[{"OA_type":"gold","title":"Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001","issue":"1","ddc":["520"],"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"doi":"10.1093/mnras/stag505","arxiv":1,"date_created":"2026-04-19T22:07:42Z","has_accepted_license":"1","status":"public","type":"journal_article","day":"01","DOAJ_listed":"1","acknowledgement":"This project has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (Grant agreement numbers 101002408). The observationsfrom the FOcal Reducer/low dispersion Spectrograph 2 (FORS2) instrument were collected at the European Southern Observatory (ESO) under ESO programme(s) 113.26ES.001. This work has made use of data from the European Space\r\nAgency (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/conso\r\nrtium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grants No. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and\r\nHumboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University\r\nof Warwick, Ruhr University Bochum, Northwestern University and former partners the University of Washington, Los Alamos National Laboratories, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. This work has made use of data from the Asteroid Terrestrialimpact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African\r\nAstronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile.\r\nThis work makes use of observations from the Las Cumbres Observatory global telescope network. Research at Lick Observatory is partially supported by a generous gift from Google. A major upgrade of the Kast spectrograph on the Shane 3 m telescope at Lick Observatory was made possible through generous gifts from William and Marina Kast as well as the Heising–Simons Foundation. The Isaac Newton Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. Observations reported here were obtained at the Multiple Mirror Telescope (MMT) Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Based on observations collected at Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC).","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_number":"stag505","intvolume":" 548","date_published":"2026-05-01T00:00:00Z","citation":{"chicago":"Elms, Abbigail K., Stefano Bagnulo, Pier Emmanuel Tremblay, Tim Cunningham, James Munday, John Landstreet, Kareem El-Badry, et al. “Detection of a Weak Magnetic Field in the Balmer Emission Line White Dwarf WDJ1653−1001.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag505.","ieee":"A. K. Elms et al., “Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 1. Oxford University Press, 2026.","ama":"Elms AK, Bagnulo S, Tremblay PE, et al. Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. 2026;548(1). doi:10.1093/mnras/stag505","mla":"Elms, Abbigail K., et al. “Detection of a Weak Magnetic Field in the Balmer Emission Line White Dwarf WDJ1653−1001.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 1, stag505, Oxford University Press, 2026, doi:10.1093/mnras/stag505.","apa":"Elms, A. K., Bagnulo, S., Tremblay, P. E., Cunningham, T., Munday, J., Landstreet, J., … Weinberger, A. (2026). Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag505","ista":"Elms AK, Bagnulo S, Tremblay PE, Cunningham T, Munday J, Landstreet J, El-Badry K, Caiazzo I, Melis C, Pinter V, Weinberger A. 2026. Detection of a weak magnetic field in the Balmer emission line white dwarf WDJ1653−1001. Monthly Notices of the Royal Astronomical Society. 548(1), stag505.","short":"A.K. Elms, S. Bagnulo, P.E. Tremblay, T. Cunningham, J. Munday, J. Landstreet, K. El-Badry, I. Caiazzo, C. Melis, V. Pinter, A. Weinberger, Monthly Notices of the Royal Astronomical Society 548 (2026)."},"article_processing_charge":"Yes","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","month":"05","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","date_updated":"2026-05-04T12:11:53Z","file_date_updated":"2026-05-04T12:10:40Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_size":4991495,"date_updated":"2026-05-04T12:10:40Z","content_type":"application/pdf","file_id":"21794","relation":"main_file","file_name":"2026_MNRAS_Elms.pdf","creator":"dernst","success":1,"date_created":"2026-05-04T12:10:40Z","checksum":"75c48d70d10a9a48875f577e04da80bc","access_level":"open_access"}],"publication_status":"published","year":"2026","volume":548,"oa_version":"Published Version","_id":"21745","oa":1,"article_type":"original","abstract":[{"text":"The small DAHe and DAe spectral classes comprise isolated, hydrogen-dominated atmosphere white dwarfs that exhibit variable photometric flux and Balmer line emission. These mysterious systems offer unique insight into the complex interplay between magnetic fields, stellar rotation and atmospheric activity in single white dwarfs. DAHe stars have detectable magnetic fields through Zeeman-split spectral lines, whereas DAe stars lack such splitting. We report the first discovery and characterization of magnetism in the DAe white dwarf WD J165335.21−100116.33 with new time-resolved spectropolarimetry from FORS2. We detect a weak but variable longitudinal magnetic field with values Bz > −9.2 ± 2.4 kG and Bz < −2.2 ± 1.0 kG. Independent ZTF and ATLAS photometry reveal a consistent period of P = 80.3070 ± 0.0007 h. Time-resolved optical spectroscopy obtained with six ground-based instruments demonstrates strong modulation in the strength of the Hα and Hβ Balmer line emission with P = 80.2922 ± 0.0108 h. The photometric flux and Balmer emission strength vary in antiphase, with the strongest magnetic detections coinciding with phases of low photometric flux and strong line emission. These characteristicssupport the theory that a magnetically active, temperature-inverted spot/region is producing an optically thin chromospheric emission region. Comparison with other DAe and DAHe white dwarfsreveals all systems have a strikingly similar antiphase phenomenology, reinforcing the theory that they are subject to a unified physical mechanism. With the detection of a weak magnetic field, we reclassify WD J165335.21−100116.33 as a low-field DAHe white dwarf. ","lang":"eng"}],"author":[{"last_name":"Elms","first_name":"Abbigail K.","full_name":"Elms, Abbigail K."},{"first_name":"Stefano","last_name":"Bagnulo","full_name":"Bagnulo, Stefano"},{"last_name":"Tremblay","first_name":"Pier Emmanuel","full_name":"Tremblay, Pier Emmanuel"},{"first_name":"Tim","last_name":"Cunningham","full_name":"Cunningham, Tim"},{"full_name":"Munday, James","last_name":"Munday","first_name":"James"},{"last_name":"Landstreet","first_name":"John","full_name":"Landstreet, John"},{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"first_name":"Ilaria","last_name":"Caiazzo","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"last_name":"Melis","first_name":"Carl","full_name":"Melis, Carl"},{"full_name":"Pinter, Viktoria","first_name":"Viktoria","last_name":"Pinter"},{"first_name":"Alycia","last_name":"Weinberger","full_name":"Weinberger, Alycia"}],"external_id":{"arxiv":["2603.12048"]},"department":[{"_id":"IlCa"}]},{"file":[{"access_level":"open_access","checksum":"a64094199db4dedb12fc121b7c65fe97","date_created":"2026-05-07T07:51:06Z","success":1,"creator":"dernst","file_name":"2026_MNRAS_Parsons.pdf","relation":"main_file","file_id":"21834","content_type":"application/pdf","file_size":5955512,"date_updated":"2026-05-07T07:51:06Z"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":547,"year":"2026","publication_status":"published","date_updated":"2026-05-07T07:51:58Z","file_date_updated":"2026-05-07T07:51:06Z","external_id":{"arxiv":["2603.12888"]},"author":[{"last_name":"Parsons","first_name":"S. G.","full_name":"Parsons, S. G."},{"full_name":"Brown, A. J.","last_name":"Brown","first_name":"A. J."},{"full_name":"Casewell, S. L.","first_name":"S. L.","last_name":"Casewell"},{"full_name":"Littlefair, S. P.","first_name":"S. P.","last_name":"Littlefair"},{"id":"4d122fc8-6083-11f0-87a5-97d68b860333","full_name":"van Roestel, Joannes C","last_name":"van Roestel","first_name":"Joannes C"},{"first_name":"A.","last_name":"Rebassa-Mansergas","full_name":"Rebassa-Mansergas, A."},{"first_name":"R.","last_name":"Murillo-Ojeda","full_name":"Murillo-Ojeda, R."},{"last_name":"Zorotovic","first_name":"M.","full_name":"Zorotovic, M."},{"full_name":"Schreiber, M. R.","first_name":"M. R.","last_name":"Schreiber"},{"last_name":"Bagnulo","first_name":"S.","full_name":"Bagnulo, S."},{"last_name":"Stroet","first_name":"M. A.","full_name":"Stroet, M. A."},{"last_name":"Castro Segura","first_name":"N.","full_name":"Castro Segura, N."},{"full_name":"Dhillon, V. S.","last_name":"Dhillon","first_name":"V. S."},{"last_name":"Dyer","first_name":"M. J.","full_name":"Dyer, M. J."},{"full_name":"Garbutt, J. A.","first_name":"J. A.","last_name":"Garbutt"},{"last_name":"Green","first_name":"M. J.","full_name":"Green, M. J."},{"first_name":"D.","last_name":"Jarvis","full_name":"Jarvis, D."},{"full_name":"Kennedy, M. R.","first_name":"M. R.","last_name":"Kennedy"},{"full_name":"Kerry, P.","first_name":"P.","last_name":"Kerry"},{"first_name":"J.","last_name":"Mccormac","full_name":"Mccormac, J."},{"full_name":"Munday, J.","last_name":"Munday","first_name":"J."