloes. In this work, we interpret these data building upon an empirical quasar population model that has been applied successfully to quasar clustering and demographic measurements at z ≈ 2–4. We use a new, large-volume N-body simulation with more than a trillion particles, FLAMINGO-10k, to model quasars and galaxies simultaneously. We successfully reproduce observations of z ≈ 6 quasars and galaxies (i.e. their clustering properties and luminosity functions), and infer key quantities such as their luminosity–halo mass relation, the mass function of their host haloes, and their duty cycle/occupation fraction. Our key findings\r\nare (i) quasars reside on average in ≈ 1012.5 M haloes (corresponding to ≈ 5σ fluctuations in the initial conditions of the linear density field), but the distribution of host halo masses is quite broad; (ii) the duty cycle of (UV-bright) quasar activity is relatively low (≈ 1 per cent); (iii) galaxies (that are bright in [O III]) live in much smaller haloes (≈ 1010.9 M) and have a larger duty cycle (occupation fraction) of ≈ 13 per cent. Finally, we focus on the inferred properties of quasars and present a homogeneous analysis of their evolution with redshift. The picture that emerges reveals a strong evolution of the host halo mass and duty cycle of quasars at z ≈ 2–6, and calls for new investigations of the role of quasar activity across cosmic time."}],"date_published":"2024-11-01T00:00:00Z","title":"A unified model for the clustering of quasars and galaxies at z ≈ 6","month":"11","citation":{"mla":"Pizzati, Elia, et al. “A Unified Model for the Clustering of Quasars and Galaxies at z ≈ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 4, Oxford University Press, 2024, pp. 3155–75, doi:<a href=\"https://doi.org/10.1093/mnras/stae2307\">10.1093/mnras/stae2307</a>.","ista":"Pizzati E, Hennawi JF, Schaye J, Schaller M, Eilers AC, Wang F, Frenk CS, Elbers W, Helly JC, Mackenzie R, Matthee JJ, Bordoloi R, Kashino D, Naidu RP, Yue M. 2024. A unified model for the clustering of quasars and galaxies at z ≈ 6. Monthly Notices of the Royal Astronomical Society. 534(4), 3155–3175.","ama":"Pizzati E, Hennawi JF, Schaye J, et al. A unified model for the clustering of quasars and galaxies at z ≈ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;534(4):3155-3175. doi:<a href=\"https://doi.org/10.1093/mnras/stae2307\">10.1093/mnras/stae2307</a>","chicago":"Pizzati, Elia, Joseph F. Hennawi, Joop Schaye, Matthieu Schaller, Anna Christina Eilers, Feige Wang, Carlos S. Frenk, et al. “A Unified Model for the Clustering of Quasars and Galaxies at z ≈ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2307\">https://doi.org/10.1093/mnras/stae2307</a>.","apa":"Pizzati, E., Hennawi, J. F., Schaye, J., Schaller, M., Eilers, A. C., Wang, F., … Yue, M. (2024). A unified model for the clustering of quasars and galaxies at z ≈ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2307\">https://doi.org/10.1093/mnras/stae2307</a>","short":"E. Pizzati, J.F. Hennawi, J. Schaye, M. Schaller, A.C. Eilers, F. Wang, C.S. Frenk, W. Elbers, J.C. Helly, R. Mackenzie, J.J. Matthee, R. Bordoloi, D. Kashino, R.P. Naidu, M. Yue, Monthly Notices of the Royal Astronomical Society 534 (2024) 3155–3175.","ieee":"E. Pizzati <i>et al.</i>, “A unified model for the clustering of quasars and galaxies at z ≈ 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 4. Oxford University Press, pp. 3155–3175, 2024."},"day":"01","language":[{"iso":"eng"}],"OA_type":"gold","publication_status":"published","file_date_updated":"2024-11-12T07:17:26Z","department":[{"_id":"JoMa"}],"external_id":{"isi":["001335663900008"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"OA_place":"publisher","article_processing_charge":"Yes","scopus_import":"1","doi":"10.1093/mnras/stae2307","intvolume":"       534","_id":"18523","author":[{"last_name":"Pizzati","full_name":"Pizzati, Elia","first_name":"Elia"},{"last_name":"Hennawi","first_name":"Joseph F.","full_name":"Hennawi, Joseph F."},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Schaller","full_name":"Schaller, Matthieu","first_name":"Matthieu"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"last_name":"Wang","first_name":"Feige","full_name":"Wang, Feige"},{"last_name":"Frenk","first_name":"Carlos S.","full_name":"Frenk, Carlos S."