[{"citation":{"ieee":"T. Kist <i>et al.</i>, “First constraints on the local ionization topology in front of two quasars at z ∼ 7.5,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 3. Oxford University Press, 2026.","short":"T. Kist, J.F. Hennawi, F.B. Davies, E. Bañados, S.E.I. Bosman, Z. Cai, A.C. Eilers, X. Fan, Z. Haiman, H.D. Jun, Y. Liu, J. Yang, F. Wang, Monthly Notices of the Royal Astronomical Society 545 (2026).","mla":"Kist, Timo, et al. “First Constraints on the Local Ionization Topology in Front of Two Quasars at z ∼ 7.5.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 3, staf2219, Oxford University Press, 2026, doi:<a href=\"https://doi.org/10.1093/mnras/staf2219\">10.1093/mnras/staf2219</a>.","chicago":"Kist, Timo, Joseph F. Hennawi, Frederick B. Davies, Eduardo Bañados, Sarah E.I. Bosman, Zheng Cai, Anna Christina Eilers, et al. “First Constraints on the Local Ionization Topology in Front of Two Quasars at z ∼ 7.5.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2026. <a href=\"https://doi.org/10.1093/mnras/staf2219\">https://doi.org/10.1093/mnras/staf2219</a>.","ista":"Kist T, Hennawi JF, Davies FB, Bañados E, Bosman SEI, Cai Z, Eilers AC, Fan X, Haiman Z, Jun HD, Liu Y, Yang J, Wang F. 2026. First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. Monthly Notices of the Royal Astronomical Society. 545(3), staf2219.","ama":"Kist T, Hennawi JF, Davies FB, et al. First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. <i>Monthly Notices of the Royal Astronomical Society</i>. 2026;545(3). doi:<a href=\"https://doi.org/10.1093/mnras/staf2219\">10.1093/mnras/staf2219</a>","apa":"Kist, T., Hennawi, J. F., Davies, F. B., Bañados, E., Bosman, S. E. I., Cai, Z., … Wang, F. (2026). First constraints on the local ionization topology in front of two quasars at z ∼ 7.5. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf2219\">https://doi.org/10.1093/mnras/staf2219</a>"},"PlanS_conform":"1","article_processing_charge":"Yes","title":"First constraints on the local ionization topology in front of two quasars at z ∼ 7.5","month":"01","_id":"20974","doi":"10.1093/mnras/staf2219","OA_place":"publisher","OA_type":"gold","article_type":"original","arxiv":1,"ddc":["520"],"type":"journal_article","day":"01","publisher":"Oxford University Press","issue":"3","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2026","oa_version":"Published Version","date_updated":"2026-01-12T09:45:54Z","has_accepted_license":"1","date_published":"2026-01-01T00:00:00Z","abstract":[{"lang":"eng","text":"Thus far, Lyman-α damping wings towards quasars have been used to probe the global ionization state of the foreground intergalactic medium (IGM). A new parametrization has demonstrated that the damping wing signature also carries local information about the distribution of neutral hydrogen (H I) in front of the quasar before it started shining. Leveraging a recently introduced Bayesian JAX-based Hamiltonian Monte Carlo inference framework, we derive constraints on the Lorentzian-weighted H I column density NDW H I , the quasar’s distance rpatch to the first neutral patch, and its lifetime tQ based on James Webb Space\r\nTelescope (JWST) Near Infrared Spectrograph (NIRSpec) spectra of the two z ∼ 7.5 quasars J1007+2115 and J1342+0928. After folding in model-dependent topology information, we find that J1007+2115 (and J1342+0928) is most likely to reside in a (xH1)= 0.32+0.22 −0.20 (0.58+0.23 −0.23) neutral IGM while shining for a remarkably short lifetime of log10 tQ/yr = 4.14+0.74 −0.18 (an intermediate lifetime of 5.64+0.25 −0.43) along a sightline with log10 NDW\r\nH I /cm−2 = 19.70+0.35 −0.86 (20.24+0.25 −0.22) and rpatch = 28.9+54.0 −14.4 cMpc\r\n(10.9+5.6−5.9 cMpc). In light of the potential presence of local absorbers in the foreground of J1342+0928 as has been recently suggested, we also demonstrate how the Lorentzian-weighted column density NDW H I provides a natural means for quantifying their contribution to the observed damping wing signal."}],"license":"https://creativecommons.org/licenses/by/4.0/","article_number":"staf2219","quality_controlled":"1","volume":545,"language":[{"iso":"eng"}],"department":[{"_id":"ZoHa"}],"external_id":{"arxiv":["2508.21818"]},"date_created":"2026-01-11T23:01:34Z","publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"DOAJ_listed":"1","acknowledgement":"We acknowledge helpful conversations with the ENIGMA group at UC Santa Barbara and Leiden University. This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programmes #1219 and #1764. This work made use of numpy (C. R. Harris et al. 2020), scipy (P. Virtanen et al. 2020), jax (J. Bradbury et al. 2018), numpyro (E. Bingham et al. 2018; D. Phan, N. Pradhan & M. Jankowiak 2019), sklearn (F. Pedregosa et al. 2011), astropy (Astropy Collaboration 2013, 2018, 2022), PypeIt (J. Prochaska et al. 2020), skycalc_ipy (K. Leschinski 2021), h5py (A. Collette 2013), matplotlib (J. D. Hunter 2007), corner.py (D. Foreman-Mackey 2016), and IPython (F. Pérez & B. E. Granger 2007). TK and JFH acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 885301). JFH acknowledges support from NSF grant no. 2307180. SEIB was supported by the Deutsche Forschungsgemeinschaft (DFG) under Emmy Noether grant number BO 5771/1-1. FW acknowledges support from NSF award AST-2513040.","file":[{"access_level":"open_access","relation":"main_file","success":1,"date_updated":"2026-01-12T09:43:07Z","checksum":"68f04ab0fdcee4f12341d116c5f794cd","content_type":"application/pdf","file_size":2174272,"creator":"dernst","file_name":"2026_MonthNoticesRAS_Kist.pdf","date_created":"2026-01-12T09:43:07Z","file_id":"20979"}],"intvolume":"       545","publication":"Monthly Notices of the Royal Astronomical Society","author":[{"full_name":"Kist, Timo","last_name":"Kist","first_name":"Timo"},{"first_name":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"first_name":"Frederick B.","full_name":"Davies, Frederick B.","last_name":"Davies"},{"last_name":"Bañados","full_name":"Bañados, Eduardo","first_name":"Eduardo"},{"last_name":"Bosman","full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I."},{"first_name":"Zheng","last_name":"Cai","full_name":"Cai, Zheng"},{"last_name":"Eilers","full_name":"Eilers, Anna Christina","first_name":"Anna Christina"},{"first_name":"Xiaohui","full_name":"Fan, Xiaohui","last_name":"Fan"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","orcid":"0000-0003-3633-5403"},{"last_name":"Jun","full_name":"Jun, Hyunsung D.","first_name":"Hyunsung D."},{"last_name":"Liu","full_name":"Liu, Yichen","first_name":"Yichen"},{"first_name":"Jinyi","last_name":"Yang","full_name":"Yang, Jinyi"},{"first_name":"Feige","full_name":"Wang, Feige","last_name":"Wang"}],"scopus_import":"1","file_date_updated":"2026-01-12T09:43:07Z"},{"article_number":"staf2131","abstract":[{"text":"Little Red Dots (LRDs) are compact sources at z > 5 discovered through James Webb Space Telescope spectroscopy. Their spectra exhibit broad Balmer emission lines (>~1000 km s^−1), alongside absorption features and a pronounced Balmer break – evidence for a dense, neutral hydrogen medium, in which the n = 2 state is significantly populated. When interpreted as arising\r\nfrom active galactic nucleus broad-line regions, inferred black hole masses from local scaling relations exceed expectations given their stellar masses, challenging models of early black hole–galaxy co-evolution. However, radiative transfer effects in dense media may also impact the formation of hydrogen emission lines. We model three scattering processes shaping hydrogen\r\nline profiles: resonance scattering by hydrogen in the n = 2 state, Raman scattering of ultraviolet (UV) radiation by ground-state hydrogen, and Thomson scattering by free electrons. Using 3D Monte Carlo radiative transfer simulations, we examine their imprint on line shapes and ratios. Resonance scattering produces strong deviations from Case B flux ratios, clear differences\r\nbetween Hα and Hβ, and encodes gas kinematics in line profiles but cannot broaden Hβ due to conversion to Paα. While Raman scattering can yield broad wings, scattering of the UV continuum is disfavoured given the absence of strong full width at half-maximum variations across transitions. Raman scattering of higher Lyman-series emission can produce Hα/Hβ wing\r\nwidth ratios of  >~1.28, agreeing with observations. Thomson scattering can reproduce the observed >~ 1000 km s^−1 wings under plausible conditions – e.g. Te ∼ 10^4 K and Ne ∼ 10^24 cm^−2 – and lead to black hole mass overestimates by factors  10. Our results provide a framework for interpreting hydrogen lines in LRDs and similar systems.","lang":"eng"}],"volume":545,"quality_controlled":"1","date_created":"2026-01-25T23:01:39Z","department":[{"_id":"JoMa"}],"external_id":{"arxiv":["2508.08768"]},"language":[{"iso":"eng"}],"publication_status":"published","file":[{"file_size":5600366,"date_created":"2026-02-12T12:44:33Z","file_id":"21220","file_name":"2026_MonthNoticesRAS_Chang.pdf","creator":"dernst","date_updated":"2026-02-12T12:44:33Z","content_type":"application/pdf","checksum":"52ba7d7b5b80af0c50f57e4c2acc3930","success":1,"relation":"main_file","access_level":"open_access"}],"DOAJ_listed":"1","acknowledgement":"The authorsthank the anonymousreferee for constructive comments, which improved the clarity of this paper. SJC acknowledges support from the ERC synergy grant 101166930 – RECAP. MG thanks the Max Planck Society for support through the Max Planck Research Group, and the European Union forsupport through ERC-2024-STG 101165038 (ReMMU). JM acknowledges funding by the European Union (ERC, AGENTS, 101076224). CAM acknowledges support\r\nby the European Union ERC grant RISES (101163035), Carlsberg Foundation (CF22-1322), and VILLUM FONDEN (37459). Computations were performed on HPC systems Freya and Orion at the Max Planck Computing and Data Facility.","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"file_date_updated":"2026-02-12T12:44:33Z","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","author":[{"last_name":"Chang","full_name":"Chang, Seok Jun","first_name":"Seok Jun"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"Charlotte","last_name":"Mason","full_name":"Mason, Charlotte"}],"intvolume":"       545","article_processing_charge":"Yes","PlanS_conform":"1","citation":{"ieee":"S. J. Chang, M. Gronke, J. J. Matthee, and C. Mason, “Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 4. Oxford University Press, 2026.","short":"S.J. Chang, M. Gronke, J.J. Matthee, C. Mason, Monthly Notices of the Royal Astronomical Society 545 (2026).","mla":"Chang, Seok Jun, et al. “Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 545, no. 4, staf2131, Oxford University Press, 2026, doi:<a href=\"https://doi.org/10.1093/mnras/staf2131\">10.1093/mnras/staf2131</a>.","chicago":"Chang, Seok Jun, Max Gronke, Jorryt J Matthee, and Charlotte Mason. “Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2026. <a href=\"https://doi.org/10.1093/mnras/staf2131\">https://doi.org/10.1093/mnras/staf2131</a>.","ista":"Chang SJ, Gronke M, Matthee JJ, Mason C. 2026. Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. Monthly Notices of the Royal Astronomical Society. 545(4), staf2131.","ama":"Chang SJ, Gronke M, Matthee JJ, Mason C. Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. <i>Monthly Notices of the Royal Astronomical Society</i>. 2026;545(4). doi:<a href=\"https://doi.org/10.1093/mnras/staf2131\">10.1093/mnras/staf2131</a>","apa":"Chang, S. J., Gronke, M., Matthee, J. J., &#38; Mason, C. (2026). Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf2131\">https://doi.org/10.1093/mnras/staf2131</a>"},"_id":"21038","month":"02","title":"Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots","OA_type":"gold","article_type":"original","doi":"10.1093/mnras/staf2131","OA_place":"publisher","ddc":["520"],"arxiv":1,"issue":"4","publisher":"Oxford University Press","day":"01","type":"journal_article","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","date_published":"2026-02-01T00:00:00Z","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"date_updated":"2026-02-12T12:56:33Z","year":"2026","oa_version":"Published Version"},{"date_created":"2025-06-15T22:01:29Z","external_id":{"arxiv":["2503.12675"],"isi":["001493143700001"]},"department":[{"_id":"IlCa"}],"language":[{"iso":"eng"}],"publication_status":"published","abstract":[{"text":"We report the discovery of two new magnetic cataclysmic variables with brown dwarf companions and long orbital periods (P_{\\rm orb}=95\\pm1 and 104\\pm2 min). This discovery increases the sample of candidate magnetic period bouncers with confirmed sub-stellar donors from four to six. We also find their X-ray luminosity from archival XMM–Newton observations to be in the range L_{\\rm X}\\approx10^{28}-10^{29} \\mathrm{erg\\,s^{-1}} in the 0.25–10 keV band. This low luminosity is comparable with the other candidates, and at least an order of magnitude lower than the X-ray luminosities typically measured in cataclysmic variables. The X-ray fluxes imply mass transfer rates that are much lower than predicted by evolutionary models, even if some of the discrepancy is due to the accretion energy being emitted in other bands, such as via cyclotron emission at infrared wavelengths. Although it is possible that some or all of these systems formed directly as binaries containing a brown dwarf, it is likely that the donor used to be a low-mass star and that the systems followed the evolutionary track for cataclysmic variables, evolving past the period bounce. The donor in long period systems is expected to be a low-mass, cold brown dwarf. This hypothesis is supported by near-infrared photometric observations that constrain the donors in the two systems to be brown dwarfs cooler than \r\n1100 K (spectral types T5 or later), most likely losing mass via Roche Lobe overflow or winds. The serendipitous discovery of two magnetic period bouncers in the small footprint of the XMM–Newton catalogue implies a large space density of these type of systems, possibly compatible with the prediction of 40–70 per cent of magnetic cataclysmic variables to be period bouncers.","lang":"eng"}],"volume":540,"quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-06-23T07:28:36Z","author":[{"first_name":"Tim","full_name":"Cunningham, Tim","last_name":"Cunningham"},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"first_name":"Gracjan","last_name":"Sienkiewicz","full_name":"Sienkiewicz, Gracjan"},{"full_name":"Wheatley, Peter J.","last_name":"Wheatley","first_name":"Peter J."},{"full_name":"Gänsicke, Boris T.","last_name":"Gänsicke","first_name":"Boris T."