},{"full_name":"Pelisoli, I.","first_name":"I.","last_name":"Pelisoli"},{"full_name":"Pike, E.","first_name":"E.","last_name":"Pike"},{"full_name":"Sahman, D. I.","last_name":"Sahman","first_name":"D. I."},{"last_name":"Yates","first_name":"A.","full_name":"Yates, A."}],"abstract":[{"lang":"eng","text":"It is predicted that half or more of all cataclysmic variables (CVs) should have evolved past the period minimum and now exist as so-called period bouncers where a white dwarf should be accreting from a Roche lobe filling substellar companion. However, this prediction stands in stark contrast to observations, where only a few per cent of CVs are found in this evolutionary phase. A potential solution to this discrepancy is that a magnetic field emerges from within the white dwarf after the system has reached the period minimum. The transfer of angular momentum from the spin of the white dwarf into the orbit then pushes the two stars apart, detaching them for potentially billions of years. Here we present the discovery of ZTF J021804.16+071152.93, a detached 0.69 +- 0.01 M, 19 MG magnetic white dwarf plus 37 +- 5MJup brown dwarf binary with an orbital period of 1.7 h. The kinematics of the system indicate that it is a high probability member of the Galactic thick disc. However, this strongly disagrees with the much younger age of the system obtained from the white dwarf parameters, implying that the system may have been accreting in the past. This system is therefore consistent with having detached as a result of the emergence of the magnetic field of the white dwarf when the system was still mass transferring, and may represent the ultimate fate for many (perhaps even most) CVs."}],"department":[{"_id":"IlCa"}],"_id":"21780","oa_version":"Published Version","article_type":"original","oa":1,"has_accepted_license":"1","status":"public","arxiv":1,"doi":"10.1093/mnras/stag521","date_created":"2026-05-03T22:01:37Z","acknowledgement":"The results presented in this paper are based on observations collected at the European Southern Observatory under programme IDs 113.D-0277 and 114.D-0066 and on observations made with the Gran Telescopio Canarias (programme ID GTC119-23B), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma.\r\n\r\nSGP acknowledges support by the Science and Technology Facilities Council (grant ST/B001174/1). ARM acknowledges support from MINECO under the PID2023-148661NB-I00 grant and by the AGAUR/Generalitat de Catalunya grant SGR-386/2021. RMO was funded by INTA through grant PRE-OBSERVATORIO and acknowledges support from project PID2023-146210NB-I00 funded by MICIU/AEI/10.13039/501100011033 and by ERDF/EU. MZ acknowledges support from FONDECYT (grants 1250525 and 1221059). VSD and HiPERCAM were funded by the Science and Technology Facilities Council (grant ST/Z000033/1). MRS thanks for support from FONDECYT (grant No. 1221059). This project received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (Grant agreement numbers 101002408-MOS100PC).","DOAJ_listed":"1","day":"01","type":"journal_article","issue":"4","title":"ZTF J021804.16+071152.93: A dead cataclysmic variable and potential solution to the missing period bouncer cataclysmic variables","OA_type":"gold","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","publisher":"Oxford University Press","OA_place":"publisher","language":[{"iso":"eng"}],"month":"04","intvolume":" 547","article_number":"stag521","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"citation":{"mla":"Parsons, S. G., et al. “ZTF J021804.16+071152.93: A Dead Cataclysmic Variable and Potential Solution to the Missing Period Bouncer Cataclysmic Variables.” Monthly Notices of the Royal Astronomical Society, vol. 547, no. 4, stag521, Oxford University Press, 2026, doi:10.1093/mnras/stag521.","chicago":"Parsons, S. G., A. J. Brown, S. L. Casewell, S. P. Littlefair, Joannes C van Roestel, A. Rebassa-Mansergas, R. Murillo-Ojeda, et al. “ZTF J021804.16+071152.93: A Dead Cataclysmic Variable and Potential Solution to the Missing Period Bouncer Cataclysmic Variables.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag521.","ieee":"S. G. Parsons et al., “ZTF J021804.16+071152.93: A dead cataclysmic variable and potential solution to the missing period bouncer cataclysmic variables,” Monthly Notices of the Royal Astronomical Society, vol. 547, no. 4. Oxford University Press, 2026.","ama":"Parsons SG, Brown AJ, Casewell SL, et al. ZTF J021804.16+071152.93: A dead cataclysmic variable and potential solution to the missing period bouncer cataclysmic variables. Monthly Notices of the Royal Astronomical Society. 2026;547(4). doi:10.1093/mnras/stag521","short":"S.G. Parsons, A.J. Brown, S.L. Casewell, S.P. Littlefair, J.C. van Roestel, A. Rebassa-Mansergas, R. Murillo-Ojeda, M. Zorotovic, M.R. Schreiber, S. Bagnulo, M.A. Stroet, N. Castro Segura, V.S. Dhillon, M.J. Dyer, J.A. Garbutt, M.J. Green, D. Jarvis, M.R. Kennedy, P. Kerry, J. Mccormac, J. Munday, I. Pelisoli, E. Pike, D.I. Sahman, A. Yates, Monthly Notices of the Royal Astronomical Society 547 (2026).","apa":"Parsons, S. G., Brown, A. J., Casewell, S. L., Littlefair, S. P., van Roestel, J. C., Rebassa-Mansergas, A., … Yates, A. (2026). ZTF J021804.16+071152.93: A dead cataclysmic variable and potential solution to the missing period bouncer cataclysmic variables. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag521","ista":"Parsons SG, Brown AJ, Casewell SL, Littlefair SP, van Roestel JC, Rebassa-Mansergas A, Murillo-Ojeda R, Zorotovic M, Schreiber MR, Bagnulo S, Stroet MA, Castro Segura N, Dhillon VS, Dyer MJ, Garbutt JA, Green MJ, Jarvis D, Kennedy MR, Kerry P, Mccormac J, Munday J, Pelisoli I, Pike E, Sahman DI, Yates A. 2026. ZTF J021804.16+071152.93: A dead cataclysmic variable and potential solution to the missing period bouncer cataclysmic variables. Monthly Notices of the Royal Astronomical Society. 547(4), stag521."},"date_published":"2026-04-01T00:00:00Z"},{"article_type":"original","oa":1,"_id":"21897","oa_version":"Published Version","PlanS_conform":"1","department":[{"_id":"IlCa"}],"external_id":{"arxiv":["2604.06460"]},"author":[{"last_name":"Green","first_name":"Matthew J","full_name":"Green, Matthew J"},{"full_name":"Marsh, Thomas R","last_name":"Marsh","first_name":"Thomas R"},{"full_name":"van Roestel, Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","first_name":"Joannes C","last_name":"van Roestel"},{"full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny","last_name":"Wong"},{"full_name":"Belloni, Diogo","last_name":"Belloni","first_name":"Diogo"},{"first_name":"Mukremin","last_name":"Kilic","full_name":"Kilic, Mukremin"},{"first_name":"Elmé","last_name":"Breedt","full_name":"Breedt, Elmé"},{"first_name":"Alex","last_name":"Brown","full_name":"Brown, Alex"},{"full_name":"Copperwheat, Chris M","first_name":"Chris M","last_name":"Copperwheat"},{"full_name":"Chakpor, Anurak","first_name":"Anurak","last_name":"Chakpor"},{"full_name":"Dhillon, V S","last_name":"Dhillon","first_name":"V S"},{"first_name":"Noel Castro","last_name":"Segura","full_name":"Segura, Noel Castro"},{"first_name":"Martin J","last_name":"Dyer","full_name":"Dyer, Martin J"},{"full_name":"Garbutt, James","first_name":"James","last_name":"Garbutt"},{"full_name":"Jarvis, Dan","last_name":"Jarvis","first_name":"Dan"},{"first_name":"Vasu","last_name":"Kengkriangkrai","full_name":"Kengkriangkrai, Vasu"},{"full_name":"Kennedy, Mark R","last_name":"Kennedy","first_name":"Mark R"},{"last_name":"Kerry","first_name":"Paul","full_name":"Kerry, Paul"},{"last_name":"Kupfer","first_name":"Thomas","full_name":"Kupfer, Thomas"},{"full_name":"Littlefair, S P","last_name":"Littlefair","first_name":"S P"},{"first_name":"James","last_name":"McCormac","full_name":"McCormac, James"},{"first_name":"James","last_name":"Munday","full_name":"Munday, James"},{"last_name":"Parsons","first_name":"Steven G","full_name":"Parsons, Steven G"},{"full_name":"Pike, Eleanor","first_name":"Eleanor","last_name":"Pike"},{"full_name":"Pelisoli, Ingrid","first_name":"Ingrid","last_name":"Pelisoli"},{"last_name":"Rodríguez-Gil","first_name":"Pablo","full_name":"Rodríguez-Gil, Pablo"},{"full_name":"Sahman, David I","last_name":"Sahman","first_name":"David I"},{"first_name":"Amalie","last_name":"Yates","full_name":"Yates, Amalie"}],"abstract":[{"lang":"eng","text":"Ultracompact binary systems, consisting of two compact objects in an orbit $\\lesssim 0.5 {\\rm R}_\\odot$, should exhibit measurable rates of orbital period change ($\\dot{P} \\ne 0$) due to the emission of gravitational waves (GWs). Measurements of $\\dot{P}$ have so far been limited to the shortest-period ultracompact binaries ($\\lesssim 20$ min). Among the AM CVn-type subclass, several works have proposed the presence of extra angular momentum loss beyond GW emission, with magnetic braking being a widely discussed mechanism. If present, this magnetic braking would dominate the angular momentum loss of AM CVn-type binaries with orbital periods $\\gtrsim 30$ min. In this work, we present a long-term eclipse timing study of two AM CVn-type binaries, YZ LMi and Gaia14aae, with respective orbital periods of 28.3 min and 49.7 min and continuous observations since 2006 and 2015. Both systems show $\\dot{P}$ consistent with zero within $2\\sigma$. Their $3\\sigma$ upper limits are $1.1 \\times 10^{-13}\\, {\\rm s \\, s}^{-1}$ and $9.7 \\times 10^{-14}\\, {\\rm s \\, s}^{-1}$, respectively. These non-detections are most simply explained by a scenario in which secular angular momentum loss is not substantially stronger than GW emission at all orbital periods, but is combined with deviations from the secular $\\dot{P}$ whose time-scales span decades but whose amplitude is $\\lesssim 10^{-13}\\, {\\rm s \\, s}^{-1}$. Our non-detections of $\\dot{P}$ represent a limit on the strength of any enhanced angular momentum loss beyond pure GW emission."