},{"first_name":"Willem","full_name":"Elbers, Willem","last_name":"Elbers"},{"first_name":"John C.","full_name":"Helly, John C.","last_name":"Helly"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Bordoloi, Rongmon","first_name":"Rongmon","last_name":"Bordoloi"},{"last_name":"Kashino","full_name":"Kashino, Daichi","first_name":"Daichi"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"full_name":"Yue, Minghao","first_name":"Minghao","last_name":"Yue"}],"status":"public","quality_controlled":"1","DOAJ_listed":"1","oa_version":"Published Version","ddc":["520"],"fulldoi":"https://doi.org/10.1093/mnras/stae2307","date_created":"2024-11-10T23:01:58Z","issue":"4","volume":534,"das_tickbox":"1","publication":"Monthly Notices of the Royal Astronomical Society","acknowledgement":"We are grateful to Junya Arita and the SHELLQs team for sharing their data on the quasar autocorrelation function and to Jan-Torge Schindler for discussion on the QLF. We acknowledge helpful conversations with the ENIGMA group at UC Santa Barbara and Leiden University. EP is grateful to Rob McGibbon and Victor Forouhar Moreno for help with the simulation outputs, and to Timo Kist, Jiamu Huang, and Vikram Khaire for comments on an early version of the manuscript. JFH and EP acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 885301). This work is partly supported by funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No 860744 (BiD4BESt). FW acknowledges support from NSF grant AST-2308258. This 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 Director’s Discretionary Time allocation in 2023/24, under the auspices of the UKRI-funded\r\nDiRAC 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.","has_accepted_license":"1","oa":1,"dataavailabilitystatement":"The derived data generated in this research will be shared on reasonable requests to the corresponding author.","file":[{"checksum":"9ea6285dd1d04d7a9e7b40a4c9e11edb","creator":"dernst","relation":"main_file","access_level":"open_access","success":1,"file_size":2954312,"content_type":"application/pdf","date_created":"2024-11-12T07:17:26Z","file_id":"18542","file_name":"2024_MonthlyNRoyalAstronSoc_Pizzati.pdf","date_updated":"2024-11-12T07:17:26Z"}],"article_type":"original","supplementarymaterial":"yes","date_updated":"2026-10-15T09:35:12Z","page":"3155-3175","type":"journal_article","publisher":"Oxford University Press","isi":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]}},{"OA_type":"hybrid","language":[{"iso":"eng"}],"day":"01","department":[{"_id":"JoMa"}],"file_date_updated":"2024-11-11T08:54:11Z","publication_status":"published","year":"2024","month":"10","citation":{"short":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, G. Popping, Astronomy &#38; Astrophysics 690 (2024).","apa":"Di Cesare, C., Ginolfi, M., Graziani, L., Schneider, R., Romano, M., &#38; Popping, G. (2024). Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>","ieee":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping, “Carbon envelopes around merging galaxies at z ~ 4.5,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","chicago":"Di Cesare, Claudia, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>.","ama":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>","ista":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. 2024. Carbon envelopes around merging galaxies at z ~ 4.5. Astronomy &#38; Astrophysics. 690, A255.","mla":"Di Cesare, Claudia, et al. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A255, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>."},"title":"Carbon envelopes around merging galaxies at z ~ 4.5","abstract":[{"text":"Context. Galaxies evolve through a dynamic exchange of material with their immediate surrounding environment, the so-called circumgalactic medium (CGM). Understanding the physics of gas flows and the nature of the CGM is fundamental to studying galaxy evolution, especially at 4 ≤ z ≤ 6 (i.e., after the Epoch of Reionization) when galaxies rapidly assembled their masses and reached their chemical maturity. Galactic outflows are predicted to enrich the CGM with metals, although it has also been suggested that gas stripping in systems undergoing a major merger may play a role.