},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"first_name":"Riccardo","full_name":"Arcodia, Riccardo","last_name":"Arcodia"},{"first_name":"David","full_name":"Charbonneau, David","last_name":"Charbonneau"},{"first_name":"Liam","last_name":"Connor","full_name":"Connor, Liam"},{"first_name":"Kishalay","full_name":"De, Kishalay","last_name":"De"},{"full_name":"Hakala, Pasi","last_name":"Hakala","first_name":"Pasi"},{"last_name":"Kenyon","full_name":"Kenyon, Scott J.","first_name":"Scott J."},{"first_name":"Sumit Kumar","last_name":"Maheshwari","full_name":"Maheshwari, Sumit Kumar"},{"first_name":"Antonio C.","last_name":"Rodriguez","full_name":"Rodriguez, Antonio C."},{"full_name":"Van Roestel, Jan","last_name":"Van Roestel","first_name":"Jan"},{"first_name":"Pier Emmanuel","full_name":"Tremblay, Pier Emmanuel","last_name":"Tremblay"}],"scopus_import":"1","intvolume":"       540","isi":1,"acknowledgement":"We thank Matthias Schreiber for his insightful comments. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51527.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Support for this work was provided by NASA through Chandra Award Number GO4-25014X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. IC was also supported by NASA through grants from the Space Telescope Science Institute, under NASA contracts NASA.22K1813, NAS5-26555, and NAS5-03127. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 101020057). This research was supported in part by grant NSF PHY-1748958 to the Kavli Institute for Theoretical Physics (KITP). PJW acknowledges support from the UK Science and Technology Facilities Council (STFC) through consolidated grants ST/T000406/1 and ST/X001121/1. RA was supported by NASA through the NASA Hubble Fellowship grant #HST-HF2-51499.001-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.\r\n\r\nThis research has made use of data obtained from the 4XMM XMM–Newton Serendipitous Source Catalogue compiled by the 10 institutes of the XMM–Newton Survey Science Centre selected by ESA. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard–Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This work is based in part on data obtained as part of the UKIDSS. This research made use of hips2fits,4 a service provided by CDS, and of astropy (Astropy Collaboration 2013).","file":[{"date_updated":"2025-06-23T07:28:36Z","content_type":"application/pdf","checksum":"5e675d3696c222e919d6916bad194b01","file_size":3212636,"date_created":"2025-06-23T07:28:36Z","file_id":"19864","file_name":"2025_MonthlyNoticesRAS_Cunningham.pdf","creator":"dernst","relation":"main_file","access_level":"open_access","success":1}],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"OA_type":"gold","article_type":"original","OA_place":"publisher","doi":"10.1093/mnras/staf561","ddc":["520"],"arxiv":1,"article_processing_charge":"Yes","citation":{"apa":"Cunningham, T., Caiazzo, I., Sienkiewicz, G., Wheatley, P. J., Gänsicke, B. T., El-Badry, K., … Tremblay, P. E. (2025). Discovery of two new polars evolved past the period bounce. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf561\">https://doi.org/10.1093/mnras/staf561</a>","ama":"Cunningham T, Caiazzo I, Sienkiewicz G, et al. Discovery of two new polars evolved past the period bounce. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;540(1):633-649. doi:<a href=\"https://doi.org/10.1093/mnras/staf561\">10.1093/mnras/staf561</a>","ista":"Cunningham T, Caiazzo I, Sienkiewicz G, Wheatley PJ, Gänsicke BT, El-Badry K, Arcodia R, Charbonneau D, Connor L, De K, Hakala P, Kenyon SJ, Maheshwari SK, Rodriguez AC, Van Roestel J, Tremblay PE. 2025. Discovery of two new polars evolved past the period bounce. Monthly Notices of the Royal Astronomical Society. 540(1), 633–649.","chicago":"Cunningham, Tim, Ilaria Caiazzo, Gracjan Sienkiewicz, Peter J. Wheatley, Boris T. Gänsicke, Kareem El-Badry, Riccardo Arcodia, et al. “Discovery of Two New Polars Evolved Past the Period Bounce.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf561\">https://doi.org/10.1093/mnras/staf561</a>.","short":"T. Cunningham, I. Caiazzo, G. Sienkiewicz, P.J. Wheatley, B.T. Gänsicke, K. El-Badry, R. Arcodia, D. Charbonneau, L. Connor, K. De, P. Hakala, S.J. Kenyon, S.K. Maheshwari, A.C. Rodriguez, J. Van Roestel, P.E. Tremblay, Monthly Notices of the Royal Astronomical Society 540 (2025) 633–649.","mla":"Cunningham, Tim, et al. “Discovery of Two New Polars Evolved Past the Period Bounce.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 540, no. 1, Oxford University Press, 2025, pp. 633–49, doi:<a href=\"https://doi.org/10.1093/mnras/staf561\">10.1093/mnras/staf561</a>.","ieee":"T. Cunningham <i>et al.</i>, “Discovery of two new polars evolved past the period bounce,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 540, no. 1. Oxford University Press, pp. 633–649, 2025."},"_id":"19840","month":"06","title":"Discovery of two new polars evolved past the period bounce","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"633-649","date_published":"2025-06-01T00:00:00Z","has_accepted_license":"1","date_updated":"2025-09-30T12:50:33Z","oa_version":"Published Version","year":"2025","issue":"1","publisher":"Oxford University Press","type":"journal_article","day":"01","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"}},{"article_processing_charge":"Yes","citation":{"apa":"Gazagnes, S., Chisholm, J., Endsley, R., Berg, D. A., Leclercq, F., Jurlin, N., … Schaerer, D. (2025). A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf768\">https://doi.org/10.1093/mnras/staf768</a>","ama":"Gazagnes S, Chisholm J, Endsley R, et al. A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;540(3):2331-2348. doi:<a href=\"https://doi.org/10.1093/mnras/staf768\">10.1093/mnras/staf768</a>","ista":"Gazagnes S, Chisholm J, Endsley R, Berg DA, Leclercq F, Jurlin N, Saldana-Lopez A, Finkelstein SL, Flury SR, Guseva NG, Henry A, Izotov YI, Jung I, Matthee JJ, Schaerer D. 2025. A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization. Monthly Notices of the Royal Astronomical Society. 540(3), 2331–2348.","chicago":"Gazagnes, S., J. Chisholm, R. Endsley, D. A. Berg, F. Leclercq, N. Jurlin, A. Saldana-Lopez, et al. “A Negligible Contribution of Two Luminous z ∼7.5 Galaxies to the Ionizing Photon Budget of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf768\">https://doi.org/10.1093/mnras/staf768</a>.","short":"S. Gazagnes, J. Chisholm, R. Endsley, D.A. Berg, F. Leclercq, N. Jurlin, A. Saldana-Lopez, S.L. Finkelstein, S.R. Flury, N.G. Guseva, A. Henry, Y.I. Izotov, I. Jung, J.J. Matthee, D. Schaerer, Monthly Notices of the Royal Astronomical Society 540 (2025) 2331–2348.","mla":"Gazagnes, S., et al. “A Negligible Contribution of Two Luminous z ∼7.5 Galaxies to the Ionizing Photon Budget of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 540, no. 3, Oxford University Press, 2025, pp. 2331–48, doi:<a href=\"https://doi.org/10.1093/mnras/staf768\">10.1093/mnras/staf768</a>.","ieee":"S. Gazagnes <i>et al.</i>, “A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 540, no. 3. Oxford University Press, pp. 2331–2348, 2025."},"_id":"19855","month":"07","title":"A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization","article_type":"original","OA_type":"gold","OA_place":"publisher","doi":"10.1093/mnras/staf768","ddc":["520"],"arxiv":1,"issue":"3","publisher":"Oxford University Press","type":"journal_article","day":"01","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"2331-2348","has_accepted_license":"1","date_published":"2025-07-01T00:00:00Z","date_updated":"2025-09-30T13:34:20Z","oa_version":"Published Version","year":"2025","abstract":[{"lang":"eng","text":"We present indirect constraints on the absolute escape fraction of ionizing photons (f_{\\rm esc}^{\\rm LyC}) of the system GN 42912 which comprises two luminous galaxies (M_{\\rm UV} magnitudes of -20.89 and -20.37) at z\\sim7.5, GN 42912-NE and GN 42912-SW, to determine their contribution to the ionizing photon budget of the Epoch of Reionization (EoR). The high-resolution James Webb Space Telescope NIRSpec and NIRCam observations reveal the two galaxies are separated by only ~0.1\" (0.5 kpc) on the sky and have a 358 km s^{-1} velocity separation. GN 42912-NE and GN 42912-SW are relatively massive for this redshift (log(M_\\ast/M_\\odot) \\sim 8.4 and 8.9, respectively), with gas-phase metallicities of 18 per cent and 23 per cent solar, O_{32} ratios of 5.3 and >5.8, and \\beta slopes of -1.92 and -1.51, respectively. We use the Mg II\\lambda\\lambda2796,2803 doublet to constrain f_{\\rm esc}^{\\rm LyC}. Mg II has an ionization potential close to that of neutral hydrogen and, in the optically thin regime, can be used as an indirect tracer of the LyC leakage. We establish realistic conservative upper limits on f_{\\rm esc}^{\\rm LyC} of 8.5 per cent for GN 42912-NE and 14 per cent for GN 42912-SW. These estimates align with f_{\\rm esc}^{\\rm LyC} trends observed with \\beta, O_{32}, and the H\\beta equivalent width at z<4. The small inferred ionized region sizes (<0.3 pMpc) around both galaxies indicate they have not ionized a significant fraction of the surrounding neutral gas. While these z>7 f_{\\rm esc}^{\\rm LyC} constraints do not decisively determine a specific reionization model, they support a minor contribution from these two relatively luminous galaxies to the EoR."}],"volume":540,"quality_controlled":"1","date_created":"2025-06-22T22:02:05Z","external_id":{"arxiv":["2410.03337"],"isi":["001506103600001"]},"department":[{"_id":"JoMa"}],"language":[{"iso":"eng"}],"publication_status":"published","file":[{"access_level":"open_access","relation":"main_file","success":1,"date_updated":"2025-06-23T11:02:59Z","content_type":"application/pdf","checksum":"f912c990a0474f1ddf9be6b8a89c7759","file_size":3111567,"creator":"dernst","file_name":"2025_MonthlyNoticesRAS_Gazagnes.pdf","file_id":"19870","date_created":"2025-06-23T11:02:59Z"}],"acknowledgement":"This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–03127 for JWST. These observations are associated with program #01871. Support for program #01871 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–03127. SG is grateful for the support enabled by the Harlan J. Smith McDonald fellowship. YI and NG acknowledge support from the Simons Foundation and the National Academy of Sciences of Ukraine (Project 0121U109612). ASL acknowledges support from Knut and Alice Wallenberg Foundation.","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","file_date_updated":"2025-06-23T11:02:59Z","author":[{"first_name":"S.","last_name":"Gazagnes","full_name":"Gazagnes, S."},{"full_name":"Chisholm, J.","last_name":"Chisholm","first_name":"J."},{"first_name":"R.","full_name":"Endsley, R.","last_name":"Endsley"},{"last_name":"Berg","full_name":"Berg, D. A.","first_name":"D. A."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"full_name":"Jurlin, N.","last_name":"Jurlin","first_name":"N."},{"full_name":"Saldana-Lopez, A.","last_name":"Saldana-Lopez","first_name":"A."},{"first_name":"S. L.","last_name":"Finkelstein","full_name":"Finkelstein, S. L."},{"first_name":"S. R.","last_name":"Flury","full_name":"Flury, S. R."},{"first_name":"N. G.","full_name":"Guseva, N. G.","last_name":"Guseva"},{"full_name":"Henry, A.","last_name":"Henry","first_name":"A."},{"first_name":"Y. I.","full_name":"Izotov, Y. I.","last_name":"Izotov"},{"last_name":"Jung","full_name":"Jung, I.","first_name":"I."},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"full_name":"Schaerer, D.","last_name":"Schaerer","first_name":"D."}],"intvolume":"       540","isi":1},{"type":"journal_article","day":"01","publisher":"Oxford University Press","issue":"2","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","page":"1348-1376","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2025","oa_version":"Published Version","date_updated":"2025-09-30T14:03:40Z","date_published":"2025-08-01T00:00:00Z","has_accepted_license":"1","citation":{"short":"C.A. Pirie, P.N. Best, K.J. Duncan, D.J. Mcleod, R.K. Cochrane, M. Clausen, J.S. Dunlop, S.R. Flury, J.E. Geach, C.L. Hale, E. Ibar, R. Kondapally, Z. Li, J.J. Matthee, R.J. Mclure, L. Ossa-Fuentes, A.L. Patrick, I. Smail, D. Sobral, H.M.O. Stephenson, J.P. Stott, A.M. Swinbank, Monthly Notices of the Royal Astronomical Society 541 (2025) 1348–1376.","mla":"Pirie, C. A., et al. “The JWST Emission Line Survey (JELS): An Untargeted Search for H α Emission Line Galaxies at z &#62; 6 and Their Physical Properties.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2, Oxford University Press, 2025, pp. 1348–76, doi:<a href=\"https://doi.org/10.1093/mnras/staf1006\">10.1093/mnras/staf1006</a>.","ieee":"C. A. Pirie <i>et al.</i>, “The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z &#62; 6 and their physical properties,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2. Oxford University Press, pp. 1348–1376, 2025.","ama":"Pirie CA, Best PN, Duncan KJ, et al. The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z &#62; 6 and their physical properties. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;541(2):1348-1376. doi:<a href=\"https://doi.org/10.1093/mnras/staf1006\">10.1093/mnras/staf1006</a>","apa":"Pirie, C. A., Best, P. N., Duncan, K. J., Mcleod, D. J., Cochrane, R. K., Clausen, M., … Swinbank, A. M. (2025). The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z &#62; 6 and their physical properties. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1006\">https://doi.org/10.1093/mnras/staf1006</a>","chicago":"Pirie, C. A., P. N. Best, K. J. Duncan, D. J. Mcleod, R. K. Cochrane, M. Clausen, J. S. Dunlop, et al. “The JWST Emission Line Survey (JELS): An Untargeted Search for H α Emission Line Galaxies at z &#62; 6 and Their Physical Properties.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1006\">https://doi.org/10.1093/mnras/staf1006</a>.","ista":"Pirie CA, Best PN, Duncan KJ, Mcleod DJ, Cochrane RK, Clausen M, Dunlop JS, Flury SR, Geach JE, Hale CL, Ibar E, Kondapally R, Li Z, Matthee JJ, Mclure RJ, Ossa-Fuentes L, Patrick AL, Smail I, Sobral D, Stephenson HMO, Stott JP, Swinbank AM. 2025. The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z &#62; 6 and their physical properties. Monthly Notices of the Royal Astronomical Society. 541(2), 1348–1376."