}],"file_date_updated":"2026-05-21T06:37:42Z","date_updated":"2026-05-21T06:41:41Z","keyword":["binaries: close – stars","dwarf novae – novae","cataclysmic variables – white dwarfs"],"volume":548,"year":"2026","publication_status":"published","file":[{"file_name":"2026_MNRAS_Green.pdf","content_type":"application/pdf","file_id":"21903","relation":"main_file","date_updated":"2026-05-21T06:37:42Z","file_size":3960296,"access_level":"open_access","date_created":"2026-05-21T06:37:42Z","checksum":"2c4463926c5cb84ce555ef2005b52ddd","creator":"dernst","success":1}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"M.J. Green, T.R. Marsh, J.C. van Roestel, T.L.S. Wong, D. Belloni, M. Kilic, E. Breedt, A. Brown, C.M. Copperwheat, A. Chakpor, V.S. Dhillon, N.C. Segura, M.J. Dyer, J. Garbutt, D. Jarvis, V. Kengkriangkrai, M.R. Kennedy, P. Kerry, T. Kupfer, S.P. Littlefair, J. McCormac, J. Munday, S.G. Parsons, E. Pike, I. Pelisoli, P. Rodríguez-Gil, D.I. Sahman, A. Yates, Monthly Notices of the Royal Astronomical Society 548 (2026).","ista":"Green MJ, Marsh TR, van Roestel JC, Wong TLS, Belloni D, Kilic M, Breedt E, Brown A, Copperwheat CM, Chakpor A, Dhillon VS, Segura NC, Dyer MJ, Garbutt J, Jarvis D, Kengkriangkrai V, Kennedy MR, Kerry P, Kupfer T, Littlefair SP, McCormac J, Munday J, Parsons SG, Pike E, Pelisoli I, Rodríguez-Gil P, Sahman DI, Yates A. 2026. No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. 548(3), stag673.","apa":"Green, M. J., Marsh, T. R., van Roestel, J. C., Wong, T. L. S., Belloni, D., Kilic, M., … Yates, A. (2026). No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag673","mla":"Green, Matthew J., et al. “No Period Change in Two Long-Period AM CVn Binaries.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3, stag673, Oxford University Press, 2026, doi:10.1093/mnras/stag673.","ama":"Green MJ, Marsh TR, van Roestel JC, et al. No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. 2026;548(3). doi:10.1093/mnras/stag673","chicago":"Green, Matthew J, Thomas R Marsh, Joannes C van Roestel, Tin Long Sunny Wong, Diogo Belloni, Mukremin Kilic, Elmé Breedt, et al. “No Period Change in Two Long-Period AM CVn Binaries.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag673.","ieee":"M. J. Green et al., “No period change in two long-period AM CVn binaries,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3. Oxford University Press, 2026."},"date_published":"2026-04-09T00:00:00Z","intvolume":" 548","article_number":"stag673","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"04","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"ddc":["520"],"issue":"3","title":"No period change in two long-period AM CVn binaries","OA_type":"gold","acknowledgement":"We are grateful to the anonymousreferee fortheirinsightful comments. MJG thanks Mitch Begelman and the JILA department at the University of Colorado, Boulder, for providing office space at which much of this paper was written. This work is supported in part by the United States National Aeronautics and Space Administration (NASA) under grants\r\n80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380, and the United States National Science Foundation (NSF) under grant AST-2508429. VSD and HiPERCAM are funded by the Science and Technology Facilities Council (grant ST/Z000033/1). IP acknowledges support from the Royal Society through a University Research Fellowship (URF\\R1\\231496). This project has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement numbers 101002408 – MOS100PC). CMC receives funding from United Kingdom Research and Innovation grant numbers ST/X005933/1 and ST/W001934/1. This article is based in part on observations made in the Observatorios de Canarias del Instituto de Astrofísica de Canarias (IAC) with the the William Herschel Telescope (WHT) operated on the island of La Palma by the Isaac Newton Group (ING) in the Observatorio del Roque de los Muchachos. It is also based in part on observations made with the Gran Telescopio Canarias (GTC) under proposal ID GTC18-24A, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Further data were obtained using the 2.4 m Thai National Telescope (TNT) operated by the National Astronomy Research Institute of Thailand\r\n(NARIT), and the 200-inch Hale Telescope at Palomar Observatory operated by the California Institute of Technology. Software packages used in this work include the ultracam and hipercam reduction pipelines, lcurve (C. M. Copperwheat et al. 2010), numpy, astropy, matplotlib, and emcee (D. Foreman-Mackey et al. 2013).","DOAJ_listed":"1","type":"journal_article","day":"09","status":"public","has_accepted_license":"1","arxiv":1,"date_created":"2026-05-20T14:34:03Z","doi":"10.1093/mnras/stag673"},{"date_published":"2026-05-01T00:00:00Z","citation":{"mla":"Roberts-Borsani, Guido, et al. “JWST Spectroscopic Insights into the Diversity of Galaxies in the First 500 Myr: Short-Lived Snapshots along a Common Evolutionary Pathway.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3, stag701, Oxford University Press, 2026, doi:10.1093/mnras/stag701.","ama":"Roberts-Borsani G, Oesch PA, Ellis R, et al. JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. 2026;548(3). doi:10.1093/mnras/stag701","ieee":"G. Roberts-Borsani et al., “JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3. Oxford University Press, 2026.","chicago":"Roberts-Borsani, Guido, Pascal A Oesch, Richard Ellis, Andrea Weibel, Emma Giovinazzo, Rychard Bouwens, Pratika Dayal, et al. “JWST Spectroscopic Insights into the Diversity of Galaxies in the First 500 Myr: Short-Lived Snapshots along a Common Evolutionary Pathway.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag701.","short":"G. Roberts-Borsani, P.A. Oesch, R. Ellis, A. Weibel, E. Giovinazzo, R. Bouwens, P. Dayal, A. Fontana, K.E. Heintz, J.J. Matthee, R.A. Meyer, L. Pentericci, A. Shapley, S. Tacchella, T. Treu, F. Walter, H. Atek, S. Bose, M. Castellano, Y. Fudamoto, T. Morishita, R.P. Naidu, R.L. Sanders, A. van der Wel, Monthly Notices of the Royal Astronomical Society 548 (2026).","ista":"Roberts-Borsani G, Oesch PA, Ellis R, Weibel A, Giovinazzo E, Bouwens R, Dayal P, Fontana A, Heintz KE, Matthee JJ, Meyer RA, Pentericci L, Shapley A, Tacchella S, Treu T, Walter F, Atek H, Bose S, Castellano M, Fudamoto Y, Morishita T, Naidu RP, Sanders RL, van der Wel A. 2026. JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. 548(3), stag701.","apa":"Roberts-Borsani, G., Oesch, P. A., Ellis, R., Weibel, A., Giovinazzo, E., Bouwens, R., … van der Wel, A. (2026). JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag701"},"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_number":"stag701","intvolume":" 548","month":"05","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","article_processing_charge":"Yes","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","ddc":["520"],"scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"OA_type":"gold","issue":"3","title":"JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway","day":"01","type":"journal_article","DOAJ_listed":"1","acknowledgement":"We thank the anonymous referee for useful and constructive\r\nfeedback that improved the manuscript. GRB is grateful to Vasily\r\nBelokurov and Sarah Kane for providing the relevant abundances\r\nforthe Aurora data in Fig. 11, as well asto Tiger Yu-Yang Hsiao for\r\nhelpful discussions regarding the MACS 0647-JD source. We are\r\nalso grateful to Gabe Brammerfor useful discussions and his continuous efforts in maintaining and improving the msaexp code,\r\nfrom which the high-z community continues to benefit greatly.\r\nLastly, we also thank the numerous teams of the observational\r\nprograms used in this study, for developing these valuable data\r\nsets. The data used in this study are derived from the following\r\nprograms: 1181 (PI Eisenstein; D. J. Eisenstein et al. 2023a), 1210\r\n(PI Luetzgendorf; D. J. Eisenstein et al. 2023a), 1211 (PI Isaak;\r\nM. V. Maseda et al. 2024), 1286 (PI Luetzgendorf; D. J. Eisenstein\r\net al. 2023a), 1287 (PI Isaak; D. J. Eisenstein et al. 2023a), 1345\r\n(PI Finkelstein; S. L. Finkelstein et al. 2025), 1433 (PI Coe; T. Y.-\r\nY. Hsiao et al. 2024a), 2561 (PI Labbé; R. Bezanson et al. 2022),\r\n2750 (PI Arrabal Haro; P. Arrabal Haro et al. 2023b), 3073 (PI\r\nCastellano; M. Castellano et al. 2024), 3215 (PIs Eisenstein &\r\nMaiolino; D. J. Eisenstein et al. 2023b), 5224 (PIs Oesch & Naidu;\r\nOesch et al. in preparation), 6368 (PI Dickinson; V. Kokorev et al.\r\n2025). The authors acknowledge the aforementioned teams and\r\nPIs where development of their observing program(s) was done\r\nwith a zero-exclusive-access period.