\r\n\r\nAims. In this work, we explore the metal enrichment of the medium around merging galaxies at z ∼ 4.5, observed by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE). To do so, we study the nature of the [CII] 158 μm emission in the CGM around these systems, using simulations to help disentangle the mechanisms contributing to the CGM metal pollution.\r\n\r\nMethods. By adopting an updated classification of major merger systems in the ALPINE survey, we selected and analyzed merging galaxies whose components can be spatially and/or spectrally resolved in a robust way. This makes it possible to distinguish between the [CII] emission coming from the single components of the system and that coming from the system as a whole. We also made use of the dustyGadget cosmological simulation to select synthetic analogs of observed galaxies and guide the interpretation of the observational results.\r\n\r\nResults. We find a large diffuse [CII] envelope (≳20 kpc) embedding all the merging systems, with at least 25% of the total [CII] emission coming from the medium between the galaxies. Using predictions from dustyGadget, we suggest that this emission has a multi-fold nature, with dynamical interactions between galaxies playing a major role in stripping the gas and enriching the medium with heavy elements.","lang":"eng"}],"date_published":"2024-10-01T00:00:00Z","researchdata_availability":"no","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","corr_author":"1","author":[{"id":"2d002343-372f-11ef-98ec-a164d20427cb","last_name":"Di Cesare","first_name":"Claudia","full_name":"Di Cesare, Claudia"},{"last_name":"Ginolfi","full_name":"Ginolfi, M.","first_name":"M."},{"first_name":"L.","full_name":"Graziani, L.","last_name":"Graziani"},{"first_name":"R.","full_name":"Schneider, R.","last_name":"Schneider"},{"first_name":"M.","full_name":"Romano, M.","last_name":"Romano"},{"full_name":"Popping, G.","first_name":"G.","last_name":"Popping"}],"_id":"18527","status":"public","quality_controlled":"1","doi":"10.1051/0004-6361/202449164","intvolume":"       690","fulldoi":"https://doi.org/10.1051/0004-6361/202449164","ddc":["520"],"article_number":"A255","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"external_id":{"arxiv":["2401.03020"],"isi":["001332213700013"]},"scopus_import":"1","arxiv":1,"article_processing_charge":"No","OA_place":"publisher","oa":1,"date_created":"2024-11-10T23:02:00Z","has_accepted_license":"1","acknowledgement":"The authors would like to thank the anonymous referee for the useful suggestions which improved this article. This paper is based on data obtained with the ALMA Observatory, under Large Program 2017.1.00428.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. CDC would like to thank the GESO group at the European Southern Observatory (ESO) for the useful discussions while preparing this manuscript. The simulated data underlying this article will be shared on reasonable request to the corresponding author. CDC acknowledged support from Sapienza University of Rome program “Bando per la mobilità individuale all’estero” (DR n.1607 del 14 June 2021) during the visiting period (June-November 2022) at ESO Garching, Germany. LG and RS acknowledge support from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and from the Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:B81I18001170001). MR acknowledges support from the Narodowe Centrum Nauki (UMO-2020/38/E/ST9/00077) and support from the Foundation for Polish Science (FNP) under the program START 063.2023. We have benefited from the publicly available software CASA and CARTA and programming language Python, including the numpy (https://numpy.org), matplotlib (https://matplotlib.org), scipy (https://scipy.org) and astropy (http://www.astropy.org) packages. ","publication":"Astronomy & Astrophysics","das_tickbox":"0","volume":690,"publisher":"EDP Sciences","type":"journal_article","isi":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_type":"original","file":[{"date_created":"2024-11-11T08:54:11Z","date_updated":"2024-11-11T08:54:11Z","file_name":"2024_AstronomyAstrophysics_diCesare.pdf","file_id":"18533","relation":"main_file","creator":"dernst","checksum":"24c65a64047aba156f39b01425269bdb","content_type":"application/pdf","file_size":8033864,"success":1,"access_level":"open_access"}],"date_updated":"2026-10-15T09:35:32Z","supplementarymaterial":"yes"},{"publication_identifier":{"eissn":["1049-5258"]},"type":"conference","publisher":"Neural