},"PlanS_conform":"1","article_processing_charge":"Yes","title":"The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z > 6 and their physical properties","month":"08","_id":"20027","OA_place":"publisher","doi":"10.1093/mnras/staf1006","OA_type":"gold","article_type":"original","arxiv":1,"ddc":["520"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"DOAJ_listed":"1","acknowledgement":"The authors would like to thank Adam Carnall and Joel Leja for their helpful advice with the SED fitting of our sample, Callum Donnan for his advice on the selection techniques of high-redshift\r\ngalaxies, Alice Shapley for discussion around H α SFR calibrations at high-redshift, Fred Jennings for providing insight into the interpretation of SFR ratios, and the anonymous referee for their helpful comments – all of which have greatly improved this paper. Several other authors acknowledge the support of the UK Science and Technology Facilities Council (STFC) via grants ST/W507441/1 (CAP), ST/V000594/1 (DJM, PNB, RK, and RJM), ST/Y000951/1 (PNB and RK) and ST/X001075/1 (AMS and IRS), and through an Ernest Rutherford Fellowship (KJD; grant number ST/W003120/1). RKC was funded by support for programme #02321, provided by\r\nNASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-03127. RKC and CLH are both grateful for support from the Leverhulme Trust via a Leverhulme Early Career Fellowship, and CLH also acknowledges support from the Oxford Hintze Centre for Astrophysical Surveys which is funded through generous support from the Hintze Family\r\nCharitable Foundation. JSD acknowledges the support of the Royal Society via a Royal Society Research Professorship. EI gratefully acknowledge financialsupport from ANID–MILENIO–NCN2024 112 and ANID FONDECYT Regular 1221846. LOF acknowledges by ANID BECAS/DOCTORADO NACIONAL 21220499.","file":[{"access_level":"open_access","relation":"main_file","success":1,"checksum":"f8708c78016f8917765026502c6b50b6","content_type":"application/pdf","date_updated":"2025-07-22T07:19:20Z","file_name":"2025_MonthlyNoticesRAS_Pirie.pdf","creator":"dernst","file_id":"20064","date_created":"2025-07-22T07:19:20Z","file_size":38102038}],"isi":1,"intvolume":"       541","author":[{"first_name":"C. A.","full_name":"Pirie, C. A.","last_name":"Pirie"},{"full_name":"Best, P. N.","last_name":"Best","first_name":"P. N."},{"last_name":"Duncan","full_name":"Duncan, K. J.","first_name":"K. J."},{"full_name":"Mcleod, D. J.","last_name":"Mcleod","first_name":"D. J."},{"last_name":"Cochrane","full_name":"Cochrane, R. K.","first_name":"R. K."},{"first_name":"M.","full_name":"Clausen, M.","last_name":"Clausen"},{"first_name":"J. S.","full_name":"Dunlop, J. S.","last_name":"Dunlop"},{"first_name":"S. R.","last_name":"Flury","full_name":"Flury, S. R."},{"first_name":"J. E.","last_name":"Geach","full_name":"Geach, J. E."},{"first_name":"C. L.","last_name":"Hale","full_name":"Hale, C. L."},{"first_name":"E.","last_name":"Ibar","full_name":"Ibar, E."},{"first_name":"R.","full_name":"Kondapally, R.","last_name":"Kondapally"},{"last_name":"Li","full_name":"Li, Zefeng","first_name":"Zefeng"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Mclure, R. J.","last_name":"Mclure","first_name":"R. J."},{"first_name":"L.","last_name":"Ossa-Fuentes","full_name":"Ossa-Fuentes, L."},{"full_name":"Patrick, A. L.","last_name":"Patrick","first_name":"A. L."},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"first_name":"H. M.O.","full_name":"Stephenson, H. M.O.","last_name":"Stephenson"},{"first_name":"J. P.","full_name":"Stott, J. P.","last_name":"Stott"},{"first_name":"A. M.","full_name":"Swinbank, A. M.","last_name":"Swinbank"}],"scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-07-22T07:19:20Z","abstract":[{"lang":"eng","text":"We present the first results of the JWST Emission Line Survey (JELS). Utilizing the first NIRCam narrow-band imaging at 4.7 μm, over 63 arcmin2 in the PRIMER/COSMOS field, we have identified 609 emission line galaxy candidates. From these, we robustly selected 35 H α star-forming galaxies at z ∼ 6.1, with H α star-formation rates (SFRH α) of ∼ 0.9 − 15 M yr−1.\r\nCombining our unique H α sample with the exquisite panchromatic data in the field, we explored their physical properties and star-formation histories, and compared these to a broad-band selected sample at z ∼ 6 which has offered vital new insights into the nature of high-redshift galaxies. UV-continuum slopes (β) were considerably redder for our H α sample (\u0004β\u0005 ∼ −1.92)\r\ncompared to the broad-band sample (\u0004β\u0005 ∼ −2.35). This was not due to dust attenuation as our H α sample was relatively dustpoor (median AV = 0.23); instead, we argue that the reddened slopes could be due to nebular continuum. We compared SFRH α and the UV-continuum-derived SFRUV to SED-fitted measurements averaged over canonical time-scales of 10 and 100 Myr (SFR10 and SFR100). We found an increase in recent SFR for our sample of H α emitters, particularly at lower stellar masses (< 109 M). We also found that SFRH α strongly traces SFR averaged over 10 Myr time-scales, whereas the UV-continuum overpredicts SFR on 100 Myr time-scales at low stellar masses. These results point to our H α sample undergoing ‘bursty’ star\r\nformation. Our F356W z ∼ 6 sample showed a larger scatter in SFR10/SFR100 across all stellar masses, which has highlighted how narrow-band photometric selections of H α emitters are key to quantifying the burstiness of star-formation activity. "}],"quality_controlled":"1","volume":541,"language":[{"iso":"eng"}],"external_id":{"isi":["001527095600001"],"arxiv":["2410.11808"]},"department":[{"_id":"JoMa"}],"date_created":"2025-07-20T22:02:00Z","publication_status":"published"},{"file":[{"file_size":4451937,"file_id":"20063","date_created":"2025-07-22T07:02:02Z","creator":"dernst","file_name":"2025_MonthlyNoticesRAS_Duncan.pdf","date_updated":"2025-07-22T07:02:02Z","checksum":"abedbbce98d448f374dc922dad9133fc","content_type":"application/pdf","success":1,"relation":"main_file","access_level":"open_access"}],"acknowledgement":"We thank the anonymous referee for their helpful and constructive feedback that hassignificantly improved this manuscript. The authors also thank DavidCoulter and ArminRestfor allowing the inclusion of JELS targets in their director’s discretionary observing programme. KJD acknowledges support from the Science and Technology Facilities Council (STFC) through an Ernest Rutherford Fellowship (grant number ST/W003120/1). DJM, PNB, RK, and RJM acknowledge the support of the UK STFC via grant ST/V000594/1. PNB and RK are grateful for support from the UK STFC via grant ST/Y000951/1. RKC was funded by support for programme #02321, provided by NASA through a grant from the Space Telescope Science Institute,\r\nwhich is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-03127. RKC is grateful for support from the Leverhulme Trust via the Leverhulme Early Career Fellowship.JSD acknowledgesthe support of the Royal Society via a Royal Society Research Professorship. CLH acknowledges support from the Leverhulme Trust through an Early Career Research Fellowship and also acknowledge support from the Oxford\r\nHintze Centre for Astrophysical Surveys which is funded through generous support from the Hintze Family Charitable Foundation. EI gratefully acknowledge financial support from ANID –MILENIO – NCN2024 112 and ANID FONDECYT Regular 1221846. AMS and IRS acknowledge support from the STFC via grant ST/X001075/1.This work was initiated in part at Aspen Center for Physics, which is supported by National Science Foundation grant PHY-2210452.","DOAJ_listed":"1","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","author":[{"first_name":"K. J.","last_name":"Duncan","full_name":"Duncan, K. J."},{"last_name":"Mcleod","full_name":"Mcleod, D. J.","first_name":"D. J."},{"first_name":"P. N.","last_name":"Best","full_name":"Best, P. N."},{"first_name":"C. A.","last_name":"Pirie","full_name":"Pirie, C. A."},{"full_name":"Clausen, M.","last_name":"Clausen","first_name":"M."},{"first_name":"R. K.","last_name":"Cochrane","full_name":"Cochrane, R. K."},{"first_name":"J. S.","full_name":"Dunlop, J. S.","last_name":"Dunlop"},{"last_name":"Flury","full_name":"Flury, S. R.","first_name":"S. R."},{"last_name":"Geach","full_name":"Geach, J. E.","first_name":"J. E."},{"full_name":"Grogin, N. A.","last_name":"Grogin","first_name":"N. A."},{"first_name":"C. L.","last_name":"Hale","full_name":"Hale, C. L."},{"first_name":"E.","full_name":"Ibar, E.","last_name":"Ibar"},{"last_name":"Kondapally","full_name":"Kondapally, R.","first_name":"R."},{"first_name":"Zefeng","full_name":"Li, Zefeng","last_name":"Li"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"R. J.","full_name":"Mclure, R. J.","last_name":"Mclure"},{"first_name":"Luis","last_name":"Ossa-Fuentes","full_name":"Ossa-Fuentes, Luis"},{"first_name":"A. L.","full_name":"Patrick, A. L.","last_name":"Patrick"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"first_name":"H. M.O.","last_name":"Stephenson","full_name":"Stephenson, H. M.O."},{"first_name":"J. P.","full_name":"Stott, J. P.","last_name":"Stott"},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."}],"publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-07-22T07:02:02Z","isi":1,"intvolume":"       541","volume":541,"quality_controlled":"1","abstract":[{"lang":"eng","text":"We present the JWST Emission-Line Survey (JELS), a JWST imaging programme exploiting the wavelength coverage and sensitivity of the Near-Infrared Camera (NIRCam) to extend narrow-band rest-optical emission-line selection into the Epoch of Reionization (EoR) for the first time, and to enable unique studies of the resolved ionized gas morphology in individual galaxies across cosmic history. The primary JELS observations comprise ∼ 4.7 μm narrow-band imaging over ∼ 63 arcmin2 designed to enable selection of H α emitters at z ∼ 6.1 and a host of novel emission-line samples, including [O III] (z ∼ 8.3) and Paschen α/β (z ∼ 1.5/2.8). For the F466N/F470N narrow-band observations, the emission-line sensitivities achieved are up to ∼ 2× more sensitive than current slitless spectroscopy surveys (5σ limits of 0.8–1.2×10−18 erg s−1cm−2), corresponding to unobscured H α star formation rates (SFRs) of 0.9–1.3 M yr−1 at z ∼ 6.1, extending emission-line selections in the EoR to fainter populations. Simultaneously, JELS also adds F200W broad-band and F212N narrow-band imaging (H α at z ∼ 2.23) that probes SFRs  5× fainter than previous ground-based narrow-band studies (∼ 0.2 M yr−1), offering an unprecedented resolved view of star formation at cosmic noon. We present the detailed JELS design, key data processing steps specific to the survey observations, and demonstrate the exceptional data quality and imaging sensitivity achieved. We then summarize the key scientific goals of JELS, demonstrate the precision and accuracy of the expected redshift and measured emission-line recovery through detailed simulations, and present examples of spectroscopically confirmed H α and [O III] emitters discovered by JELS that illustrate the novel parameter space probed."}],"publication_status":"published","date_created":"2025-07-20T22:02:00Z","external_id":{"isi":["001527085900001"],"arxiv":["2410.09000"]},"department":[{"_id":"JoMa"}],"language":[{"iso":"eng"}],"status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"issue":"2","day":"01","publisher":"Oxford University Press","type":"journal_article","date_published":"2025-08-01T00:00:00Z","has_accepted_license":"1","date_updated":"2025-09-30T14:03:01Z","year":"2025","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"1329-1347","_id":"20028","month":"08","title":"The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization","article_processing_charge":"Yes","PlanS_conform":"1","citation":{"mla":"Duncan, K. J., et al. “The JWST Emission-Line Survey: Extending Rest-Optical Narrow-Band Emission-Line Selection into the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2, Oxford University Press, 2025, pp. 1329–47, doi:<a href=\"https://doi.org/10.1093/mnras/staf1061\">10.1093/mnras/staf1061</a>.","short":"K.J. Duncan, D.J. Mcleod, P.N. Best, C.A. Pirie, M. Clausen, R.K. Cochrane, J.S. Dunlop, S.R. Flury, J.E. Geach, N.A. Grogin, C.L. Hale, E. Ibar, R. Kondapally, Z. Li, J.J. Matthee, R.J. Mclure, L. Ossa-Fuentes, A.L. Patrick, I. Smail, D. Sobral, H.M.O. Stephenson, J.P. Stott, A.M. Swinbank, Monthly Notices of the Royal Astronomical Society 541 (2025) 1329–1347.","ieee":"K. J. Duncan <i>et al.</i>, “The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2. Oxford University Press, pp. 1329–1347, 2025.","apa":"Duncan, K. J., Mcleod, D. J., Best, P. N., Pirie, C. A., Clausen, M., Cochrane, R. K., … Swinbank, A. M. (2025). The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1061\">https://doi.org/10.1093/mnras/staf1061</a>","ama":"Duncan KJ, Mcleod DJ, Best PN, et al. The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;541(2):1329-1347. doi:<a href=\"https://doi.org/10.1093/mnras/staf1061\">10.1093/mnras/staf1061</a>","ista":"Duncan KJ, Mcleod DJ, Best PN, Pirie CA, Clausen M, Cochrane RK, Dunlop JS, Flury SR, Geach JE, Grogin NA, Hale CL, Ibar E, Kondapally R, Li Z, Matthee JJ, Mclure RJ, Ossa-Fuentes L, Patrick AL, Smail I, Sobral D, Stephenson HMO, Stott JP, Swinbank AM. 2025. The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 541(2), 1329–1347.","chicago":"Duncan, K. J., D. J. Mcleod, P. N. Best, C. A. Pirie, M. Clausen, R. K. Cochrane, J. S. Dunlop, et al. “The JWST Emission-Line Survey: Extending Rest-Optical Narrow-Band Emission-Line Selection into the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1061\">https://doi.org/10.1093/mnras/staf1061</a>."