\r\nThis work is based on observations made with the\r\nNASA/ESA/CSA JWST. The data were obtained from the\r\nMikulski Archive for Space Telescopes at the Space Telescope\r\nScience Institute, which is operated by the Association of\r\nUniversities for Research in Astronomy, Inc., under NASA\r\ncontract NAS 5-03127 for JWST. The specific observations\r\nanalysed can be accessed via DOI 10.17909/jqj3-ws37. Some\r\nof the data products presented herein were retrieved from the\r\nDawn JWST Archive (DJA). DJA is an initiative of the Cosmic\r\nDawn Center (DAWN), which is funded by the Danish National\r\nResearch Foundation under grant DNRF140.\r\nRSE acknowledges generous financial support from the Peter\r\nand Patricia Gruber Foundation. YF acknowledgessupportsfrom\r\nJSPS KAKENHI Grant Numbers JP22K21349 and JP23K13149.\r\nThis work has received funding from the Swiss State Secretariat\r\nfor Education, Research and Innovation (SERI) under contract\r\nnumber MB22.00072, as well as from the Swiss National Science\r\nFoundation (SNSF) through project grant 200020_207349.","arxiv":1,"date_created":"2026-05-20T14:34:29Z","doi":"10.1093/mnras/stag701","status":"public","has_accepted_license":"1","oa":1,"article_type":"original","oa_version":"Published Version","_id":"21898","department":[{"_id":"JoMa"}],"PlanS_conform":"1","abstract":[{"lang":"eng","text":"We investigate the nature and spectroscopic diversity of early galaxies from a sample of 41 sources at $z\\geqslant 10$ with James Webb Space Telescope (JWST)/NIRSpec prism observations. We compare the properties of strong ultraviolet (UV) line emitters, traced by intense C iv emission, with those of more ‘typical’ sources with weak or undetected C iv. The more typical (or ‘C iv-weak’) sources reveal significant scatter in their C iii] line strengths, UV continuum slopes, and physical sizes, spanning C iii] equivalent widths (EWs) of $\\sim$1–51 Å, UV slopes of $\\beta \\sim -1.6$ to $-2.6$, and half-light radii of $\\sim$50–1000 pc. In contrast, C iv-strong sources occupy the tail of these distributions, with C iii] EWs of 16–51 Å, UV slopes $\\beta \\lesssim -2.5$, compact morphologies ($r_{\\rm 50} \\lesssim 100$ pc), and elevated star formation surface densities ($\\Sigma _{\\rm SFR} \\gtrsim 100\\, M_\\odot \\, \\mathrm{yr}^{-1}\\, \\mathrm{kpc}^{-2}$). These properties suggest concentrated starbursts that temporarily outshine the host galaxy. Comparing average properties from composite spectra, we find the diversity of the sample is primarily driven by bursty star formation on very short time-scales ($\\le$3 Myr), with strong C iv emitters observed at the apex of the bursts and sources devoid of emission lines during relative inactivity. An apparent association between strong C iv and enhanced nitrogen abundance suggests both may be modulated by the same duty cycle, reflecting a generic mode of star formation. We show that active galactic nuclei are unlikely to contribute significantly to this duty cycle based on UV line diagnostics and photoionization models. Our results support a picture whereby brief bursts and lulls can explain the spectral diversity and early growth of bright galaxies in the first 500 Myr."}],"author":[{"first_name":"Guido","last_name":"Roberts-Borsani","full_name":"Roberts-Borsani, Guido"},{"last_name":"Oesch","first_name":"Pascal A","full_name":"Oesch, Pascal A"},{"full_name":"Ellis, Richard","last_name":"Ellis","first_name":"Richard"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"full_name":"Giovinazzo, Emma","first_name":"Emma","last_name":"Giovinazzo"},{"full_name":"Bouwens, Rychard","first_name":"Rychard","last_name":"Bouwens"},{"last_name":"Dayal","first_name":"Pratika","full_name":"Dayal, Pratika"},{"first_name":"Adriano","last_name":"Fontana","full_name":"Fontana, Adriano"},{"full_name":"Heintz, Kasper E","last_name":"Heintz","first_name":"Kasper E"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee"},{"first_name":"Romain A","last_name":"Meyer","full_name":"Meyer, Romain A"},{"first_name":"Laura","last_name":"Pentericci","full_name":"Pentericci, Laura"},{"last_name":"Shapley","first_name":"Alice","full_name":"Shapley, Alice"},{"first_name":"Sandro","last_name":"Tacchella","full_name":"Tacchella, Sandro"},{"last_name":"Treu","first_name":"Tommaso","full_name":"Treu, Tommaso"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"last_name":"Atek","first_name":"Hakim","full_name":"Atek, Hakim"},{"full_name":"Bose, Sownak","first_name":"Sownak","last_name":"Bose"},{"full_name":"Castellano, Marco","first_name":"Marco","last_name":"Castellano"},{"last_name":"Fudamoto","first_name":"Yoshinobu","full_name":"Fudamoto, Yoshinobu"},{"last_name":"Morishita","first_name":"Takahiro","full_name":"Morishita, Takahiro"},{"full_name":"Naidu, Rohan P","last_name":"Naidu","first_name":"Rohan P"},{"last_name":"Sanders","first_name":"Ryan L","full_name":"Sanders, Ryan L"},{"full_name":"van der Wel, Arjen","first_name":"Arjen","last_name":"van der Wel"}],"external_id":{"arxiv":["2508.21708"]},"file_date_updated":"2026-05-21T06:14:23Z","date_updated":"2026-05-21T06:16:04Z","publication_status":"published","volume":548,"year":"2026","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"creator":"dernst","success":1,"date_created":"2026-05-21T06:14:23Z","checksum":"b8f52c6fc5e06b3a505310e7d5898ecf","access_level":"open_access","file_size":3539140,"date_updated":"2026-05-21T06:14:23Z","content_type":"application/pdf","file_id":"21902","relation":"main_file","file_name":"2026_MNRAS_RobertsBorsani.pdf"}]},{"file":[{"success":1,"creator":"dernst","checksum":"68f04ab0fdcee4f12341d116c5f794cd","date_created":"2026-01-12T09:43:07Z","access_level":"open_access","date_updated":"2026-01-12T09:43:07Z","file_size":2174272,"relation":"main_file","file_id":"20979","content_type":"application/pdf","file_name":"2026_MonthNoticesRAS_Kist.pdf"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":545,"year":"2026","publication_status":"published","date_updated":"2026-01-12T09:45:54Z","file_date_updated":"2026-01-12T09:43:07Z","external_id":{"arxiv":["2508.21818"]},"author":[{"last_name":"Kist","first_name":"Timo","full_name":"Kist, Timo"},{"first_name":"Joseph F.","last_name":"Hennawi","full_name":"Hennawi, Joseph F."},{"first_name":"Frederick B.","last_name":"Davies","full_name":"Davies, Frederick B."},{"full_name":"Bañados, Eduardo","first_name":"Eduardo","last_name":"Bañados"},{"full_name":"Bosman, Sarah E.I.","first_name":"Sarah E.I.","last_name":"Bosman"},{"last_name":"Cai","first_name":"Zheng","full_name":"Cai, Zheng"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"full_name":"Fan, Xiaohui","first_name":"Xiaohui","last_name":"Fan"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"full_name":"Jun, Hyunsung D.","first_name":"Hyunsung D.","last_name":"Jun"},{"last_name":"Liu","first_name":"Yichen","full_name":"Liu, Yichen"},{"first_name":"Jinyi","last_name":"Yang","full_name":"Yang, Jinyi"},{"full_name":"Wang, Feige","first_name":"Feige","last_name":"Wang"}],"abstract":[{"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.","lang":"eng"}],"PlanS_conform":"1","department":[{"_id":"ZoHa"}],"_id":"20974","oa_version":"Published Version","article_type":"original","oa":1,"has_accepted_license":"1","status":"public","arxiv":1,"date_created":"2026-01-11T23:01:34Z","doi":"10.1093/mnras/staf2219","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.","DOAJ_listed":"1","type":"journal_article","day":"01","title":"First constraints on the local ionization topology in front of two quasars at z ∼ 7.5","issue":"3","OA_type":"gold","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","OA_place":"publisher","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"01","intvolume":" 545","article_number":"staf2219","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"citation":{"mla":"Kist, Timo, et al. “First Constraints on the Local Ionization Topology in Front of Two Quasars at z ∼ 7.5.” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 3, staf2219, Oxford University Press, 2026, doi:10.1093/mnras/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. Monthly Notices of the Royal Astronomical Society. 2026;545(3). doi:10.1093/mnras/staf2219","ieee":"T. Kist et al., “First constraints on the local ionization topology in front of two quasars at z ∼ 7.5,” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 3. Oxford University Press, 2026.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/staf2219.","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).","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.","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf2219"},"date_published":"2026-01-01T00:00:00Z"},{"quality_controlled":"1","article_processing_charge":"Yes","publication":"Monthly Notices of the Royal Astronomical Society","month":"02","publisher":"Oxford University Press","OA_place":"publisher","language":[{"iso":"eng"}],"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_number":"staf2131","intvolume":" 545","citation":{"short":"S.J. Chang, M. Gronke, J.J. Matthee, C. Mason, Monthly Notices of the Royal Astronomical Society 545 (2026).","apa":"Chang, S. J., Gronke, M., Matthee, J. J., & 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. Oxford University Press. https://doi.org/10.1093/mnras/staf2131","ista":"Chang SJ, Gronke M, Matthee JJ, Mason C. 2026. Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots. Monthly Notices of the Royal Astronomical Society. 545(4), staf2131.","mla":"Chang, Seok Jun, et al. “Impact of Resonance, Raman, and Thomson Scattering on Hydrogen Line Formation in Little Red Dots.” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 4, staf2131, Oxford University Press, 2026, doi:10.1093/mnras/staf2131.","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,” Monthly Notices of the Royal Astronomical Society, vol. 545, no. 4. Oxford University Press, 2026.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/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. Monthly Notices of the Royal Astronomical Society. 2026;545(4). doi:10.1093/mnras/staf2131"},"date_published":"2026-02-01T00:00:00Z","date_created":"2026-01-25T23:01:39Z","doi":"10.1093/mnras/staf2131","arxiv":1,"has_accepted_license":"1","status":"public","type":"journal_article","day":"01","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.","DOAJ_listed":"1","issue":"4","title":"Impact of resonance, Raman, and Thomson scattering on hydrogen line formation in Little Red Dots","OA_type":"gold","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","ddc":["520"],"abstract":[{"lang":"eng","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."}],"external_id":{"arxiv":["2508.08768"]},"author":[{"full_name":"Chang, Seok Jun","first_name":"Seok Jun","last_name":"Chang"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Charlotte","last_name":"Mason","full_name":"Mason, Charlotte"}],"department":[{"_id":"JoMa"}],"PlanS_conform":"1","oa_version":"Published Version","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"_id":"21038","oa":1,"article_type":"original","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_size":5600366,"date_updated":"2026-02-12T12:44:33Z","content_type":"application/pdf","file_id":"21220","relation":"main_file","file_name":"2026_MonthNoticesRAS_Chang.pdf","creator":"dernst","success":1,"date_created":"2026-02-12T12:44:33Z","checksum":"52ba7d7b5b80af0c50f57e4c2acc3930","access_level":"open_access"}],"publication_status":"published","year":"2026","volume":545,"date_updated":"2026-02-12T12:56:33Z","file_date_updated":"2026-02-12T12:44:33Z"},{"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","month":"06","intvolume":" 540","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-06-01T00:00:00Z","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf561","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.","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.","ieee":"T. Cunningham et al., “Discovery of two new polars evolved past the period bounce,” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 1. Oxford University Press, pp. 633–649, 2025.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf561.","ama":"Cunningham T, Caiazzo I, Sienkiewicz G, et al. Discovery of two new polars evolved past the period bounce. Monthly Notices of the Royal Astronomical Society. 2025;540(1):633-649. doi:10.1093/mnras/staf561","mla":"Cunningham, Tim, et al. “Discovery of Two New Polars Evolved Past the Period Bounce.” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 1, Oxford University Press, 2025, pp. 633–49, doi:10.1093/mnras/staf561."},"status":"public","has_accepted_license":"1","doi":"10.1093/mnras/staf561","arxiv":1,"date_created":"2025-06-15T22:01:29Z","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).","type":"journal_article","day":"01","OA_type":"gold","issue":"1","title":"Discovery of two new polars evolved past the period bounce","ddc":["520"],"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"author":[{"last_name":"Cunningham","first_name":"Tim","full_name":"Cunningham, Tim"},{"last_name":"Caiazzo","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria"},{"first_name":"Gracjan","last_name":"Sienkiewicz","full_name":"Sienkiewicz, Gracjan"},{"last_name":"Wheatley","first_name":"Peter J.","full_name":"Wheatley, Peter J."},{"first_name":"Boris T.","last_name":"Gänsicke","full_name":"Gänsicke, Boris T."},{"full_name":"El-Badry, Kareem","first_name":"Kareem","last_name":"El-Badry"},{"first_name":"Riccardo","last_name":"Arcodia","full_name":"Arcodia, Riccardo"},{"last_name":"Charbonneau","first_name":"David","full_name":"Charbonneau, David"},{"last_name":"Connor","first_name":"Liam","full_name":"Connor, Liam"},{"first_name":"Kishalay","last_name":"De","full_name":"De, Kishalay"},{"full_name":"Hakala, Pasi","first_name":"Pasi","last_name":"Hakala"},{"last_name":"Kenyon","first_name":"Scott J.","full_name":"Kenyon, Scott J."},{"full_name":"Maheshwari, Sumit Kumar","last_name":"Maheshwari","first_name":"Sumit Kumar"},{"full_name":"Rodriguez, Antonio C.","first_name":"Antonio C.","last_name":"Rodriguez"},{"first_name":"Jan","last_name":"Van Roestel","full_name":"Van Roestel, Jan"},{"first_name":"Pier Emmanuel","last_name":"Tremblay","full_name":"Tremblay, Pier Emmanuel"}],"external_id":{"arxiv":["2503.12675"],"isi":["001493143700001"]},"abstract":[{"lang":"eng","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."}],"department":[{"_id":"IlCa"}],"_id":"19840","oa_version":"Published Version","article_type":"original","page":"633-649","oa":1,"file":[{"relation":"main_file","content_type":"application/pdf","file_id":"19864","date_updated":"2025-06-23T07:28:36Z","file_size":3212636,"file_name":"2025_MonthlyNoticesRAS_Cunningham.pdf","checksum":"5e675d3696c222e919d6916bad194b01","date_created":"2025-06-23T07:28:36Z","success":1,"creator":"dernst","access_level":"open_access"}],"isi":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","volume":540,"year":"2025","publication_status":"published","date_updated":"2025-09-30T12:50:33Z","file_date_updated":"2025-06-23T07:28:36Z"},{"article_type":"original","page":"2331-2348","oa":1,"_id":"19855","oa_version":"Published Version","department":[{"_id":"JoMa"}],"external_id":{"arxiv":["2410.03337"],"isi":["001506103600001"]},"author":[{"full_name":"Gazagnes, S.","last_name":"Gazagnes","first_name":"S."},{"first_name":"J.","last_name":"Chisholm","full_name":"Chisholm, J."},{"full_name":"Endsley, R.","last_name":"Endsley","first_name":"R."},{"full_name":"Berg, D. A.","first_name":"D. A.","last_name":"Berg"},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"last_name":"Jurlin","first_name":"N.","full_name":"Jurlin, N."},{"first_name":"A.","last_name":"Saldana-Lopez","full_name":"Saldana-Lopez, A."},{"last_name":"Finkelstein","first_name":"S. L.","full_name":"Finkelstein, S. L."},{"full_name":"Flury, S. R.","first_name":"S. R.","last_name":"Flury"},{"full_name":"Guseva, N. G.","last_name":"Guseva","first_name":"N. G."},{"last_name":"Henry","first_name":"A.","full_name":"Henry, A."},{"full_name":"Izotov, Y. I.","last_name":"Izotov","first_name":"Y. I."},{"last_name":"Jung","first_name":"I.","full_name":"Jung, I."},{"last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."}],"abstract":[{"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.","lang":"eng"}],"file_date_updated":"2025-06-23T11:02:59Z","date_updated":"2025-09-30T13:34:20Z","year":"2025","volume":540,"publication_status":"published","file":[{"file_name":"2025_MonthlyNoticesRAS_Gazagnes.pdf","file_size":3111567,"date_updated":"2025-06-23T11:02:59Z","relation":"main_file","file_id":"19870","content_type":"application/pdf","access_level":"open_access","success":1,"creator":"dernst","checksum":"f912c990a0474f1ddf9be6b8a89c7759","date_created":"2025-06-23T11:02:59Z"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","isi":1,"citation":{"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.","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf768","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.","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. Monthly Notices of the Royal Astronomical Society. 2025;540(3):2331-2348. doi:10.1093/mnras/staf768","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf768.","ieee":"S. Gazagnes et al., “A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization,” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 3. Oxford University Press, pp. 2331–2348, 2025.","mla":"Gazagnes, S., et al. “A Negligible Contribution of Two Luminous z ∼7.5 Galaxies to the Ionizing Photon Budget of Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 540, no. 3, Oxford University Press, 2025, pp. 2331–48, doi:10.1093/mnras/staf768."},"date_published":"2025-07-01T00:00:00Z","intvolume":" 540","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publisher":"Oxford University Press","OA_place":"publisher","language":[{"iso":"eng"}],"month":"07","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"ddc":["520"],"issue":"3","title":"A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization","OA_type":"gold","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.","type":"journal_article","day":"01","has_accepted_license":"1","status":"public","date_created":"2025-06-22T22:02:05Z","arxiv":1,"doi":"10.1093/mnras/staf768"},{"file":[{"access_level":"open_access","success":1,"creator":"dernst","checksum":"f8708c78016f8917765026502c6b50b6","date_created":"2025-07-22T07:19:20Z","file_name":"2025_MonthlyNoticesRAS_Pirie.pdf","file_size":38102038,"date_updated":"2025-07-22T07:19:20Z","relation":"main_file","file_id":"20064","content_type":"application/pdf"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","isi":1,"year":"2025","volume":541,"publication_status":"published","date_updated":"2025-09-30T14:03:40Z","file_date_updated":"2025-07-22T07:19:20Z","author":[{"last_name":"Pirie","first_name":"C. A.","full_name":"Pirie, C. A."