Information Processing Systems Foundation","supplementarymaterial":"no","date_updated":"2026-10-15T09:39:46Z","main_file_link":[{"open_access":"1","url":"https://doi.org/10.52202/079017-4156"}],"oa":1,"alternative_title":["Advances in Neural Information Processing Systems"],"volume":37,"publication":"38th Annual Conference on Neural Information Processing Systems","das_tickbox":"0","acknowledgement":"We acknowledge support from the National Science Foundation (NSF) and the Simons Foundation for the Collaboration on the Theoretical Foundations of Deep Learning through awards DMS-2031883 and #814639 as well as the TILOS institute (NSF CCF-2112665). This work used the programs (1) XSEDE (Extreme science and engineering discovery environment) which is supported by NSF grant numbers ACI-1548562, and (2) ACCESS (Advanced cyberinfrastructure coordination ecosystem: services & support) which is supported by NSF grants numbers #2138259, #2138286, #2138307, #2137603, and #2138296. Specifically, we used the resources from SDSC Expanse GPU compute nodes, and NCSA Delta system, via allocations TG-CIS220009. Marco Mondelli is supported by the 2019 Lopez-Loreta prize. We also acknowledge useful feedback from anonymous reviewers. ","date_created":"2025-01-27T11:11:40Z","fulldoi":"https://doi.org/10.52202/079017-4156","doi":"10.52202/079017-4156","intvolume":"        37","status":"public","_id":"18890","author":[{"last_name":"Beaglehole","first_name":"Daniel","full_name":"Beaglehole, Daniel"},{"full_name":"Súkeník, Peter","first_name":"Peter","last_name":"Súkeník","id":"d64d6a8d-eb8e-11eb-b029-96fd216dec3c"},{"id":"27EB676C-8706-11E9-9510-7717E6697425","orcid":"0000-0002-3242-7020","last_name":"Mondelli","first_name":"Marco","full_name":"Mondelli, Marco"},{"full_name":"Belkin, Mikhail","first_name":"Mikhail","last_name":"Belkin"}],"quality_controlled":"1","corr_author":"1","oa_version":"Published Version","article_processing_charge":"No","OA_place":"publisher","arxiv":1,"scopus_import":"1","conference":{"name":"NeurIPS: Neural Information Processing Systems","start_date":"2024-12-16","end_date":"2024-12-16","location":"Vancouver, Canada"},"external_id":{"arxiv":["2402.13728"]},"publication_status":"published","department":[{"_id":"GradSch"},{"_id":"MaMo"}],"day":"01","language":[{"iso":"eng"}],"project":[{"_id":"059876FA-7A3F-11EA-A408-12923DDC885E","name":"Prix Lopez-Loretta 2019 - Marco Mondelli"}],"OA_type":"free access","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"Deep Neural Collapse (DNC) refers to the surprisingly rigid structure of the data representations in the final layers of Deep Neural Networks (DNNs). Though the phenomenon has been measured in a variety of settings, its emergence is typically explained via data-agnostic approaches, such as the unconstrained features model. In this work, we introduce a data-dependent setting where DNC forms due to feature learning through the average gradient outer product (AGOP). The AGOP is defined with respect to a learned predictor and is equal to the uncentered covariance matrix of its input-output gradients averaged over the training dataset. The Deep Recursive Feature Machine (Deep RFM) is a method that constructs a neural network by iteratively mapping the data with the AGOP and applying an untrained random feature map. We demonstrate empirically that DNC occurs in Deep RFM across standard settings as a consequence of the projection with the AGOP matrix computed at each layer. Further, we theoretically explain DNC in Deep RFM in an asymptotic setting and as a result of kernel learning. We then provide evidence that this mechanism holds for neural networks more generally. In particular, we show that the right singular vectors and values of the weights can be responsible for the majority of within-class variability collapse for DNNs trained in the feature learning regime. As observed in recent work, this singular structure is highly correlated with that of the AGOP.","lang":"eng"}],"researchdata_availability":"no","date_published":"2024-12-01T00:00:00Z","citation":{"apa":"Beaglehole, D., Súkeník, P., Mondelli, M., &#38; Belkin, M. (2024). Average