},"ddc":["520"],"arxiv":1,"OA_type":"gold","article_type":"original","OA_place":"publisher","doi":"10.1093/mnras/staf1061"},{"date_created":"2025-08-31T22:01:31Z","external_id":{"isi":["001553472000001"],"arxiv":["2501.12986"]},"department":[{"_id":"ZoHa"}],"language":[{"iso":"eng"}],"publication_status":"published","abstract":[{"text":"Population III stars are possible precursors to early supermassive black holes (BHs). The presence of soft UV Lyman–Werner (LW) background radiation can suppress Population III star formation in minihaloes and allow them to form in pristine atomic-cooling haloes. In the absence of molecular hydrogen (⁠H2⁠) cooling, atomic-cooling haloes enable rapid collapse with suppressed fragmentation. High background LW fluxes from preceding star-formation have been proposed to dissociate H2⁠. This flux can be supplemented by LW radiation from one or more Population III star(s) in the same halo, reducing the necessary background level. Here, we consider atomic-cooling haloes in which multiple protostellar cores form close to one another nearly simultaneously. We assess whether the first star’s LW radiation can dissociate nearby \r\n⁠, enabling rapid accretion on to a nearby protostellar core, and the prompt formation of a second, supermassive star (SMS) from warm, atomically-cooled gas. We use a set of hydrodynamical simulations with the code enzo, with identical LW backgrounds centred on a halo with two adjacent collapsing gas clumps. When an additional large local LW flux is introduced, we observe immediate reductions in both the accretion rates and the stellar masses that form within these clumps. While the LW flux reduces the H2 fraction and increases the gas temperature, the halo core’s potential well is too shallow to promptly heat the gas to >1000 K and increase the second protostar’s accretion rate. We conclude that this internal LW feedback scenario is unlikely to facilitate SMS or massive BH seed formation.","lang":"eng"}],"volume":542,"quality_controlled":"1","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-09-03T05:44:47Z","author":[{"first_name":"James","last_name":"Sullivan","full_name":"Sullivan, James"},{"orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"first_name":"Mihir","full_name":"Kulkarni, Mihir","last_name":"Kulkarni"},{"last_name":"Visbal","full_name":"Visbal, Eli","first_name":"Eli"}],"isi":1,"intvolume":"       542","DOAJ_listed":"1","file":[{"access_level":"open_access","relation":"main_file","success":1,"date_updated":"2025-09-03T05:44:47Z","checksum":"2a06796b27da0b33d479dba170ba4b3f","content_type":"application/pdf","file_size":2780496,"creator":"dernst","file_name":"2025_MonthlyNoticesRAS_Sullivan.pdf","date_created":"2025-09-03T05:44:47Z","file_id":"20279"}],"acknowledgement":"We thank the anonymous referee for comments that helped us improve the clarity of this manuscript. We acknowledge support from the United States National Science Foundation (NSF) grant AST-2006176 and the National Aeronautics and Space Administration (NASA) grants 80NSSC24K0440 and 80NSSC22K0822 (ZH). We also acknowledge support from NSF grant AST-2009309, NASA Astrophysics Theory Program grant 80NSSC22K0629, and Space Telescope Science Institute grant JWST-AR-05238 (EV). The simulations in this work were run on Texas Advanced Computing Center’s Stampede2 and Stampede3 systems. We used Stampede2 and Purdue University’s computing system Anvil for data analysis.","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"OA_type":"gold","article_type":"original","doi":"10.1093/mnras/staf1269","OA_place":"publisher","ddc":["520"],"arxiv":1,"article_processing_charge":"Yes","PlanS_conform":"1","citation":{"apa":"Sullivan, J., Haiman, Z., Kulkarni, M., &#38; Visbal, E. (2025). Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1269\">https://doi.org/10.1093/mnras/staf1269</a>","ama":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;542(2):822-838. doi:<a href=\"https://doi.org/10.1093/mnras/staf1269\">10.1093/mnras/staf1269</a>","ista":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. 2025. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 542(2), 822–838.","chicago":"Sullivan, James, Zoltán Haiman, Mihir Kulkarni, and Eli Visbal. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1269\">https://doi.org/10.1093/mnras/staf1269</a>.","mla":"Sullivan, James, et al. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 542, no. 2, Oxford University Press, 2025, pp. 822–38, doi:<a href=\"https://doi.org/10.1093/mnras/staf1269\">10.1093/mnras/staf1269</a>.","short":"J. Sullivan, Z. Haiman, M. Kulkarni, E. Visbal, Monthly Notices of the Royal Astronomical Society 542 (2025) 822–838.","ieee":"J. Sullivan, Z. Haiman, M. Kulkarni, and E. Visbal, “Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 542, no. 2. Oxford University Press, pp. 822–838, 2025."},"_id":"20250","month":"09","title":"Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"822-838","date_published":"2025-09-01T00:00:00Z","has_accepted_license":"1","date_updated":"2025-09-30T14:28:05Z","year":"2025","oa_version":"Published Version","issue":"2","type":"journal_article","publisher":"Oxford University Press","day":"01","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"}},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"DOAJ_listed":"1","file":[{"access_level":"open_access","relation":"main_file","success":1,"content_type":"application/pdf","checksum":"d3190e974ce771e96c4c16ee98abb82a","date_updated":"2025-10-27T09:06:51Z","creator":"dernst","file_name":"2025_MonthlyNoticesRAS_Komori.pdf","file_id":"20549","date_created":"2025-10-27T09:06:51Z","file_size":4864160}],"acknowledgement":"We thank Seiji Fujimoto for discussions in the early stage of this work. We were supported by JSPS (Japan Society for the Promotion of Science) KAKENHI Grant Numbers 21H04489, 22H04939, 23H00131, 24H00002, 24K17095, 25K01038, and 25K01039. Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit organization operated as a scientific partnership among the California Institute of Technology,\r\nthe University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this\r\nmountain. This research made use of MONTAGE. It is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation\r\nTechnologies Project, underCooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.","isi":1,"intvolume":"       543","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","file_date_updated":"2025-10-27T09:06:51Z","author":[{"first_name":"Fuga","full_name":"Komori, Fuga","last_name":"Komori"},{"first_name":"Akio K","full_name":"Inoue, Akio K","last_name":"Inoue"},{"last_name":"Mawatari","full_name":"Mawatari, Ken","first_name":"Ken"},{"first_name":"Yuma","last_name":"Sugahara","full_name":"Sugahara, Yuma"},{"full_name":"Umehata, Hideki","last_name":"Umehata","first_name":"Hideki"},{"first_name":"Rhythm","last_name":"Shimakawa","full_name":"Shimakawa, Rhythm"},{"full_name":"Yamanaka, Satoshi","last_name":"Yamanaka","first_name":"Satoshi"},{"first_name":"Takuya","full_name":"Hashimoto, Takuya","last_name":"Hashimoto"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Toru","last_name":"Misawa","full_name":"Misawa, Toru"}],"quality_controlled":"1","volume":543,"abstract":[{"lang":"eng","text":"The H i gas distribution in damped Lyman $\\alpha$ absorbers (DLAs) has remained elusive due to the point-source nature of background quasar emission. Observing DLAs against spatially extended background galaxies provides a new method for constraining their size and structure. Using the Keck Cosmic Web Imager, we present the first ‘silhouette’ image of a DLA at $z=3.34$, identified in the spectrum of a background galaxy at $z=3.61$. Although the silhouette remains unresolved due to limited spatial resolution, this represents a successful proof-of-concept for studying DLA morphology using extended background sources. Possible residual emission in the DLA trough suggests an optical depth contrast exceeding $10^7$ in the internal structure, implying a sharp edge or patchy structure. A Lyman $\\alpha$ emitter (LAE) at $z_{\\rm LAE}=3.3433\\pm 0.0005$, consistent with the DLA redshift, is detected at an angular separation of $1{{_{.}^{\\prime\\prime}} }73\\pm 0{{_{.}^{\\prime\\prime}} }28$ ($12.9\\pm 2.1$ kpc). The DLA is surrounded by three galaxies within 140 kpc in projected distance and 500 km s$^{-1}$ in line-of-sight velocity, indicating that it resides in the circumgalactic medium of the LAE or within a galaxy group/protocluster environment. An O i  $\\lambda 1302$ absorption at $z_{\\rm OI}=3.3288\\pm 0.0004$ is also detected along the line of sight. This absorber may trace metal-enriched outflow from the LAE or a gas-rich galaxy exhibiting the highest star formation activity among the surrounding galaxies. Future large spectroscopic surveys of galaxies will expand such a DLA sample, and three-dimensional spectroscopy for it will shed new light on the role of intergalactic dense gas in galaxy formation and evolution."}],"publication_status":"published","language":[{"iso":"eng"}],"department":[{"_id":"JoMa"}],"external_id":{"isi":["001592326700001"]},"date_created":"2025-10-27T08:18:07Z","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","publisher":"Oxford University Press","day":"25","type":"journal_article","issue":"3","oa_version":"Published Version","year":"2025","date_updated":"2025-12-01T15:07:43Z","has_accepted_license":"1","date_published":"2025-09-25T00:00:00Z","page":"2943-2957","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy","month":"09","_id":"20545","citation":{"ieee":"F. Komori <i>et al.</i>, “The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3. Oxford University Press, pp. 2943–2957, 2025.","mla":"Komori, Fuga, et al. “The First Direct Imaging of the Silhouette of a Damped Lyman α System along the Line-of-Sight to a Background Galaxy.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3, Oxford University Press, 2025, pp. 2943–57, doi:<a href=\"https://doi.org/10.1093/mnras/staf1622\">10.1093/mnras/staf1622</a>.","short":"F. Komori, A.K. Inoue, K. Mawatari, Y. Sugahara, H. Umehata, R. Shimakawa, S. Yamanaka, T. Hashimoto, J.J. Matthee, T. Misawa, Monthly Notices of the Royal Astronomical Society 543 (2025) 2943–2957.","chicago":"Komori, Fuga, Akio K Inoue, Ken Mawatari, Yuma Sugahara, Hideki Umehata, Rhythm Shimakawa, Satoshi Yamanaka, Takuya Hashimoto, Jorryt J Matthee, and Toru Misawa. “The First Direct Imaging of the Silhouette of a Damped Lyman α System along the Line-of-Sight to a Background Galaxy.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1622\">https://doi.org/10.1093/mnras/staf1622</a>.","ista":"Komori F, Inoue AK, Mawatari K, Sugahara Y, Umehata H, Shimakawa R, Yamanaka S, Hashimoto T, Matthee JJ, Misawa T. 2025. The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy. Monthly Notices of the Royal Astronomical Society. 543(3), 2943–2957.","ama":"Komori F, Inoue AK, Mawatari K, et al. The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;543(3):2943-2957. doi:<a href=\"https://doi.org/10.1093/mnras/staf1622\">10.1093/mnras/staf1622</a>","apa":"Komori, F., Inoue, A. K., Mawatari, K., Sugahara, Y., Umehata, H., Shimakawa, R., … Misawa, T. (2025). The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1622\">https://doi.org/10.1093/mnras/staf1622</a>"},"PlanS_conform":"1","article_processing_charge":"Yes","ddc":["520"],"doi":"10.1093/mnras/staf1622","OA_place":"publisher","OA_type":"gold","article_type":"original"},{"abstract":[{"text":"We used observations from the JWST Emission Line Survey (JELS) to measure the half-light radii (re) of 23 Hα-emitting starforming (SF) galaxies at z = 6.1 in the PRIMER/COSMOS field. Galaxy sizes were measured in JWST near-infrared camera observations in rest-frame Hα (tracing recent star formation) with the F466N and F470N narrow-band filters from JELS, and\r\ncompared against rest-R- and V -band (tracing established stellar populations) and near-ultraviolet sizes. We find a size–stellar mass(re − M∗) relationship with a slope that is consistent with literature values at lower redshifts, though offset to lowersizes. We observe a large scatter in re at low stellar mass (M∗ < 10^8.4 Mo) which we believe is the result of bursty star formation histories (SFHs) of SF galaxies at the Epoch of Reionization (EoR). We find that the stellar and ionized gas components are similar in size at z = 6.1. The evidence of already-established stellar components in these Hα emitters (HAEs) indicates previous episodes of star formation have occurred. As such, following other JELS studies finding our HAEs are undergoing a current burst of star formation, we believe our results indicate that SF galaxies at the end of the EoR have already experienced a bursty SFH. From our re − M∗ relationship, we find re,F444W = 0.76 ± 0.46 kpc for fixed stellar mass M∗ = 10^9.25 M, which is in agreement with other observations and simulations of SF galaxies in the literature. We find a close-pair (major) merger fraction of (fmaj. merger =0.44 ± 0.22) fmerger = 0.43 ± 0.11 for galaxy separations d <~ 25 kpc, which is in agreement with other z ≈ 6 studies.","lang":"eng"}],"quality_controlled":"1","volume":544,"language":[{"iso":"eng"}],"department":[{"_id":"JoMa"}],"external_id":{"isi":["001611415800001"]},"date_created":"2025-11-23T23:01:37Z","publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"DOAJ_listed":"1","file":[{"content_type":"application/pdf","checksum":"ddb3f429d2246bbf536efb4b0e52f3a8","date_updated":"2025-11-24T10:35:15Z","date_created":"2025-11-24T10:35:15Z","file_id":"20678","creator":"dernst","file_name":"2025_MonthlyNoticesRAS_Stephenson.pdf","file_size":3625308,"relation":"main_file","access_level":"open_access","success":1}],"acknowledgement":"This work makes use of ASTROPY, 7 a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018, 2022), as well as the NUMPY (C. R. Harris et al. 2020) and SCIPY (P.Virtanen et al. 2020) packages(see also T. E. Oliphant 2007). All plots\r\nwere created using the MATPLOTLIB 2D graphics PYTHON package (J. D. Hunter 2007). Conversions between redshift and lookback time in our selected cosmological model were done using the Javascript cosmological calculator from E. L. Wright (2006).8 The authors would like to thank the anonymous referee for their constructive comments and suggestions which have strengthened the analysis of this work and improved the paper. The authors also gratefully acknowledge Ian Smail for providing valuable feedback and helping to guide the science of this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space\r\nTelescope. The data were obtained from the Mikulski Archive for Space Telescopes9 at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programs GO no. 2321 (JELS) and GO no. 1837 (PRIMER). The authors acknowledge the PRIMER team for developing their observing program with a zero-exclusive-access period. HMOS acknowledges support from an STFC PhD studentship and the Faculty of Science and Technology at Lancaster University. PNB is grateful for support from the UK STFC\r\nvia grants ST/V000594/1 and ST/Y000951/1. JSD acknowledges the support of the Royal Society via a Royal Society Research Professorship. LOF acknowledges funding by ANID BECAS/DOCTORADO NACIONAL 21220499.CLH acknowledges support from the Oxford\r\nHintze Centre for Astrophysical Surveys which is funded through generous support from the Hintze family charity foundation. EI gratefully acknowledge financial support from ANID – MILENIO –NCN2024 112 and ANID FONDECYT Regular 1221846. For the purpose of open access, the authors have applied a Creative Commons attribution (CC BY) licence to any author accepted manuscript version arising.","intvolume":"       544","isi":1,"publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-11-24T10:35:15Z","author":[{"full_name":"Stephenson, H. M.O.","last_name":"Stephenson","first_name":"H. M.O."},{"last_name":"Stott","full_name":"Stott, J. P.","first_name":"J. P."},{"last_name":"Pirie","full_name":"Pirie, C. A.","first_name":"C. A."},{"first_name":"K. J.","last_name":"Duncan","full_name":"Duncan, K. J."},{"first_name":"D. J.","last_name":"Mcleod","full_name":"Mcleod, D. J."},{"first_name":"P. N.","last_name":"Best","full_name":"Best, P. N."},{"last_name":"Brinch","full_name":"Brinch, M.","first_name":"M."},{"first_name":"M.","last_name":"Clausen","full_name":"Clausen, M."},{"last_name":"Cochrane","full_name":"Cochrane, R. K.","first_name":"R. K."},{"first_name":"J. S.","last_name":"Dunlop","full_name":"Dunlop, J. S."},{"last_name":"Flury","full_name":"Flury, S. R.","first_name":"S. R."