},{"last_name":"Best","first_name":"P. N.","full_name":"Best, P. N."},{"first_name":"K. J.","last_name":"Duncan","full_name":"Duncan, K. J."},{"first_name":"D. J.","last_name":"Mcleod","full_name":"Mcleod, D. J."},{"last_name":"Cochrane","first_name":"R. K.","full_name":"Cochrane, R. K."},{"full_name":"Clausen, M.","first_name":"M.","last_name":"Clausen"},{"full_name":"Dunlop, J. S.","first_name":"J. S.","last_name":"Dunlop"},{"full_name":"Flury, S. R.","first_name":"S. R.","last_name":"Flury"},{"last_name":"Geach","first_name":"J. E.","full_name":"Geach, J. E."},{"full_name":"Hale, C. L.","last_name":"Hale","first_name":"C. L."},{"first_name":"E.","last_name":"Ibar","full_name":"Ibar, E."},{"full_name":"Kondapally, R.","first_name":"R.","last_name":"Kondapally"},{"full_name":"Li, Zefeng","last_name":"Li","first_name":"Zefeng"},{"last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Mclure, R. J.","first_name":"R. J.","last_name":"Mclure"},{"last_name":"Ossa-Fuentes","first_name":"L.","full_name":"Ossa-Fuentes, L."},{"full_name":"Patrick, A. L.","last_name":"Patrick","first_name":"A. L."},{"full_name":"Smail, Ian","first_name":"Ian","last_name":"Smail"},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"full_name":"Stephenson, H. M.O.","last_name":"Stephenson","first_name":"H. M.O."},{"full_name":"Stott, J. P.","last_name":"Stott","first_name":"J. P."},{"full_name":"Swinbank, A. M.","last_name":"Swinbank","first_name":"A. M."}],"external_id":{"isi":["001527095600001"],"arxiv":["2410.11808"]},"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. "}],"PlanS_conform":"1","department":[{"_id":"JoMa"}],"_id":"20027","oa_version":"Published Version","page":"1348-1376","article_type":"original","oa":1,"status":"public","has_accepted_license":"1","date_created":"2025-07-20T22:02:00Z","doi":"10.1093/mnras/staf1006","arxiv":1,"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.","day":"01","type":"journal_article","OA_type":"gold","issue":"2","title":"The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z > 6 and their physical properties","ddc":["520"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","month":"08","intvolume":" 541","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-08-01T00:00:00Z","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.","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 > 6 and their physical properties. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1006","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 > 6 and their physical properties. Monthly Notices of the Royal Astronomical Society. 541(2), 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 > 6 and Their Physical Properties.” Monthly Notices of the Royal Astronomical Society, vol. 541, no. 2, Oxford University Press, 2025, pp. 1348–76, doi:10.1093/mnras/staf1006.","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 > 6 and their physical properties. Monthly Notices of the Royal Astronomical Society. 2025;541(2):1348-1376. doi:10.1093/mnras/staf1006","ieee":"C. A. Pirie et al., “The JWST Emission Line Survey (JELS): An untargeted search for H α emission line galaxies at z > 6 and their physical properties,” Monthly Notices of the Royal Astronomical Society, vol. 541, no. 2. Oxford University Press, pp. 1348–1376, 2025.","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 > 6 and Their Physical Properties.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1006."}},{"day":"01","type":"journal_article","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","doi":"10.1093/mnras/staf1061","date_created":"2025-07-20T22:02:00Z","arxiv":1,"status":"public","has_accepted_license":"1","scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"ddc":["520"],"title":"The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization","issue":"2","OA_type":"gold","month":"08","OA_place":"publisher","publisher":"Oxford University Press","language":[{"iso":"eng"}],"quality_controlled":"1","article_processing_charge":"Yes","publication":"Monthly Notices of the Royal Astronomical Society","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.” Monthly Notices of the Royal Astronomical Society, vol. 541, no. 2, Oxford University Press, 2025, pp. 1329–47, doi:10.1093/mnras/staf1061.","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. Monthly Notices of the Royal Astronomical Society. 2025;541(2):1329-1347. doi:10.1093/mnras/staf1061","ieee":"K. J. Duncan et al., “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, vol. 541, no. 2. Oxford University Press, pp. 1329–1347, 2025.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1061.","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.","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1061","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."},"date_published":"2025-08-01T00:00:00Z","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":" 541","publication_status":"published","year":"2025","volume":541,"isi":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","file":[{"file_size":4451937,"date_updated":"2025-07-22T07:02:02Z","file_id":"20063","content_type":"application/pdf","relation":"main_file","file_name":"2025_MonthlyNoticesRAS_Duncan.pdf","creator":"dernst","success":1,"date_created":"2025-07-22T07:02:02Z","checksum":"abedbbce98d448f374dc922dad9133fc","access_level":"open_access"}],"file_date_updated":"2025-07-22T07:02:02Z","date_updated":"2025-09-30T14:03:01Z","department":[{"_id":"JoMa"}],"PlanS_conform":"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."}],"external_id":{"isi":["001527085900001"],"arxiv":["2410.09000"]},"author":[{"last_name":"Duncan","first_name":"K. J.","full_name":"Duncan, K. J."},{"first_name":"D. J.","last_name":"Mcleod","full_name":"Mcleod, D. J."},{"last_name":"Best","first_name":"P. N.","full_name":"Best, P. N."},{"last_name":"Pirie","first_name":"C. A.","full_name":"Pirie, C. A."},{"full_name":"Clausen, M.","first_name":"M.","last_name":"Clausen"},{"full_name":"Cochrane, R. K.","last_name":"Cochrane","first_name":"R. K."},{"first_name":"J. S.","last_name":"Dunlop","full_name":"Dunlop, J. S."},{"last_name":"Flury","first_name":"S. R.","full_name":"Flury, S. R."},{"first_name":"J. E.","last_name":"Geach","full_name":"Geach, J. E."},{"first_name":"N. A.","last_name":"Grogin","full_name":"Grogin, N. A."},{"first_name":"C. L.","last_name":"Hale","full_name":"Hale, C. L."},{"last_name":"Ibar","first_name":"E.","full_name":"Ibar, E."},{"full_name":"Kondapally, R.","first_name":"R.","last_name":"Kondapally"},{"full_name":"Li, Zefeng","last_name":"Li","first_name":"Zefeng"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"R. J.","last_name":"Mclure","full_name":"Mclure, R. J."},{"last_name":"Ossa-Fuentes","first_name":"Luis","full_name":"Ossa-Fuentes, Luis"},{"first_name":"A. L.","last_name":"Patrick","full_name":"Patrick, A. L."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"last_name":"Sobral","first_name":"D.","full_name":"Sobral, D."},{"last_name":"Stephenson","first_name":"H. M.O.","full_name":"Stephenson, H. M.O."},{"full_name":"Stott, J. P.","last_name":"Stott","first_name":"J. P."},{"first_name":"A. M.","last_name":"Swinbank","full_name":"Swinbank, A. M."}],"oa":1,"page":"1329-1347","article_type":"original","oa_version":"Published Version","_id":"20028"},{"OA_type":"gold","issue":"2","title":"Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?","ddc":["520"],"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"has_accepted_license":"1","status":"public","doi":"10.1093/mnras/staf1269","date_created":"2025-08-31T22:01:31Z","arxiv":1,"DOAJ_listed":"1","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.","day":"01","type":"journal_article","intvolume":" 542","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-09-01T00:00:00Z","citation":{"mla":"Sullivan, James, et al. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2, Oxford University Press, 2025, pp. 822–38, doi:10.1093/mnras/staf1269.","ama":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? Monthly Notices of the Royal Astronomical Society. 2025;542(2):822-838. doi:10.1093/mnras/staf1269","chicago":"Sullivan, James, Zoltán Haiman, Mihir Kulkarni, and Eli Visbal. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1269.","ieee":"J. Sullivan, Z. Haiman, M. Kulkarni, and E. Visbal, “Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?,” Monthly Notices of the Royal Astronomical Society, vol. 542, no. 2. Oxford University Press, pp. 822–838, 2025.","short":"J. Sullivan, Z. Haiman, M. Kulkarni, E. Visbal, Monthly Notices of the Royal Astronomical Society 542 (2025) 822–838.","apa":"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. Oxford University Press. https://doi.org/10.1093/mnras/staf1269","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."