gradient outer product as a mechanism for deep neural collapse. In <i>38th Annual Conference on Neural Information Processing Systems</i> (Vol. 37). Vancouver, Canada: Neural Information Processing Systems Foundation. <a href=\"https://doi.org/10.52202/079017-4156\">https://doi.org/10.52202/079017-4156</a>","short":"D. Beaglehole, P. Súkeník, M. Mondelli, M. Belkin, in:, 38th Annual Conference on Neural Information Processing Systems, Neural Information Processing Systems Foundation, 2024.","ieee":"D. Beaglehole, P. Súkeník, M. Mondelli, and M. Belkin, “Average gradient outer product as a mechanism for deep neural collapse,” in <i>38th Annual Conference on Neural Information Processing Systems</i>, Vancouver, Canada, 2024, vol. 37.","ama":"Beaglehole D, Súkeník P, Mondelli M, Belkin M. Average gradient outer product as a mechanism for deep neural collapse. In: <i>38th Annual Conference on Neural Information Processing Systems</i>. Vol 37. Neural Information Processing Systems Foundation; 2024. doi:<a href=\"https://doi.org/10.52202/079017-4156\">10.52202/079017-4156</a>","chicago":"Beaglehole, Daniel, Peter Súkeník, Marco Mondelli, and Mikhail Belkin. “Average Gradient Outer Product as a Mechanism for Deep Neural Collapse.” In <i>38th Annual Conference on Neural Information Processing Systems</i>, Vol. 37. Neural Information Processing Systems Foundation, 2024. <a href=\"https://doi.org/10.52202/079017-4156\">https://doi.org/10.52202/079017-4156</a>.","mla":"Beaglehole, Daniel, et al. “Average Gradient Outer Product as a Mechanism for Deep Neural Collapse.” <i>38th Annual Conference on Neural Information Processing Systems</i>, vol. 37, Neural Information Processing Systems Foundation, 2024, doi:<a href=\"https://doi.org/10.52202/079017-4156\">10.52202/079017-4156</a>.","ista":"Beaglehole D, Súkeník P, Mondelli M, Belkin M. 2024. Average gradient outer product as a mechanism for deep neural collapse. 38th Annual Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems, Advances in Neural Information Processing Systems, vol. 37."},"month":"12","title":"Average gradient outer product as a mechanism for deep neural collapse","year":"2024"},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.52202/079017-0560"}],"oa":1,"has_accepted_license":"1","das_tickbox":"0","publication":"38th Annual Conference on Neural Information Processing Systems","alternative_title":["Advances in Neural Information Processing Systems"],"volume":37,"date_created":"2025-01-24T17:58:16Z","publication_identifier":{"eissn":["1049-5258"]},"publisher":"Neural Information Processing Systems Foundation","type":"conference","date_updated":"2026-10-15T09:38:13Z","supplementarymaterial":"no","department":[{"_id":"GradSch"},{"_id":"ChLa"}],"publication_status":"published","OA_type":"free access","language":[{"iso":"eng"}],"day":"01","title":"Banded square root matrix factorization for differentially private model training","citation":{"ieee":"N. Kalinin and C. Lampert, “Banded square root matrix factorization for differentially private model training,” in <i>38th Annual Conference on Neural Information Processing Systems</i>, Vancouver, Canada, 2024, vol. 37.","short":"N. Kalinin, C. Lampert, in:, 38th Annual Conference on Neural Information Processing Systems, Neural Information Processing Systems Foundation, 2024.","apa":"Kalinin, N., &#38; Lampert, C. (2024). Banded square root matrix factorization for differentially private model training. In <i>38th Annual Conference on Neural Information Processing Systems</i> (Vol. 37). Vancouver, Canada: Neural Information Processing Systems Foundation. <a href=\"https://doi.org/10.52202/079017-0560\">https://doi.org/10.52202/079017-0560</a>","chicago":"Kalinin, Nikita, and Christoph Lampert. “Banded Square Root Matrix Factorization for Differentially Private Model Training.” In <i>38th Annual Conference on Neural Information Processing Systems</i>, Vol. 37. Neural Information Processing Systems Foundation, 2024. <a href=\"https://doi.org/10.52202/079017-0560\">https://doi.org/10.52202/079017-0560</a>.","ama":"Kalinin N, Lampert C. Banded square root matrix factorization for differentially private model training. In: <i>38th Annual Conference on Neural Information Processing Systems</i>. Vol 37. Neural Information Processing Systems Foundation; 2024. doi:<a href=\"https://doi.org/10.52202/079017-0560\">10.52202/079017-0560</a>","ista":"Kalinin N, Lampert C. 2024. Banded square root matrix factorization for differentially private model training. 