},{"first_name":"J. E.","last_name":"Geach","full_name":"Geach, J. E."},{"first_name":"C. L.","full_name":"Hale, C. L.","last_name":"Hale"},{"first_name":"E.","full_name":"Ibar, E.","last_name":"Ibar"},{"first_name":"Zefeng","full_name":"Li, Zefeng","last_name":"Li"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Mclure","full_name":"Mclure, R. J.","first_name":"R. J."},{"first_name":"L.","last_name":"Ossa-Fuentes","full_name":"Ossa-Fuentes, L."},{"full_name":"Patrick, A. L.","last_name":"Patrick","first_name":"A. L."},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Swinbank, A. M.","last_name":"Swinbank","first_name":"A. M."}],"scopus_import":"1","citation":{"apa":"Stephenson, H. M. O., Stott, J. P., Pirie, C. A., Duncan, K. J., Mcleod, D. J., Best, P. N., … Swinbank, A. M. (2025). The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1725\">https://doi.org/10.1093/mnras/staf1725</a>","ama":"Stephenson HMO, Stott JP, Pirie CA, et al. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;544(2):1412-1431. doi:<a href=\"https://doi.org/10.1093/mnras/staf1725\">10.1093/mnras/staf1725</a>","ista":"Stephenson HMO, Stott JP, Pirie CA, Duncan KJ, Mcleod DJ, Best PN, Brinch M, Clausen M, Cochrane RK, Dunlop JS, Flury SR, Geach JE, Hale CL, Ibar E, Li Z, Matthee JJ, Mclure RJ, Ossa-Fuentes L, Patrick AL, Sobral D, Swinbank AM. 2025. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 544(2), 1412–1431.","chicago":"Stephenson, H. M.O., J. P. Stott, C. A. Pirie, K. J. Duncan, D. J. Mcleod, P. N. Best, M. Brinch, et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1725\">https://doi.org/10.1093/mnras/staf1725</a>.","mla":"Stephenson, H. M. O., et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2, Oxford University Press, 2025, pp. 1412–31, doi:<a href=\"https://doi.org/10.1093/mnras/staf1725\">10.1093/mnras/staf1725</a>.","short":"H.M.O. Stephenson, J.P. Stott, C.A. Pirie, K.J. Duncan, D.J. Mcleod, P.N. Best, M. Brinch, M. Clausen, R.K. Cochrane, J.S. Dunlop, S.R. Flury, J.E. Geach, C.L. Hale, E. Ibar, Z. Li, J.J. Matthee, R.J. Mclure, L. Ossa-Fuentes, A.L. Patrick, D. Sobral, A.M. Swinbank, Monthly Notices of the Royal Astronomical Society 544 (2025) 1412–1431.","ieee":"H. M. O. Stephenson <i>et al.</i>, “The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2. Oxford University Press, pp. 1412–1431, 2025."},"PlanS_conform":"1","article_processing_charge":"Yes","title":"The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization","month":"12","_id":"20660","doi":"10.1093/mnras/staf1725","OA_place":"publisher","article_type":"original","OA_type":"gold","ddc":["520"],"publisher":"Oxford University Press","type":"journal_article","day":"01","issue":"2","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","page":"1412-1431","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Published Version","year":"2025","date_updated":"2025-12-01T15:25:11Z","has_accepted_license":"1","date_published":"2025-12-01T00:00:00Z"},{"article_processing_charge":"Yes","PlanS_conform":"1","citation":{"apa":"Dalmasso, N., Watson, P. J., Treu, T., Trenti, M., Vulcani, B., Nanayakkara, T., … Pentericci, L. (2025). Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1837\">https://doi.org/10.1093/mnras/staf1837</a>","ama":"Dalmasso N, Watson PJ, Treu T, et al. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;544(2):1915-1925. doi:<a href=\"https://doi.org/10.1093/mnras/staf1837\">10.1093/mnras/staf1837</a>","ista":"Dalmasso N, Watson PJ, Treu T, Trenti M, Vulcani B, Nanayakkara T, Bradač M, Jones T, Boyett K, Wang X, Mascia S, Pentericci L. 2025. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. Monthly Notices of the Royal Astronomical Society. 544(2), 1915–1925.","chicago":"Dalmasso, Nicolò, Peter J. Watson, Tommaso Treu, Michele Trenti, Benedetta Vulcani, Themiya Nanayakkara, Maruša Bradač, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1837\">https://doi.org/10.1093/mnras/staf1837</a>.","mla":"Dalmasso, Nicolò, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2, Oxford University Press, 2025, pp. 1915–25, doi:<a href=\"https://doi.org/10.1093/mnras/staf1837\">10.1093/mnras/staf1837</a>.","short":"N. Dalmasso, P.J. Watson, T. Treu, M. Trenti, B. Vulcani, T. Nanayakkara, M. Bradač, T. Jones, K. Boyett, X. Wang, S. Mascia, L. Pentericci, Monthly Notices of the Royal Astronomical Society 544 (2025) 1915–1925.","ieee":"N. Dalmasso <i>et al.</i>, “Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2. Oxford University Press, pp. 1915–1925, 2025."},"_id":"20661","month":"12","title":"Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies","OA_type":"gold","article_type":"original","OA_place":"publisher","doi":"10.1093/mnras/staf1837","ddc":["520"],"arxiv":1,"issue":"2","publisher":"Oxford University Press","type":"journal_article","day":"01","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"1915-1925","has_accepted_license":"1","date_published":"2025-12-01T00:00:00Z","date_updated":"2025-12-01T15:23:21Z","oa_version":"Published Version","year":"2025","abstract":[{"lang":"eng","text":"We analyse James Webb Space Telescope (JWST) Near Infrared Imager and Slitless Spectrograph (NIRISS) and Near Infrared Spectrograph (NIRSpec) spectroscopic observations in the Abell 2744 galaxy cluster field. From approximately 120 candidates, we identify 12 objects with at least two prominent emission lines among [O II] λ3727, H β λ4861, [O III] λ4959, [O III] λ5007, and H α λ6563 that are spectroscopically confirmed by both instruments. Our key findings reveal systematic differences between the two spectrographs based on source morphology and shutter aperture placement. Compact objects show comparable or higher\r\nintegrated flux in NIRSpec relative to NIRISS (within 1σ uncertainties), while extended sources consistently display higher flux in NIRISS measurements. This pattern reflects NIRSpec’s optimal coverage for compact objects while potentially undersampling extended sources. Quantitative analysis demonstrates that NIRSpec recovers at least 63 per cent of NIRISS-measured flux when the slit covers >15 per cent of the source or when Re < 1 kpc. For lower coverage or larger effective radii, the recovered flux varies from 24 per cent to 63 per cent. When studying the H α λ6563/[O III] λ5007 emission line ratio, we observe that\r\nmeasurements from these different spectrographs can vary by up to ∼0.3 dex, with significant implications for metallicity and star formation rate characterizations for individual galaxies. These results highlight the importance of considering instrumental effects when combining multi-instrument spectroscopic data and demonstrate that source morphology critically influences flux\r\nrecovery between slit-based and slitless spectroscopic modes in JWST observations."}],"volume":544,"quality_controlled":"1","date_created":"2025-11-23T23:01:38Z","department":[{"_id":"JoMa"}],"external_id":{"isi":["001615620500001"],"arxiv":["2510.27036"]},"language":[{"iso":"eng"}],"publication_status":"published","acknowledgement":"This research was supported in part by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research was supported in part by The Dr Albert Shimmins Fund through the Albert Shimmins Postgraduate Writing Up Award (University of Melbourne). This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–03127 for JWST. These observations are associated with programmes JWST-ERS-1324, JWST-GO-2561, and JWST-DDT-2756. BV and PW acknowledge support from the INAF Large Grant 2022 ‘Extragalactic Surveys with JWST’ (PI Pentericci), the INAF Mini\r\nGrant ‘1.05.24.07.01 RSN1: Spatially-Resolved Near-IR Emission of Intermediate-Redshift Jellyfish Galaxies’ (PI Watson), and are supported by the European Union – NextGenerationEU RFF M4C2 1.1 PRIN 2022 project 2022ZSL4BL INSIGHT. MB acknowledges support from the ERC Advanced Grant FIRSTLIGHT and Slovenian national research agency ARIS through grants N1-0238 and P1-0188. ","DOAJ_listed":"1","file":[{"success":1,"relation":"main_file","access_level":"open_access","file_size":1952887,"date_created":"2025-11-24T09:02:04Z","file_id":"20674","file_name":"2025_MonthlyNoticesRAS_Dalmasso.pdf","creator":"dernst","date_updated":"2025-11-24T09:02:04Z","checksum":"2caff0a3b81fed114408377323298b43","content_type":"application/pdf"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"author":[{"last_name":"Dalmasso","full_name":"Dalmasso, Nicolò","first_name":"Nicolò"},{"first_name":"Peter J.","last_name":"Watson","full_name":"Watson, Peter J."},{"first_name":"Tommaso","last_name":"Treu","full_name":"Treu, Tommaso"},{"last_name":"Trenti","full_name":"Trenti, Michele","first_name":"Michele"},{"first_name":"Benedetta","last_name":"Vulcani","full_name":"Vulcani, Benedetta"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"first_name":"Maruša","last_name":"Bradač","full_name":"Bradač, Maruša"},{"full_name":"Jones, Tucker","last_name":"Jones","first_name":"Tucker"},{"first_name":"Kristan","last_name":"Boyett","full_name":"Boyett, Kristan"},{"last_name":"Wang","full_name":"Wang, Xin","first_name":"Xin"},{"last_name":"Mascia","full_name":"Mascia, Sara","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29"},{"first_name":"Laura","full_name":"Pentericci, Laura","last_name":"Pentericci"}],"scopus_import":"1","file_date_updated":"2025-11-24T09:02:04Z","publication":"Monthly Notices of the Royal Astronomical Society","isi":1,"intvolume":"       544"},{"language":[{"iso":"eng"}],"date_created":"2025-02-02T23:01:53Z","external_id":{"arxiv":["2410.19695"],"isi":["001400731500001"]},"department":[{"_id":"YlGo"},{"_id":"LiBu"}],"publication_status":"published","abstract":[{"lang":"eng","text":"Although planets have been found orbiting binary systems, whether they can survive binary interactions is debated. While the tightest-orbit binaries should host the most dynamically stable and long-lived circumbinary planetary systems, they are also the systems that are expected to experience mass transfer, common envelope evolution, or stellar mergers. In this study, we explore the effect of stable non-conservative mass transfer on the dynamical evolution of circumbinary planets. We present a new script that seamlessly integrates binary evolution data from the 1D binary stellar evolution code MESA into the N-body simulation code REBOUND. This integration framework enables a comprehensive examination of the dynamical evolution of circumbinary planets orbiting mass-transferring binaries, while simultaneously accounting for the detailed stellar structure evolution. In addition, we introduce a recalibration method to mitigate numerical errors from updates of binary properties during the system's dynamical evolution. We construct a reference binary model in which a 2.21M⊙ star loses its hydrogen-rich envelope through non-conservative mass transfer to the 1.76M⊙ companion star, creating a 0.38M⊙ subdwarf. We find the tightest stable orbital separation for circumbinary planets to be ≃2.5 times the binary separation after mass transfer. Accounting for tides by using the interior stellar structure, we find that tidal effects become apparent after the rapid mass transfer phase and start to fade away during the latter stage of the slow mass transfer phase. Our research provides a new framework for exploring circumbinary planet dynamics in interacting binary systems."}],"quality_controlled":"1","volume":537,"intvolume":"       537","isi":1,"ec_funded":1,"author":[{"last_name":"Xing","full_name":"Xing, Zepei","first_name":"Zepei"},{"full_name":"Torres Rodriguez, Santiago","last_name":"Torres Rodriguez","first_name":"Santiago","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","orcid":"0000-0002-3150-8988"},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter"},{"first_name":"Alessandro A.","full_name":"Trani, Alessandro A.","last_name":"Trani"},{"first_name":"Valeriya","last_name":"Korol","full_name":"Korol, Valeriya"},{"first_name":"Jorge","full_name":"Cuadra, Jorge","last_name":"Cuadra"}],"scopus_import":"1","file_date_updated":"2025-12-30T07:24:34Z","publication":"Monthly Notices of the Royal Astronomical Society","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"acknowledgement":"We thank the participants of the 2023 Kavli Summer Program in Astrophysics, hosted by the Max Planck Institute for Astrophysics and funded by the Kavli Foundation. In particular, Holly Preece, Selma de Mink, and Stephen Justham for their feedback and comments on our work. ZX acknowledges support from the China Scholarship Council (CSC). ST acknowledges the funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101034413. AAT acknowledges support from the Horizon Europe research and innovation programmes under the Marie Skłodowska-Curie grant agreement no. 101103134.","file":[{"success":1,"access_level":"open_access","relation":"main_file","file_size":2974244,"file_name":"2025_MonthlyNoticesRAS_Xing.pdf","creator":"dernst","date_created":"2025-12-30T07:24:34Z","file_id":"20881","date_updated":"2025-12-30T07:24:34Z","checksum":"49fb4fe69f487d36169ccea60acbeccc","content_type":"application/pdf"}],"DOAJ_listed":"1","article_type":"original","OA_type":"gold","OA_place":"publisher","doi":"10.1093/mnras/stae2820","ddc":["520"],"arxiv":1,"PlanS_conform":"1","citation":{"mla":"Xing, Zepei, et al. “Combining REBOUND and MESA: Dynamical Evolution of Planets Orbiting Interacting Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 1, Oxford University Press, 2025, pp. 285–92, doi:<a href=\"https://doi.org/10.1093/mnras/stae2820\">10.1093/mnras/stae2820</a>.","short":"Z. Xing, S. Torres Rodriguez, Y.L.L. Götberg, A.A. Trani, V. Korol, J. Cuadra, Monthly Notices of the Royal Astronomical Society 537 (2025) 285–292.","ieee":"Z. Xing, S. Torres Rodriguez, Y. L. L. Götberg, A. A. Trani, V. Korol, and J. Cuadra, “Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 1. Oxford University Press, pp. 285–292, 2025.","apa":"Xing, Z., Torres Rodriguez, S., Götberg, Y. L. L., Trani, A. A., Korol, V., &#38; Cuadra, J. (2025). Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2820\">https://doi.org/10.1093/mnras/stae2820</a>","ama":"Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(1):285-292. doi:<a href=\"https://doi.org/10.1093/mnras/stae2820\">10.1093/mnras/stae2820</a>","ista":"Xing Z, Torres Rodriguez S, Götberg YLL, Trani AA, Korol V, Cuadra J. 2025. Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries. Monthly Notices of the Royal Astronomical Society. 537(1), 285–292.","chicago":"Xing, Zepei, Santiago Torres Rodriguez, Ylva Louise Linsdotter Götberg, Alessandro A. Trani, Valeriya Korol, and Jorge Cuadra. “Combining REBOUND and MESA: Dynamical Evolution of Planets Orbiting Interacting Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/stae2820\">https://doi.org/10.1093/mnras/stae2820</a>."