38th Annual Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems, Advances in Neural Information Processing Systems, vol. 37.","mla":"Kalinin, Nikita, and Christoph Lampert. “Banded Square Root Matrix Factorization for Differentially Private Model Training.” <i>38th Annual Conference on Neural Information Processing Systems</i>, vol. 37, Neural Information Processing Systems Foundation, 2024, doi:<a href=\"https://doi.org/10.52202/079017-0560\">10.52202/079017-0560</a>."},"month":"12","researchdata_availability":"no","date_published":"2024-12-01T00:00:00Z","abstract":[{"text":"Current state-of-the-art methods for differentially private model training are based on matrix factorization techniques. However, these methods suffer from high computational overhead because they require numerically solving a demanding optimization problem to determine an approximately optimal factorization prior to the actual model training. In this work, we present a new matrix factorization approach, BSR, which overcomes this computational bottleneck. By exploiting properties of the standard matrix square root, BSR allows to efficiently handle also large-scale problems. For the key scenario of stochastic gradient descent with momentum and weight decay, we even derive analytical expressions for BSR that render the computational overhead negligible. We prove bounds on the approximation quality that hold both in the centralized and in the federated learning setting. Our numerical experiments demonstrate that models trained using BSR perform on par with the best existing methods, while completely avoiding their computational overhead.","lang":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2024","fulldoi":"https://doi.org/10.52202/079017-0560","ddc":["000"],"oa_version":"Published Version","corr_author":"1","_id":"18875","quality_controlled":"1","status":"public","author":[{"last_name":"Kalinin","id":"4b14526e-14d2-11ed-ba64-c14c9553d137","full_name":"Kalinin, Nikita","first_name":"Nikita"},{"last_name":"Lampert","id":"40C20FD2-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-8622-7887","full_name":"Lampert, Christoph","first_name":"Christoph"}],"intvolume":"        37","doi":"10.52202/079017-0560","scopus_import":"1","arxiv":1,"article_processing_charge":"No","OA_place":"publisher","external_id":{"arxiv":["2405.13763"]},"conference":{"name":"NeurIPS: Neural Information Processing Systems","start_date":"2024-12-16","end_date":"2024-12-16","location":"Vancouver, Canada"}},{"oa_version":"Published Version","DOAJ_listed":"1","intvolume":"       976","doi":"10.3847/2041-8213/ad7b17","status":"public","_id":"18760","author":[{"first_name":"Erica","full_name":"Nelson, Erica","last_name":"Nelson"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"last_name":"Giménez-Arteaga","first_name":"Clara","full_name":"Giménez-Arteaga, Clara"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Übler","first_name":"Hannah","full_name":"Übler, Hannah"},{"full_name":"Matharu, Jasleen","first_name":"Jasleen","last_name":"Matharu"},{"last_name":"Shapley","full_name":"Shapley, Alice E.","first_name":"Alice E."},{"last_name":"Whitaker","first_name":"Katherine E.","full_name":"Whitaker, Katherine E."},{"last_name":"Wisnioski","full_name":"Wisnioski, Emily","first_name":"Emily"},{"last_name":"Förster Schreiber","full_name":"Förster Schreiber, Natascha M.","first_name":"Natascha M."},{"last_name":"Smit","full_name":"Smit, Renske","first_name":"Renske"},{"last_name":"Van Dokkum","full_name":"Van Dokkum, Pieter","first_name":"Pieter"},{"last_name":"Chisholm","first_name":"John","full_name":"Chisholm, John"},{"last_name":"Endsley","full_name":"Endsley, Ryan","first_name":"Ryan"},{"last_name":"Hartley","full_name":"Hartley, Abigail I.","first_name":"Abigail I."},{"last_name":"Gibson","full_name":"Gibson, Justus","first_name":"Justus"},{"last_name":"Giovinazzo","first_name":"Emma","full_name":"Giovinazzo, Emma"},{"last_name":"Illingworth","first_name":"Garth","full_name":"Illingworth, Garth"},{"last_name":"Labbe","full_name":"Labbe, Ivo","first_name":"Ivo"},{"last_name":"Maseda","full_name":"Maseda, Michael V.","first_name":"Michael V."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Covelo Paz","full_name":"Covelo Paz, Alba","first_name":"Alba"},{"full_name":"Price, Sedona H.","first_name":"Sedona H.","last_name":"Price"},{"first_name":"Naveen A.","full_name":"Reddy, Naveen A.","last_name":"Reddy"},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"first_name":"Andrea","full_name":"Weibel, Andrea","last_name":"Weibel"},{"last_name":"Wuyts","full_name":"Wuyts, Stijn","first_name":"Stijn"},{"last_name":"Xiao","full_name":"Xiao, Mengyuan","first_name":"Mengyuan"},{"last_name":"Alberts","full_name":"Alberts, Stacey","first_name":"Stacey"},{"last_name":"Baker","full_name":"Baker, William M.","first_name":"William M."},{"first_name":"Andrew J.","full_name":"Bunker, Andrew J.","last_name":"Bunker"},{"first_name":"Alex J.","full_name":"Cameron, Alex J.","last_name":"Cameron"},{"last_name":"Charlot","full_name":"Charlot, Stephane","first_name":"Stephane"},{"last_name":"Eisenstein","full_name":"Eisenstein, Daniel J.","first_name":"Daniel J."},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"last_name":"Ji","full_name":"Ji, Zhiyuan","first_name":"Zhiyuan"},{"last_name":"Johnson","first_name":"Benjamin D.","full_name":"Johnson, Benjamin D."},{"first_name":"Gareth C.","full_name":"Jones, Gareth C.","last_name":"Jones"},{"full_name":"Maiolino, Roberto","first_name":"Roberto","last_name":"Maiolino"},{"full_name":"Robertson, Brant","first_name":"Brant","last_name":"Robertson"},{"last_name":"Sandles","first_name":"Lester","full_name":"Sandles, Lester"},{"full_name":"Suess, Katherine A.","first_name":"Katherine A.","last_name":"Suess"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"},{"last_name":"Witstok","full_name":"Witstok, Joris","first_name":"Joris"}],"quality_controlled":"1","fulldoi":"https://doi.org/10.3847/2041-8213/ad7b17","ddc":["520"],"external_id":{"arxiv":["2310.06887"],"isi":["001364636000001"]},"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"L27","scopus_import":"1","article_processing_charge":"Yes","OA_place":"publisher","arxiv":1,"OA_type":"gold","language":[{"iso":"eng"}],"day":"01","file_date_updated":"2025-01-08T08:18:39Z","department":[{"_id":"JoMa"}],"publication_status":"published","year":"2024","citation":{"ama":"Nelson E, Brammer G, Giménez-Arteaga C, et al. Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. <i>Astrophysical Journal Letters</i>. 2024;976(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">10.3847/2041-8213/ad7b17</a>","chicago":"Nelson, Erica, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, et al. “Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4.” <i>Astrophysical Journal Letters</i>. IOP Publishing, 2024. <a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">https://doi.org/10.3847/2041-8213/ad7b17</a>.","short":"E. Nelson, G. Brammer, C. Giménez-Arteaga, P.A. Oesch, R.P. Naidu, H. Übler, J. Matharu, A.E. Shapley, K.E. Whitaker, E. Wisnioski, N.M. Förster Schreiber, R. Smit, P. Van Dokkum, J. Chisholm, R. Endsley, A.I. Hartley, J. Gibson, E. Giovinazzo, G. Illingworth, I. Labbe, M.V. Maseda, J.J. Matthee, A. Covelo Paz, S.H. Price, N.A. Reddy, I. Shivaei, A. Weibel, S. Wuyts, M. Xiao, S. Alberts, W.M. Baker, A.J. Bunker, A.J. Cameron, S. Charlot, D.J. Eisenstein, A. De Graaff, Z. Ji, B.D. Johnson, G.C. Jones, R. Maiolino, B. Robertson, L. Sandles, K.A. Suess, S. Tacchella, C.C. Williams, J. Witstok, Astrophysical Journal Letters 976 (2024).","apa":"Nelson, E., Brammer, G., Giménez-Arteaga, C., Oesch, P. A., Naidu, R. P., Übler, H., … Witstok, J. (2024). Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. <i>Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">https://doi.org/10.3847/2041-8213/ad7b17</a>","ieee":"E. Nelson <i>et al.</i>, “Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4,” <i>Astrophysical Journal Letters</i>, vol. 976, no. 2. IOP Publishing, 2024.","ista":"Nelson E, Brammer G, Giménez-Arteaga C, Oesch PA, Naidu RP, Übler H, Matharu J, Shapley AE, Whitaker KE, Wisnioski E, Förster Schreiber NM, Smit R, Van Dokkum P, Chisholm J, Endsley R, Hartley AI, Gibson J, Giovinazzo E, Illingworth G, Labbe I, Maseda MV, Matthee JJ, Covelo Paz A, Price SH, Reddy NA, Shivaei I, Weibel A, Wuyts S, Xiao M, Alberts S, Baker WM, Bunker AJ, Cameron AJ, Charlot S, Eisenstein DJ, De Graaff A, Ji Z, Johnson BD, Jones GC, Maiolino R, Robertson B, Sandles L, Suess KA, Tacchella S, Williams CC, Witstok J. 2024. Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4. Astrophysical Journal Letters. 976(2), L27.","mla":"Nelson, Erica, et al. “Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4.” <i>Astrophysical Journal Letters</i>, vol. 976, no. 2, L27, IOP Publishing, 2024, doi:<a href=\"https://doi.org/10.3847/2041-8213/ad7b17\">10.3847/2041-8213/ad7b17</a>."},"title":"Ionized gas kinematics with FRESCO: An extended, massive, rapidly rotating galaxy at z = 5.4","month":"12","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","researchdata_availability":"no","abstract":[{"lang":"eng","text":"With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at z > 5 has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at z > 5. We find a significant velocity gradient, which, if interpreted as rotation, yields Vrot = 305 ± 70 km s−1, and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of re = 2.25 kpc, the high rotation velocity in this galaxy is not due to a compact size, as may be expected in the early Universe, but rather to a high total mass, (math formula). This is a factor of roughly 10× higher than the stellar mass within re. We also observe that the radial Hα equivalent width profile and the specific star formation rate map from resolved stellar population modeling are centrally depressed by a factor of ∼1.5 from the center to re. Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside out. While large, rapidly rotating disks are common to z ∼ 2, the existence of one after only 1 Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the Universe."}],"date_published":"2024-12-01T00:00:00Z","type":"journal_article","publisher":"IOP Publishing","isi":1,"publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"article_type":"letter_note","file":[{"date_created":"2025-01-08T08:18:39Z","date_updated":"2025-01-08T08:18:39Z","file_name":"2024_AstrophysicalJour_Nelson.pdf","file_id":"18771","relation":"main_file","creator":"dernst","checksum":"5c7320196586b4340e55f215d8737185","file_size":1822989,"content_type":"application/pdf","success":1,"access_level":"open_access"}],"date_updated":"2026-10-15T09:41:31Z","supplementarymaterial":"no","oa":1,"date_created":"2025-01-05T23:01:58Z","issue":"2","publication":"Astrophysical Journal Letters","das_tickbox":"0","has_accepted_license":"1","acknowledgement":"We thank the reviewer and editorial staff for their excellent feedback and effort—the manuscript is much stronger as a result. Support for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. H.Ü. gratefully acknowledges support by the Isaac Newton Trust and by the Kavli Foundation through a Newton-Kavli Junior Fellowship. 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.S. acknowledges an STFC Ernest Rutherford Fellowship (ST/S004831/1). R.P.N. acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. M.V.M. acknowledges support from the National Science Foundation via AAG grant 2205519 and the Wisconsin Alumni Research Foundation via grant MSN251397. R.M. also acknowledges funding from a research professorship from the Royal Society. A.J.B., A.J.C., and G.C.J. acknowledge funding from the \"FirstGalaxies\" Advanced Grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 789056). I.L. acknowledges support by the Australian Research Council through Future Fellowship FT220100798. D.J.E. is supported as a Simons Investigator and by a JWST/NIRCam contract to the University of Arizona, NAS5-02015. R.M., J.W., L.S., and W.B. acknowledge support by the Science and Technology Facilities Council (STFC), the ERC through advanced grant 695671 \"QUENCH,\" and the UKRI Frontier Research grant RISEandFALL. B.E.R. acknowledges support from the NIRCam Science Team contract to the University of Arizona, NAS5-02015. The research of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The HST and JWST image mosaics of the FRESCO fields are released at MAST as a High Level Science Product (P. Oesch & D. Magee 2023).","volume":976}]