},"article_processing_charge":"Yes","month":"02","title":"Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries","_id":"18984","page":"285-292","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2025-12-30T07:25:37Z","year":"2025","oa_version":"Published Version","date_published":"2025-02-01T00:00:00Z","has_accepted_license":"1","project":[{"call_identifier":"H2020","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","grant_number":"101034413"}],"issue":"1","type":"journal_article","day":"01","publisher":"Oxford University Press","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public"},{"year":"2025","oa_version":"Published Version","date_updated":"2026-02-16T11:51:48Z","date_published":"2025-03-01T00:00:00Z","has_accepted_license":"1","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"page":"2535-2558","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","publisher":"Oxford University Press","day":"01","type":"journal_article","issue":"3","arxiv":1,"ddc":["520"],"doi":"10.1093/mnras/staf058","OA_place":"publisher","article_type":"original","OA_type":"gold","title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","month":"03","_id":"19066","citation":{"ista":"Claeyssens A, Adamo A, Messa M, Dessauges-Zavadsky M, Richard J, Kramarenko I, Matthee JJ, Naidu RP. 2025. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. 537(3), 2535–2558.","chicago":"Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky, Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>.","apa":"Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J., Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf058\">https://doi.org/10.1093/mnras/staf058</a>","ama":"Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(3):2535-2558. doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>","ieee":"A. Claeyssens <i>et al.</i>, “Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3. Oxford University Press, pp. 2535–2558, 2025.","short":"A. Claeyssens, A. Adamo, M. Messa, M. Dessauges-Zavadsky, J. Richard, I. Kramarenko, J.J. Matthee, R.P. Naidu, Monthly Notices of the Royal Astronomical Society 537 (2025) 2535–2558.","mla":"Claeyssens, Adélaïde, et al. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:<a href=\"https://doi.org/10.1093/mnras/staf058\">10.1093/mnras/staf058</a>."},"article_processing_charge":"No","intvolume":"       537","isi":1,"publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2025-02-25T06:38:43Z","scopus_import":"1","author":[{"full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens","first_name":"Adélaïde"},{"first_name":"Angela","full_name":"Adamo, Angela","last_name":"Adamo"},{"first_name":"Matteo","last_name":"Messa","full_name":"Messa, Matteo"},{"first_name":"Miroslava","last_name":"Dessauges-Zavadsky","full_name":"Dessauges-Zavadsky, Miroslava"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"DOAJ_listed":"1","file":[{"success":1,"access_level":"open_access","relation":"main_file","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf","creator":"dernst","date_created":"2025-02-25T06:38:43Z","file_id":"19084","file_size":35099276,"checksum":"431aef05755e6b5472f5e9b4c326cf84","content_type":"application/pdf","date_updated":"2025-02-25T06:38:43Z"}],"acknowledgement":"The authors thank the International Space Science Institute for sponsoring the ISSI team: ‘Star Formation within rapidly evolving galaxies’ where many ideas discussed in this article have been brainstormed. AA and AC acknowledge support by the Swedish research council Vetenskapsrådet (2021-05559). MM acknowledges the financial support through grant PRIN-MIUR 2020SKSTHZ. JM and IK acknowledge support by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. RPN acknowledges funding from JWST programme GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","publication_status":"published","language":[{"iso":"eng"}],"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"external_id":{"arxiv":["2410.10974"],"isi":["001420026000001"]},"date_created":"2025-02-23T23:01:55Z","quality_controlled":"1","volume":537,"abstract":[{"lang":"eng","text":"We present a sample of 1956 individual stellar clumps at redshift 0.7 < z < 10, detected with JWST/NIRCam in 476 galaxies lensed by the galaxy cluster Abell2744. The lensed clumps present magnifications ranging between μ = 1.8 and μ = 300. We perform simultaneous size-photometry estimates in 20 JWST/NIRCam median and broad-band filters from 0.7 to 5 μm.\r\nSpectral energy distribution (SED) fitting analyses enable us to recover the physical properties of the clumps. The majority of the clumps are spatially resolved and have effective radii in the range Reff = 10–700 pc. We restrict this first study to the 1751 post-reionization era clumps with redshift < 5.5. We find a significant evolution of the average clump ages, star formation rates (SFRs), SFR surface densities, and metallicity with increasing redshift, while median stellar mass and stellar mass surface densities are similar in the probed redshift range. We observe a strong correlation between the clump properties and the properties of their host galaxies, with more massive galaxies hosting more massive and older clumps. We find that clumps closer to their host galactic centre are on average more massive, while their ages do not show clear sign of migration. We find that clumps at cosmic noon sample the upper-mass end of the mass function to higher masses than at z > 3, reflecting the rapid increase towards the peak of the cosmic star formation history. We conclude that the results achieved over the studied redshift range are in agreement with expectation of in situ clump formation scenario from large-scale disc fragmentation. "}]},{"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"full_name":"Herard-Demanche, Thomas","last_name":"Herard-Demanche","first_name":"Thomas"},{"full_name":"Bouwens, Rychard J","last_name":"Bouwens","first_name":"Rychard J"},{"first_name":"Pascal A","last_name":"Oesch","full_name":"Oesch, Pascal A"},{"full_name":"Naidu, Rohan P","last_name":"Naidu","first_name":"Rohan P"},{"full_name":"Decarli, Roberto","last_name":"Decarli","first_name":"Roberto"},{"full_name":"Nelson, Erica J","last_name":"Nelson","first_name":"Erica J"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"first_name":"Andrea","full_name":"Weibel, Andrea","last_name":"Weibel"},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"},{"full_name":"Stefanon, Mauro","last_name":"Stefanon","first_name":"Mauro"},{"last_name":"Walter","full_name":"Walter, Fabian","first_name":"Fabian"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Romain A","full_name":"Meyer, Romain A","last_name":"Meyer"},{"full_name":"Wuyts, Stijn","last_name":"Wuyts","first_name":"Stijn"},{"first_name":"Naveen","full_name":"Reddy, Naveen","last_name":"Reddy"},{"full_name":"Rowland, Lucie","last_name":"Rowland","first_name":"Lucie"},{"first_name":"Ivana","last_name":"van Leeuwen","full_name":"van Leeuwen, Ivana"},{"first_name":"Pablo Arrabal","last_name":"Haro","full_name":"Haro, Pablo Arrabal"},{"last_name":"Dannerbauer","full_name":"Dannerbauer, Helmut","first_name":"Helmut"},{"first_name":"Alice E","last_name":"Shapley","full_name":"Shapley, Alice E"},{"last_name":"Chisholm","full_name":"Chisholm, John","first_name":"John"},{"first_name":"Pieter","last_name":"van Dokkum","full_name":"van Dokkum, Pieter"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"full_name":"Illingworth, Garth","last_name":"Illingworth","first_name":"Garth"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Irene","full_name":"Shivaei, Irene","last_name":"Shivaei"}],"file_date_updated":"2026-02-09T08:39:19Z","intvolume":"       537","acknowledgement":"We are grateful to Roberto Neri and collaborators for providing us with spatially resolved information on both the dust-continuum and [C ii] line emission from their high spatial resolution PdBI observations. This project was made possible in part by the Leiden University Fund/Bouwens Astrophysics Fund. RJB acknowledges support from NWO grants 600.065.140.11N211 (vrij competitie) and TOP grant TOP1.16.057. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. Support for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. RPN acknowledges funding from JWST programs GO-1933 and GO-2279. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the CIDEGENT/2021/059 grant, from project PID2019-109592GB-I00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación. This study forms part of the Astrophysics and High Energy Physics programme and was supported by MCIN with funding from European Union NextGenerationEU (PRTR-C17.I1) and by Generalitat Valenciana under the project n. ASFAE/2022/025. RAM acknowledges support from the ERC Advanced Grant 740246 (Cosmic_Gas) and the Swiss National Science Foundation through project grant 200020_207349.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–03127 for JWST. These observations are associated with program no. 1895.\r\n\r\nThis paper made use of several publicly available software packages. We are indebted to the respective authors for their work: ipython (Pérez & Granger 2007), matplotlib (Hunter 2007), numpy (Oliphant 2006), scipy (Virtanen et al. 2020), jupyter (Kluyver et al. 2016), astropy (Astropy Collaboration 2013, 2018), grizli (v1.7.11; Brammer 2018; Brammer et al. 2022), eazy (Brammer, van Dokkum & Coppi 2008), and SExtractor (Bertin & Arnouts 1996).","DOAJ_listed":"1","file":[{"file_size":2787493,"creator":"dernst","file_name":"2025_MonthlyNoticesRAS_HerardDemanche.pdf","date_created":"2026-02-09T08:39:19Z","file_id":"21169","date_updated":"2026-02-09T08:39:19Z","content_type":"application/pdf","checksum":"4cbade43244eaa8b60bb05a90ae613da","success":1,"access_level":"open_access","relation":"main_file"}],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","external_id":{"arxiv":["2309.04525"]},"department":[{"_id":"JoMa"}],"date_created":"2026-01-28T15:25:53Z","language":[{"iso":"eng"}],"volume":537,"quality_controlled":"1","abstract":[{"text":"We report the detection of a 13σ Hα emission line from HDF850.1 at z = 5.188 ± 0.001 using the FRESCO (First Reionization Era SpectroscopicallyComplete Observations) NIRCam F444W grism observations. Detection of Hα in HDF850.1 is noteworthy, given its high far-infrared (IR) luminosity, substantial dust obscuration, and the historical challenges in deriving its redshift.\r\nHDF850.1 shows a clear detection in the F444W imaging data, distributed between a northern and southern component, mirroring that seen in [C II] from the Plateau de Bure Interferometer. Modelling the spectral energy distribution of each component separately, we find that the northern component has a higher mass, star formation rate (SFR), and dust extinction than the southern component. The observed Hα emission appears to arise entirely from the less-obscured southern component and shows a similar \u0004v∼ + 130 km s −1 velocity offset to that seen for [C II] relative to the source systemic redshift. Leveraging Hα-derived redshiftsfrom FRESCO observations, we find that HDF850.1 isforming in one of the richest environments identified to date at z > 5, with 100 z = 5.17–5.20 galaxies distributed across 13 smaller structures and a ∼(15 cMpc)3 volume. Based on the evolution of analogous structures in cosmological simulations, the z = 5.17–5.20 structures seem likely to collapse into\r\na single > 1014M cluster by z ∼ 0. Comparing galaxy properties forming within this overdensity with those outside, we find the masses, SFRs, and UV luminosities inside the overdensity to be clearly higher. The prominence of Hα line emission from HDF850.1 and other known highly obscured z > 5 galaxies illustrates the potential of NIRCam-grism programs to map both\r\nthe early build-up of IR-luminous galaxies and overdense structures.","lang":"eng"}],"date_published":"2025-02-01T00:00:00Z","has_accepted_license":"1","oa_version":"Published Version","year":"2025","date_updated":"2026-02-09T08:50:55Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"788-808","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"type":"journal_article","publisher":"Oxford University Press","day":"01","issue":"2","arxiv":1,"ddc":["520"],"doi":"10.1093/mnras/staf030","OA_place":"publisher","OA_type":"gold","article_type":"original","_id":"21063","title":"Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures","month":"02","article_processing_charge":"Yes","citation":{"ieee":"T. Herard-Demanche <i>et al.</i>, “Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 2. Oxford University Press, pp. 788–808, 2025.","short":"T. Herard-Demanche, R.J. Bouwens, P.A. Oesch, R.P. Naidu, R. Decarli, E.J. Nelson, G. Brammer, A. Weibel, M. Xiao, M. Stefanon, F. Walter, J.J. Matthee, R.A. Meyer, S. Wuyts, N. Reddy, L. Rowland, I. van Leeuwen, P.A. Haro, H. Dannerbauer, A.E. Shapley, J. Chisholm, P. van Dokkum, I. Labbe, G. Illingworth, D. Schaerer, I. Shivaei, Monthly Notices of the Royal Astronomical Society 537 (2025) 788–808.","mla":"Herard-Demanche, Thomas, et al. “Mapping Dusty Galaxy Growth at z &#62; 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 2, Oxford University Press, 2025, pp. 788–808, doi:<a href=\"https://doi.org/10.1093/mnras/staf030\">10.1093/mnras/staf030</a>.","ista":"Herard-Demanche T, Bouwens RJ, Oesch PA, Naidu RP, Decarli R, Nelson EJ, Brammer G, Weibel A, Xiao M, Stefanon M, Walter F, Matthee JJ, Meyer RA, Wuyts S, Reddy N, Rowland L, van Leeuwen I, Haro PA, Dannerbauer H, Shapley AE, Chisholm J, van Dokkum P, Labbe I, Illingworth G, Schaerer D, Shivaei I. 2025. Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. 537(2), 788–808.","chicago":"Herard-Demanche, Thomas, Rychard J Bouwens, Pascal A Oesch, Rohan P Naidu, Roberto Decarli, Erica J Nelson, Gabriel Brammer, et al. “Mapping Dusty Galaxy Growth at z &#62; 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf030\">https://doi.org/10.1093/mnras/staf030</a>.","apa":"Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., Naidu, R. P., Decarli, R., Nelson, E. J., … Shivaei, I. (2025). Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf030\">https://doi.org/10.1093/mnras/staf030</a>","ama":"Herard-Demanche T, Bouwens RJ, Oesch PA, et al. Mapping dusty galaxy growth at z &#62; 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(2):788-808. doi:<a href=\"https://doi.org/10.1093/mnras/staf030\">10.1093/mnras/staf030</a>"},"PlanS_conform":"1"},{"file":[{"date_updated":"2026-02-10T07:07:17Z","content_type":"application/pdf","checksum":"f9b4c6a606df9493f6eb6af5ebcca6db","file_size":3689696,"file_id":"21203","date_created":"2026-02-10T07:07:17Z","file_name":"2025_MonthlyNoticesRAS_Krauth.pdf","creator":"dernst","relation":"main_file","access_level":"open_access","success":1}],"acknowledgement":"We acknowledge support from the Nationale Wetenschapsagenda Roadmap grant ‘Gravitational Waves Laser Interferometer Space Antenna/Einstein Telescope: Shivers from the Deep Universe: A National Infrastructure for Gravitational Wave Research’ (LMK), National Science Foundation grant AST-2006176 (ZH), and National Aeronautics and Space Administration Astrophysics Theory Program grant 80NSSC22K0822 (AM and ZH). JD was supported by National Aeronautics and Space Administration through the National Aeronautics and Space Administration Hubble Fellowship grant HST-HF2-51552.001A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under National Aeronautics and Space Administration contract NAS5-26555. This research was supported in part by the National Science Foundation under grant no. NSF PHY-1748958. This research has made use of National Aeronautics and Space Administration’s Astrophysics Data System. Resources supporting this work were provided by the National Aeronautics and Space Administration High-End Computing (HEC) Program through the National Aeronautics and Space Administration Advanced Supercomputing (NAS) Division at Ames Research Center. Software:  python (Oliphant 2007; Millman & Aivazis 2011), scipy (Jones et al. 2001), numpy (van der Walt, Colbert & Varoquaux 2011), and matplotlib (Hunter 2007).","DOAJ_listed":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"full_name":"Krauth, Luke Major","last_name":"Krauth","first_name":"Luke Major"},{"first_name":"Jordy","last_name":"Davelaar","full_name":"Davelaar, Jordy"},{"orcid":"0000-0003-3633-5403","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"John Ryan","full_name":"Westernacher-Schneider, John Ryan","last_name":"Westernacher-Schneider"},{"first_name":"Jonathan","full_name":"Zrake, Jonathan","last_name":"Zrake"},{"first_name":"Andrew","last_name":"MacFadyen","full_name":"MacFadyen, Andrew"}],"file_date_updated":"2026-02-10T07:07:17Z","intvolume":"       543","volume":543,"quality_controlled":"1","abstract":[{"text":"The multimessenger combination of gravitational waves (GWs) from merging massive black hole binaries (MBHBs) and the electromagnetic (EM) counterpart from the surrounding circumbinary disc (CBD) will open avenues to new scientific pursuits. In order to realize this science, we need to correctly localize the host galaxy of the merging MBHB. Multiwavelength, time-dependent EM signatures can greatly facilitate the identification of the unique EM counterpart among many sources in LISA’s localization volume. To this end, we studied merging unequal-mass MBHBs embedded in a CBD using high-resolution 2D simulations, with a $\\Gamma$-law equation of state, incorporating viscous heating, shock heating, and radiative cooling. We simulate each binary starting from before it decouples from the CBD until just after the merger. We compute EM signatures and identify distinct features before, during, and after the merger. We corroborate previous findings of a several orders of magnitude drop in the thermal X-ray luminosity near the time of merger, but with delayed timing compared to an equal-mass system. The source remains X-ray dark for hours post-merger. Our main results are a potential new signature of a sharp spike in the thermal X-ray emission just before the tell-tale steep drop occurs. This feature may further help to identify EM counterparts of LISA’s unequal MBHBs before merger without the need for extensive pre-merger monitoring. Additionally, we find a role-reversal in which the primary out-accretes the secondary during late inspiral, which may diminish signatures originating from Doppler modulation.","lang":"eng"}],"publication_status":"published","date_created":"2026-01-31T09:28:28Z","external_id":{"arxiv":["2503.01494"]},"department":[{"_id":"ZoHa"}],"language":[{"iso":"eng"}],"status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"issue":"3","type":"journal_article","day":"01","publisher":"Oxford University Press","date_published":"2025-11-01T00:00:00Z","has_accepted_license":"1","date_updated":"2026-02-10T07:10:21Z","oa_version":"Published Version","year":"2025","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"2670-2685","_id":"21122","month":"11","title":"Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers","article_processing_charge":"Yes","PlanS_conform":"1","citation":{"apa":"Krauth, L. M., Davelaar, J., Haiman, Z., Westernacher-Schneider, J. R., Zrake, J., &#38; MacFadyen, A. (2025). Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1583\">https://doi.org/10.1093/mnras/staf1583</a>","ama":"Krauth LM, Davelaar J, Haiman Z, Westernacher-Schneider JR, Zrake J, MacFadyen A. Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;543(3):2670-2685. doi:<a href=\"https://doi.org/10.1093/mnras/staf1583\">10.1093/mnras/staf1583</a>","ista":"Krauth LM, Davelaar J, Haiman Z, Westernacher-Schneider JR, Zrake J, MacFadyen A. 2025. Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers. Monthly Notices of the Royal Astronomical Society. 543(3), 2670–2685.","chicago":"Krauth, Luke Major, Jordy Davelaar, Zoltán Haiman, John Ryan Westernacher-Schneider, Jonathan Zrake, and Andrew MacFadyen. “Thermal X-Ray Signatures in Late-Stage Unequal-Mass Massive Black Hole Binary Mergers.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1583\">https://doi.org/10.1093/mnras/staf1583</a>.","short":"L.M. Krauth, J. Davelaar, Z. Haiman, J.R. Westernacher-Schneider, J. Zrake, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 543 (2025) 2670–2685.","mla":"Krauth, Luke Major, et al. “Thermal X-Ray Signatures in Late-Stage Unequal-Mass Massive Black Hole Binary Mergers.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3, Oxford University Press, 2025, pp. 2670–85, doi:<a href=\"https://doi.org/10.1093/mnras/staf1583\">10.1093/mnras/staf1583</a>.","ieee":"L. M. Krauth, J. Davelaar, Z. Haiman, J. R. Westernacher-Schneider, J. Zrake, and A. MacFadyen, “Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3. Oxford University Press, pp. 2670–2685, 2025."},"ddc":["520"],"arxiv":1,"article_type":"original","OA_type":"gold","OA_place":"publisher","doi":"10.1093/mnras/staf1583"},{"_id":"21127","month":"03","title":"Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation","article_processing_charge":"Yes","PlanS_conform":"1","citation":{"apa":"Su, K.-Y., Bryan, G. L., &#38; Haiman, Z. (2025). Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf228\">https://doi.org/10.1093/mnras/staf228</a>","ama":"Su K-Y, Bryan GL, Haiman Z. Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;538(1):11-30. doi:<a href=\"https://doi.org/10.1093/mnras/staf228\">10.1093/mnras/staf228</a>","ista":"Su K-Y, Bryan GL, Haiman Z. 2025. Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation. Monthly Notices of the Royal Astronomical Society. 538(1), 11–30.","chicago":"Su, Kung-Yi, Greg L Bryan, and Zoltán Haiman. “Self-Regulation of High-Redshift Black Hole Accretion via Jets: Challenges for SMBH Formation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf228\">https://doi.org/10.1093/mnras/staf228</a>.","short":"K.-Y. Su, G.L. Bryan, Z. Haiman, Monthly Notices of the Royal Astronomical Society 538 (2025) 11–30.","mla":"Su, Kung-Yi, et al. “Self-Regulation of High-Redshift Black Hole Accretion via Jets: Challenges for SMBH Formation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 538, no. 1, Oxford University Press, 2025, pp. 11–30, doi:<a href=\"https://doi.org/10.1093/mnras/staf228\">10.1093/mnras/staf228</a>.","ieee":"K.-Y. Su, G. L. Bryan, and Z. Haiman, “Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 538, no. 1. Oxford University Press, pp. 11–30, 2025."},"ddc":["520"],"arxiv":1,"OA_type":"gold","article_type":"original","doi":"10.1093/mnras/staf228","OA_place":"publisher","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"issue":"1","type":"journal_article","publisher":"Oxford University Press","day":"01","has_accepted_license":"1","date_published":"2025-03-01T00:00:00Z","date_updated":"2026-02-10T08:36:54Z","year":"2025","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"11-30","extern":"1","volume":538,"quality_controlled":"1","abstract":[{"lang":"eng","text":"The early growth of black holes (BHs) in atomic-cooling haloes is likely influenced by feedback on the surrounding gas. While the effects of radiative feedback are well-documented, mechanical feedback, particularly from active galactic nucleus (AGN) jets, has been comparatively less explored. Building on our previous work that examined the growth of a 100 M BH in a constant density environment regulated by AGN jets, we expand the initial BH mass range from 1 to 104 M and adopt a more realistic density profile for atomic-cooling haloes. We reaffirm the validity of our analytic models for jet cocoon propagation and feedback regulation. We identify several critical radii – namely, the terminal radius of jet cocoon propagation, the isotropization radius of the jet cocoon, and the core radius of the atomic-cooling halo – that are crucial in determining BH growth given specific gas properties and jet feedback parameters. In a significant portion of the parameter space, our findings show that jet feedback substantially disrupts the halo’s core during the initial feedback episode, preventing BH growth beyond 104 M.\r\nConversely, conditions characterized by low jet velocities and high gas densities enable sustained BH growth over extended periods. We provide a prediction for the BH mass growth as a function of time and feedback parameters. We found that, to form a supermassive BH (> 106 M) within 1 Gyr entirely by accreting gas from an atomic-cooling halo, the jet energy feedback\r\nefficiency must be  10−4M˙ BHc2 even if the seed BH mass is 104 M."}],"publication_status":"published","date_created":"2026-01-31T09:29:59Z","external_id":{"arxiv":["2409.12250"]},"language":[{"iso":"eng"}],"DOAJ_listed":"1","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staf228","open_access":"1"}],"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"first_name":"Kung-Yi","last_name":"Su","full_name":"Su, Kung-Yi"},{"first_name":"Greg L","last_name":"Bryan","full_name":"Bryan, Greg L"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"}],"intvolume":"       538"},{"_id":"21128","title":"Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes","month":"03","article_processing_charge":"Yes","citation":{"ista":"Epstein-Martin M, Tagawa H, Haiman Z, Perna R. 2025. Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes. Monthly Notices of the Royal Astronomical Society. 537(4), 3396–3420.","chicago":"Epstein-Martin, Marguerite, Hiromichi Tagawa, Zoltán Haiman, and Rosalba Perna. “Time-Dependent Models of AGN Discs with Radiation from Embedded Stellar-Mass Black Holes.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf237\">https://doi.org/10.1093/mnras/staf237</a>.","apa":"Epstein-Martin, M., Tagawa, H., Haiman, Z., &#38; Perna, R. (2025). Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf237\">https://doi.org/10.1093/mnras/staf237</a>","ama":"Epstein-Martin M, Tagawa H, Haiman Z, Perna R. Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;537(4):3396-3420. doi:<a href=\"https://doi.org/10.1093/mnras/staf237\">10.1093/mnras/staf237</a>","ieee":"M. Epstein-Martin, H. Tagawa, Z. Haiman, and R. Perna, “Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 4. Oxford University Press, pp. 3396–3420, 2025.","short":"M. Epstein-Martin, H. Tagawa, Z. Haiman, R. Perna, Monthly Notices of the Royal Astronomical Society 537 (2025) 3396–3420.","mla":"Epstein-Martin, Marguerite, et al. “Time-Dependent Models of AGN Discs with Radiation from Embedded Stellar-Mass Black Holes.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 537, no. 4, Oxford University Press, 2025, pp. 3396–420, doi:<a href=\"https://doi.org/10.1093/mnras/staf237\">10.1093/mnras/staf237</a>."},"PlanS_conform":"1","arxiv":1,"ddc":["520"],"OA_place":"publisher","doi":"10.1093/mnras/staf237","OA_type":"gold","article_type":"original","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"publisher":"Oxford University Press","day":"01","type":"journal_article","issue":"4","has_accepted_license":"1","date_published":"2025-03-01T00:00:00Z","year":"2025","oa_version":"Published Version","date_updated":"2026-02-10T09:00:44Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","page":"3396-3420","volume":537,"quality_controlled":"1","abstract":[{"text":"The brightest steady sources of radiation in the universe, active galactic nuclei (AGNs), are powered by gas accretion on to a central supermassive black hole (SMBH). The large sizes and accretion rates implicated in AGN accretion discs are expected to lead to gravitational instability and fragmentation, effectively cutting off mass inflow to the SMBH. Radiative feedback from disc-embedded stars has been invoked to yield marginally stable, steady-state solutions in the outer discs. Here, we examine the consequences of this star formation with a semi-analytical model in which stellar-mass black hole (sBH) remnants in the disc provide an additional source of stabilizing radiative feedback. Assuming star formation seeds the embedded sBH population, we model the time-evolving feedback from both stars and the growing population of accreting sBHs. We find that in the outer disc, the luminosity of the sBHs quickly dominates that of their parent stars. However, because sBHs consume less gas than stars to stabilize the disc, the presence of the sBHs enhances the mass flux to the inner disc. As a result, star formation persists over the lifetime of the AGN, damped in the outer disc, but amplified in a narrow ring in the inner disc. Heating from the embedded sBHs significantly modifies the disc’s temperature profile and hardens its spectral energy distribution, and direct emission from the sBHs adds a new hard X-ray component.","lang":"eng"}],"publication_status":"published","external_id":{"arxiv":["2405.09380"]},"date_created":"2026-01-31T09:30:19Z","language":[{"iso":"eng"}],"DOAJ_listed":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staf237"}],"author":[{"first_name":"Marguerite","full_name":"Epstein-Martin, Marguerite","last_name":"Epstein-Martin"},{"first_name":"Hiromichi","last_name":"Tagawa","full_name":"Tagawa, Hiromichi"},{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Perna, Rosalba","last_name":"Perna","first_name":"Rosalba"}],"publication":"Monthly Notices of the Royal Astronomical Society","intvolume":"       537"},{"ddc":["520"],"arxiv":1,"OA_type":"gold","article_type":"original","doi":"10.1093/mnras/stae2053","OA_place":"publisher","_id":"18172","month":"10","title":"Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants","article_processing_charge":"Yes","PlanS_conform":"1","citation":{"mla":"Hatt, Emily J., et al. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2, Oxford University Press, 2024, pp. 1060–76, doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>.","short":"E.J. Hatt, J.M.J. Ong, M.B. Nielsen, W.J. Chaplin, G.R. Davies, S. Deheuvels, J. Ballot, G. Li, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 534 (2024) 1060–1076.","ieee":"E. J. Hatt <i>et al.</i>, “Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2. Oxford University Press, pp. 1060–1076, 2024.","apa":"Hatt, E. J., Ong, J. M. J., Nielsen, M. B., Chaplin, W. J., Davies, G. R., Deheuvels, S., … Bugnet, L. A. (2024). Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>","ama":"Hatt EJ, Ong JMJ, Nielsen MB, et al. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;534(2):1060-1076. doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>","ista":"Hatt EJ, Ong JMJ, Nielsen MB, Chaplin WJ, Davies GR, Deheuvels S, Ballot J, Li G, Bugnet LA. 2024. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. Monthly Notices of the Royal Astronomical Society. 534(2), 1060–1076.","chicago":"Hatt, Emily J., J. M.Joel Ong, Martin B. Nielsen, William J. Chaplin, Guy R. Davies, Sébastien Deheuvels, Jérôme Ballot, Gang Li, and Lisa Annabelle Bugnet. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>."},"has_accepted_license":"1","date_published":"2024-10-01T00:00:00Z","date_updated":"2025-09-08T09:53:01Z","oa_version":"Published Version","year":"2024","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"1060-1076","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"issue":"2","day":"01","publisher":"Oxford University Press","type":"journal_article","publication_status":"published","date_created":"2024-10-06T22:01:11Z","department":[{"_id":"LiBu"}],"external_id":{"arxiv":["2409.01157"],"isi":["001320536900011"]},"language":[{"iso":"eng"}],"volume":534,"quality_controlled":"1","abstract":[{"lang":"eng","text":"Red Giant stars host solar-like oscillations which have mixed character, being sensitive to conditions both in the outer convection zone and deep within the interior. The properties of these modes are sensitive to both core rotation and magnetic fields. While asteroseismic studies of the former have been done on a large scale, studies of the latter are currently limited to tens of stars. We aim to produce the first large catalogue of both magnetic and rotational perturbations. We jointly constrain these parameters by devising an automated method for fitting the power spectra directly. We successfully apply the method to 302 low-luminosity red giants. We find a clear bimodality in core rotation rate. The primary peak is at δνrot = 0.32 μHz, and the secondary at δνrot = 0.47 μHz. Combining our results with literature values, we find that the percentage of stars rotating much more rapidly than the population average increases with evolutionary state. We measure magnetic splittings of 2σ significance in 23 stars. While the most extreme magnetic splitting values appear in stars with masses > 1.1M⊙, implying they formerly hosted a convective core, a small but statistically significant magnetic splitting is measured at lower masses. Asymmetry between the frequencies of a rotationally split multiplet has previously been used to diagnose the presence of a magnetic perturbation. We find that of the stars with a significant detection of magnetic perturbation, 43\\% do not show strong asymmetry. We find no strong evidence of correlation between the rotation and magnetic parameters."}],"scopus_import":"1","author":[{"first_name":"Emily J.","full_name":"Hatt, Emily J.","last_name":"Hatt"},{"first_name":"J. M.Joel","full_name":"Ong, J. M.Joel","last_name":"Ong"},{"last_name":"Nielsen","full_name":"Nielsen, Martin B.","first_name":"Martin B."},{"first_name":"William J.","full_name":"Chaplin, William J.","last_name":"Chaplin"},{"full_name":"Davies, Guy R.","last_name":"Davies","first_name":"Guy R."},{"full_name":"Deheuvels, Sébastien","last_name":"Deheuvels","first_name":"Sébastien"},{"first_name":"Jérôme","full_name":"Ballot, Jérôme","last_name":"Ballot"},{"first_name":"Gang","last_name":"Li","full_name":"Li, Gang"},{"full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000"}],"file_date_updated":"2024-10-07T09:14:03Z","publication":"Monthly Notices of the Royal Astronomical Society","intvolume":"       534","isi":1,"file":[{"access_level":"open_access","relation":"main_file","success":1,"content_type":"application/pdf","checksum":"b79f3c6a5991516abbcc8d34fa4bfb5f","date_updated":"2024-10-07T09:14:03Z","file_name":"2024_MonthlyNRoyalAstronSoc_Hatt.pdf","creator":"dernst","file_id":"18182","date_created":"2024-10-07T09:14:03Z","file_size":2813008}],"acknowledgement":"EJH, WJC, and GRD acknowledge the support of Science and Technology Facilities Council. MBN acknowledges support from the UK Space Agency. JMJO acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001, awarded by STScI (Space Telescope Science Institute), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The authors acknowledge use of the Blue-BEAR HPC service at the University of Birmingham. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission was provided by the NASA Science Mission Directorate. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/web/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC was provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (CartographY GA. 804752). SD and JB acknowledge support from the Centre National d’Etudes Spatiales (CNES).","DOAJ_listed":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1},{"citation":{"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.","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>.","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.","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>","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>","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>.","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."},"article_processing_charge":"Yes","title":"A unified model for the clustering of quasars and galaxies at z ≈ 6","month":"11","_id":"18523","OA_place":"publisher","doi":"10.1093/mnras/stae2307","article_type":"original","OA_type":"gold","ddc":["520"],"day":"01","publisher":"Oxford University Press","type":"journal_article","issue":"4","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","page":"3155-3175","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","year":"2024","oa_version":"Published Version","date_updated":"2025-09-08T14:40:22Z","has_accepted_license":"1","date_published":"2024-11-01T00:00:00Z","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."}],"quality_controlled":"1","volume":534,"language":[{"iso":"eng"}],"external_id":{"isi":["001335663900008"]},"department":[{"_id":"JoMa"}],"date_created":"2024-11-10T23:01:58Z","publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"DOAJ_listed":"1","file":[{"file_name":"2024_MonthlyNRoyalAstronSoc_Pizzati.pdf","creator":"dernst","file_id":"18542","date_created":"2024-11-12T07:17:26Z","file_size":2954312,"checksum":"9ea6285dd1d04d7a9e7b40a4c9e11edb","content_type":"application/pdf","date_updated":"2024-11-12T07:17:26Z","success":1,"access_level":"open_access","relation":"main_file"}],"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.","intvolume":"       534","isi":1,"publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2024-11-12T07:17:26Z","author":[{"full_name":"Pizzati, Elia","last_name":"Pizzati","first_name":"Elia"},{"last_name":"Hennawi","full_name":"Hennawi, Joseph F.","first_name":"Joseph F."},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Matthieu","last_name":"Schaller","full_name":"Schaller, Matthieu"},{"first_name":"Anna Christina","last_name":"Eilers","full_name":"Eilers, Anna Christina"},{"full_name":"Wang, Feige","last_name":"Wang","first_name":"Feige"},{"first_name":"Carlos S.","full_name":"Frenk, Carlos S.","last_name":"Frenk"},{"last_name":"Elbers","full_name":"Elbers, Willem","first_name":"Willem"},{"first_name":"John C.","full_name":"Helly, John C.","last_name":"Helly"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Bordoloi","full_name":"Bordoloi, Rongmon","first_name":"Rongmon"},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Minghao","last_name":"Yue","full_name":"Yue, Minghao"}],"scopus_import":"1"},{"abstract":[{"lang":"eng","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."}],"quality_controlled":"1","volume":535,"language":[{"iso":"eng"}],"external_id":{"isi":["001348009500001"]},"department":[{"_id":"JoMa"}],"date_created":"2024-11-24T23:01:49Z","publication_status":"published","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"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.","DOAJ_listed":"1","file":[{"success":1,"access_level":"open_access","relation":"main_file","file_name":"2024_MonthlyNRoyalAstronSoc_Meyer.pdf","creator":"dernst","file_id":"18613","date_created":"2024-12-03T12:52:13Z","file_size":29476699,"checksum":"efe0ce3580e01459f3be78eb111b35a9","content_type":"application/pdf","date_updated":"2024-12-03T12:52:13Z"}],"isi":1,"intvolume":"       535","author":[{"full_name":"Meyer, R. A.","last_name":"Meyer","first_name":"R. A."},{"first_name":"P. A.","full_name":"Oesch, P. A.","last_name":"Oesch"},{"first_name":"E.","full_name":"Giovinazzo, E.","last_name":"Giovinazzo"},{"first_name":"A.","last_name":"Weibel","full_name":"Weibel, A."},{"full_name":"Brammer, G.","last_name":"Brammer","first_name":"G."},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"first_name":"R. P.","last_name":"Naidu","full_name":"Naidu, R. P."},{"last_name":"Bouwens","full_name":"Bouwens, R. J.","first_name":"R. J."},{"first_name":"J.","full_name":"Chisholm, J.","last_name":"Chisholm"},{"first_name":"A.","last_name":"Covelo-Paz","full_name":"Covelo-Paz, A."},{"first_name":"Y.","full_name":"Fudamoto, Y.","last_name":"Fudamoto"},{"last_name":"Maseda","full_name":"Maseda, M.","first_name":"M."},{"full_name":"Nelson, E.","last_name":"Nelson","first_name":"E."},{"full_name":"Shivaei, I.","last_name":"Shivaei","first_name":"I."},{"first_name":"M.","last_name":"Xiao","full_name":"Xiao, M."},{"first_name":"T.","full_name":"Herard-Demanche, T.","last_name":"Herard-Demanche"},{"first_name":"G. D.","last_name":"Illingworth","full_name":"Illingworth, G. D."},{"first_name":"J.","full_name":"Kerutt, J.","last_name":"Kerutt"},{"full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048"},{"last_name":"Labbe","full_name":"Labbe, I.","first_name":"I."},{"first_name":"E.","full_name":"Leonova, E.","last_name":"Leonova"},{"full_name":"Magee, D.","last_name":"Magee","first_name":"D."},{"first_name":"J.","full_name":"Matharu, J.","last_name":"Matharu"},{"first_name":"G.","full_name":"Prieto Lyon, G.","last_name":"Prieto Lyon"},{"first_name":"N.","full_name":"Reddy, N.","last_name":"Reddy"},{"first_name":"D.","full_name":"Schaerer, D.","last_name":"Schaerer"},{"first_name":"A.","last_name":"Shapley","full_name":"Shapley, A."},{"last_name":"Stefanon","full_name":"Stefanon, M.","first_name":"M."},{"first_name":"M. A.","full_name":"Wozniak, M. A.","last_name":"Wozniak"},{"full_name":"Wuyts, S.","last_name":"Wuyts","first_name":"S."}],"scopus_import":"1","file_date_updated":"2024-12-03T12:52:13Z","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"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.","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>.","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.","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>","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>","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.","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>."},"article_processing_charge":"Yes","title":"JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 < z < 9.0 in the GOODS fields","month":"11","_id":"18585","OA_place":"publisher","doi":"10.1093/mnras/stae2353","article_type":"original","OA_type":"gold","ddc":["520"],"day":"01","type":"journal_article","publisher":"Oxford University Press","issue":"1","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"status":"public","page":"1067-1094","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","year":"2024","date_updated":"2025-09-08T14:47:58Z","has_accepted_license":"1","date_published":"2024-11-01T00:00:00Z"},{"abstract":[{"text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &amp;lt; z &amp;lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization.","lang":"eng"}],"volume":527,"quality_controlled":"1","date_created":"2024-01-22T08:22:17Z","external_id":{"isi":["001133672400004"],"arxiv":["2305.07044"]},"department":[{"_id":"GradSch"},{"_id":"JoMa"}],"language":[{"iso":"eng"}],"corr_author":"1","publication_status":"published","DOAJ_listed":"1","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. 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 number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","file":[{"access_level":"open_access","relation":"main_file","success":1,"date_updated":"2024-01-23T12:30:45Z","checksum":"9d02df4035c4951cf63dee0db1e462e9","content_type":"application/pdf","file_size":4521738,"creator":"dernst","file_name":"2024_MNAstronomSoc_Kramarenko.pdf","file_id":"14879","date_created":"2024-01-23T12:30:45Z"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication":"Monthly Notices of the Royal Astronomical Society","file_date_updated":"2024-01-23T12:30:45Z","author":[{"first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048"},{"full_name":"Kerutt, J","last_name":"Kerutt","first_name":"J"},{"first_name":"A","full_name":"Verhamme, A","last_name":"Verhamme"},{"last_name":"Oesch","full_name":"Oesch, P A","first_name":"P A"},{"first_name":"L","last_name":"Barrufet","full_name":"Barrufet, L"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"full_name":"Kusakabe, H","last_name":"Kusakabe","first_name":"H"},{"first_name":"I","full_name":"Goovaerts, I","last_name":"Goovaerts"},{"first_name":"T T","full_name":"Thai, T T","last_name":"Thai"}],"scopus_import":"1","intvolume":"       527","isi":1,"article_processing_charge":"Yes","citation":{"short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871.","mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>.","ieee":"I. Kramarenko <i>et al.</i>, “Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;527(4):9853-9871. doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>","ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871.","chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>."},"_id":"14852","month":"02","title":"Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape","article_type":"original","doi":"10.1093/mnras/stad3853","ddc":["520"],"arxiv":1,"issue":"4","type":"journal_article","publisher":"Oxford University Press","day":"01","status":"public","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"9853-9871","has_accepted_license":"1","date_published":"2024-02-01T00:00:00Z","date_updated":"2025-09-04T11:51:50Z","year":"2024","oa_version":"Published Version"}]