},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","month":"09","date_updated":"2025-09-30T14:28:05Z","file_date_updated":"2025-09-03T05:44:47Z","file":[{"creator":"dernst","success":1,"date_created":"2025-09-03T05:44:47Z","checksum":"2a06796b27da0b33d479dba170ba4b3f","access_level":"open_access","file_size":2780496,"date_updated":"2025-09-03T05:44:47Z","content_type":"application/pdf","file_id":"20279","relation":"main_file","file_name":"2025_MonthlyNoticesRAS_Sullivan.pdf"}],"isi":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","volume":542,"year":"2025","publication_status":"published","_id":"20250","oa_version":"Published Version","article_type":"original","page":"822-838","oa":1,"author":[{"first_name":"James","last_name":"Sullivan","full_name":"Sullivan, James"},{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"first_name":"Mihir","last_name":"Kulkarni","full_name":"Kulkarni, Mihir"},{"first_name":"Eli","last_name":"Visbal","full_name":"Visbal, Eli"}],"external_id":{"isi":["001553472000001"],"arxiv":["2501.12986"]},"abstract":[{"lang":"eng","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."}],"PlanS_conform":"1","department":[{"_id":"ZoHa"}]},{"isi":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_name":"2025_MonthlyNoticesRAS_Xing.pdf","file_size":2974244,"date_updated":"2025-12-30T07:24:34Z","file_id":"20881","content_type":"application/pdf","relation":"main_file","access_level":"open_access","creator":"dernst","success":1,"date_created":"2025-12-30T07:24:34Z","checksum":"49fb4fe69f487d36169ccea60acbeccc"}],"publication_status":"published","year":"2025","volume":537,"date_updated":"2025-12-30T07:25:37Z","file_date_updated":"2025-12-30T07:24:34Z","abstract":[{"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.","lang":"eng"}],"author":[{"first_name":"Zepei","last_name":"Xing","full_name":"Xing, Zepei"},{"orcid":"0000-0002-3150-8988","full_name":"Torres Rodriguez, Santiago","id":"a8df4360-4328-11ee-8f1a-e502d0c83fc2","first_name":"Santiago","last_name":"Torres Rodriguez"},{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"Alessandro A.","last_name":"Trani","full_name":"Trani, Alessandro A."},{"last_name":"Korol","first_name":"Valeriya","full_name":"Korol, Valeriya"},{"full_name":"Cuadra, Jorge","last_name":"Cuadra","first_name":"Jorge"}],"external_id":{"arxiv":["2410.19695"],"isi":["001400731500001"]},"department":[{"_id":"YlGo"},{"_id":"LiBu"}],"PlanS_conform":"1","oa_version":"Published Version","project":[{"name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","grant_number":"101034413","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"_id":"18984","ec_funded":1,"oa":1,"page":"285-292","article_type":"original","doi":"10.1093/mnras/stae2820","date_created":"2025-02-02T23:01:53Z","arxiv":1,"has_accepted_license":"1","status":"public","day":"01","type":"journal_article","DOAJ_listed":"1","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.","OA_type":"gold","issue":"1","title":"Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries","ddc":["520"],"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"article_processing_charge":"Yes","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","month":"02","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":" 537","date_published":"2025-02-01T00:00:00Z","citation":{"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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/stae2820.","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,” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 1. Oxford University Press, pp. 285–292, 2025.","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. Monthly Notices of the Royal Astronomical Society. 2025;537(1):285-292. doi:10.1093/mnras/stae2820","mla":"Xing, Zepei, et al. “Combining REBOUND and MESA: Dynamical Evolution of Planets Orbiting Interacting Binaries.” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 1, Oxford University Press, 2025, pp. 285–92, doi:10.1093/mnras/stae2820.","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.","apa":"Xing, Z., Torres Rodriguez, S., Götberg, Y. L. L., Trani, A. A., Korol, V., & Cuadra, J. (2025). Combining REBOUND and MESA: Dynamical evolution of planets orbiting interacting binaries. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stae2820","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."}},{"file_date_updated":"2025-02-25T06:38:43Z","date_updated":"2026-02-16T11:51:48Z","publication_status":"published","year":"2025","volume":537,"isi":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"access_level":"open_access","creator":"dernst","success":1,"date_created":"2025-02-25T06:38:43Z","checksum":"431aef05755e6b5472f5e9b4c326cf84","file_name":"2025_MonthlyNoticesRAS_Claeyssens.pdf","date_updated":"2025-02-25T06:38:43Z","file_size":35099276,"content_type":"application/pdf","file_id":"19084","relation":"main_file"}],"oa":1,"article_type":"original","page":"2535-2558","oa_version":"Published Version","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"_id":"19066","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"abstract":[{"text":"We present a sample of 1956 individual stellar clumps at redshift 0.7 < z < 10, detected with JWST/NIRCam in 476 galaxies lensed by the galaxy cluster Abell2744. The lensed clumps present magnifications ranging between μ = 1.8 and μ = 300. We perform simultaneous size-photometry estimates in 20 JWST/NIRCam median and broad-band filters from 0.7 to 5 μm.\r\nSpectral energy distribution (SED) fitting analyses enable us to recover the physical properties of the clumps. The majority of the clumps are spatially resolved and have effective radii in the range Reff = 10–700 pc. We restrict this first study to the 1751 post-reionization era clumps with redshift < 5.5. We find a significant evolution of the average clump ages, star formation rates (SFRs), SFR surface densities, and metallicity with increasing redshift, while median stellar mass and stellar mass surface densities are similar in the probed redshift range. We observe a strong correlation between the clump properties and the properties of their host galaxies, with more massive galaxies hosting more massive and older clumps. We find that clumps closer to their host galactic centre are on average more massive, while their ages do not show clear sign of migration. We find that clumps at cosmic noon sample the upper-mass end of the mass function to higher masses than at z > 3, reflecting the rapid increase towards the peak of the cosmic star formation history. We conclude that the results achieved over the studied redshift range are in agreement with expectation of in situ clump formation scenario from large-scale disc fragmentation. ","lang":"eng"}],"author":[{"full_name":"Claeyssens, Adélaïde","first_name":"Adélaïde","last_name":"Claeyssens"},{"full_name":"Adamo, Angela","first_name":"Angela","last_name":"Adamo"},{"last_name":"Messa","first_name":"Matteo","full_name":"Messa, Matteo"},{"full_name":"Dessauges-Zavadsky, Miroslava","last_name":"Dessauges-Zavadsky","first_name":"Miroslava"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan"},{"last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"Rohan P.","last_name":"Naidu","full_name":"Naidu, Rohan P."}],"external_id":{"isi":["001420026000001"],"arxiv":["2410.10974"]},"ddc":["520"],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","OA_type":"gold","issue":"3","title":"Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744","type":"journal_article","day":"01","DOAJ_listed":"1","acknowledgement":"The authors thank the International Space Science Institute for sponsoring the ISSI team: ‘Star Formation within rapidly evolving galaxies’ where many ideas discussed in this article have been brainstormed. AA and AC acknowledge support by the Swedish research council Vetenskapsrådet (2021-05559). MM acknowledges the financial support through grant PRIN-MIUR 2020SKSTHZ. JM and IK acknowledge support by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. RPN acknowledges funding from JWST programme GO-3516. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","date_created":"2025-02-23T23:01:55Z","arxiv":1,"doi":"10.1093/mnras/staf058","status":"public","has_accepted_license":"1","date_published":"2025-03-01T00:00:00Z","citation":{"mla":"Claeyssens, Adélaïde, et al. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 3, Oxford University Press, 2025, pp. 2535–58, doi:10.1093/mnras/staf058.","ieee":"A. Claeyssens et al., “Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744,” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 3. Oxford University Press, pp. 2535–2558, 2025.","chicago":"Claeyssens, Adélaïde, Angela Adamo, Matteo Messa, Miroslava Dessauges-Zavadsky, Johan Richard, Ivan Kramarenko, Jorryt J Matthee, and Rohan P. Naidu. “Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field Abell 2744.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf058.","ama":"Claeyssens A, Adamo A, Messa M, et al. Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. 2025;537(3):2535-2558. doi:10.1093/mnras/staf058","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.","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.","apa":"Claeyssens, A., Adamo, A., Messa, M., Dessauges-Zavadsky, M., Richard, J., Kramarenko, I., … Naidu, R. P. (2025). Tracing star formation across cosmic time at tens of parsec-scales in the lensing cluster field Abell 2744. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf058"},"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":" 537","month":"03","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","article_processing_charge":"No","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society"},{"date_updated":"2025-12-01T15:07:43Z","file_date_updated":"2025-10-27T09:06:51Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","isi":1,"file":[{"access_level":"open_access","date_created":"2025-10-27T09:06:51Z","checksum":"d3190e974ce771e96c4c16ee98abb82a","creator":"dernst","success":1,"file_name":"2025_MonthlyNoticesRAS_Komori.pdf","content_type":"application/pdf","file_id":"20549","relation":"main_file","file_size":4864160,"date_updated":"2025-10-27T09:06:51Z"}],"publication_status":"published","volume":543,"year":"2025","oa_version":"Published Version","_id":"20545","oa":1,"page":"2943-2957","article_type":"original","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."}],"author":[{"full_name":"Komori, Fuga","first_name":"Fuga","last_name":"Komori"},{"last_name":"Inoue","first_name":"Akio K","full_name":"Inoue, Akio K"},{"first_name":"Ken","last_name":"Mawatari","full_name":"Mawatari, Ken"},{"full_name":"Sugahara, Yuma","last_name":"Sugahara","first_name":"Yuma"},{"full_name":"Umehata, Hideki","first_name":"Hideki","last_name":"Umehata"},{"full_name":"Shimakawa, Rhythm","first_name":"Rhythm","last_name":"Shimakawa"},{"full_name":"Yamanaka, Satoshi","last_name":"Yamanaka","first_name":"Satoshi"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee"},{"first_name":"Toru","last_name":"Misawa","full_name":"Misawa, Toru"}],"external_id":{"isi":["001592326700001"]},"department":[{"_id":"JoMa"}],"PlanS_conform":"1","OA_type":"gold","title":"The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy","issue":"3","ddc":["520"],"scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"doi":"10.1093/mnras/staf1622","date_created":"2025-10-27T08:18:07Z","status":"public","has_accepted_license":"1","type":"journal_article","day":"25","DOAJ_listed":"1","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.","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":" 543","date_published":"2025-09-25T00:00:00Z","citation":{"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.” Monthly Notices of the Royal Astronomical Society, vol. 543, no. 3, Oxford University Press, 2025, pp. 2943–57, doi:10.1093/mnras/staf1622.","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. Monthly Notices of the Royal Astronomical Society. 2025;543(3):2943-2957. doi:10.1093/mnras/staf1622","ieee":"F. Komori et al., “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, vol. 543, no. 3. Oxford University Press, pp. 2943–2957, 2025.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1622.","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.","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.","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1622"},"article_processing_charge":"Yes","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","month":"09","language":[{"iso":"eng"}],"publisher":"Oxford University Press","OA_place":"publisher"},{"OA_type":"gold","title":"The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization","issue":"2","ddc":["520"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","has_accepted_license":"1","status":"public","date_created":"2025-11-23T23:01:37Z","doi":"10.1093/mnras/staf1725","DOAJ_listed":"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.","type":"journal_article","day":"01","intvolume":" 544","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-12-01T00:00:00Z","citation":{"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.","apa":"Stephenson, H. M. O., Stott, J. P., Pirie, C. A., Duncan, K. J., Mcleod, D. J., Best, P. N., … Swinbank, A. M. (2025). The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1725","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.","mla":"Stephenson, H. M. O., et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2, Oxford University Press, 2025, pp. 1412–31, doi:10.1093/mnras/staf1725.","chicago":"Stephenson, H. M.O., J. P. Stott, C. A. Pirie, K. J. Duncan, D. J. Mcleod, P. N. Best, M. Brinch, et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1725.","ieee":"H. M. O. Stephenson et al., “The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization,” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2. Oxford University Press, pp. 1412–1431, 2025.","ama":"Stephenson HMO, Stott JP, Pirie CA, et al. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 2025;544(2):1412-1431. doi:10.1093/mnras/staf1725"},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","month":"12","date_updated":"2025-12-01T15:25:11Z","file_date_updated":"2025-11-24T10:35:15Z","file":[{"file_name":"2025_MonthlyNoticesRAS_Stephenson.pdf","relation":"main_file","file_id":"20678","content_type":"application/pdf","date_updated":"2025-11-24T10:35:15Z","file_size":3625308,"access_level":"open_access","checksum":"ddb3f429d2246bbf536efb4b0e52f3a8","date_created":"2025-11-24T10:35:15Z","success":1,"creator":"dernst"}],"isi":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":544,"year":"2025","publication_status":"published","_id":"20660","oa_version":"Published Version","article_type":"original","page":"1412-1431","oa":1,"author":[{"full_name":"Stephenson, H. M.O.","last_name":"Stephenson","first_name":"H. M.O."},{"last_name":"Stott","first_name":"J. P.","full_name":"Stott, J. P."},{"full_name":"Pirie, C. A.","first_name":"C. A.","last_name":"Pirie"},{"first_name":"K. J.","last_name":"Duncan","full_name":"Duncan, K. J."},{"full_name":"Mcleod, D. J.","first_name":"D. J.","last_name":"Mcleod"},{"full_name":"Best, P. N.","first_name":"P. N.","last_name":"Best"},{"last_name":"Brinch","first_name":"M.","full_name":"Brinch, M."},{"last_name":"Clausen","first_name":"M.","full_name":"Clausen, M."},{"first_name":"R. K.","last_name":"Cochrane","full_name":"Cochrane, R. K."},{"full_name":"Dunlop, J. S.","first_name":"J. S.","last_name":"Dunlop"},{"last_name":"Flury","first_name":"S. R.","full_name":"Flury, S. R."},{"full_name":"Geach, J. E.","first_name":"J. E.","last_name":"Geach"},{"last_name":"Hale","first_name":"C. L.","full_name":"Hale, C. L."},{"full_name":"Ibar, E.","last_name":"Ibar","first_name":"E."},{"last_name":"Li","first_name":"Zefeng","full_name":"Li, Zefeng"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"R. J.","last_name":"Mclure","full_name":"Mclure, R. J."},{"full_name":"Ossa-Fuentes, L.","last_name":"Ossa-Fuentes","first_name":"L."},{"first_name":"A. L.","last_name":"Patrick","full_name":"Patrick, A. L."},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"first_name":"A. M.","last_name":"Swinbank","full_name":"Swinbank, A. M."}],"external_id":{"isi":["001611415800001"]},"abstract":[{"lang":"eng","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."}],"PlanS_conform":"1","department":[{"_id":"JoMa"}]},{"department":[{"_id":"JoMa"}],"PlanS_conform":"1","abstract":[{"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.","lang":"eng"}],"author":[{"full_name":"Dalmasso, Nicolò","first_name":"Nicolò","last_name":"Dalmasso"},{"last_name":"Watson","first_name":"Peter J.","full_name":"Watson, Peter J."},{"last_name":"Treu","first_name":"Tommaso","full_name":"Treu, Tommaso"},{"last_name":"Trenti","first_name":"Michele","full_name":"Trenti, Michele"},{"first_name":"Benedetta","last_name":"Vulcani","full_name":"Vulcani, Benedetta"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"last_name":"Bradač","first_name":"Maruša","full_name":"Bradač, Maruša"},{"last_name":"Jones","first_name":"Tucker","full_name":"Jones, Tucker"},{"first_name":"Kristan","last_name":"Boyett","full_name":"Boyett, Kristan"},{"first_name":"Xin","last_name":"Wang","full_name":"Wang, Xin"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara","last_name":"Mascia","first_name":"Sara"},{"full_name":"Pentericci, Laura","first_name":"Laura","last_name":"Pentericci"}],"external_id":{"isi":["001615620500001"],"arxiv":["2510.27036"]},"oa":1,"article_type":"original","page":"1915-1925","oa_version":"Published Version","_id":"20661","publication_status":"published","year":"2025","volume":544,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","isi":1,"file":[{"relation":"main_file","content_type":"application/pdf","file_id":"20674","file_size":1952887,"date_updated":"2025-11-24T09:02:04Z","file_name":"2025_MonthlyNoticesRAS_Dalmasso.pdf","checksum":"2caff0a3b81fed114408377323298b43","date_created":"2025-11-24T09:02:04Z","success":1,"creator":"dernst","access_level":"open_access"}],"file_date_updated":"2025-11-24T09:02:04Z","date_updated":"2025-12-01T15:23:21Z","month":"12","language":[{"iso":"eng"}],"publisher":"Oxford University Press","OA_place":"publisher","article_processing_charge":"Yes","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2025-12-01T00:00:00Z","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf1837","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.","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.","chicago":"Dalmasso, Nicolò, Peter J. Watson, Tommaso Treu, Michele Trenti, Benedetta Vulcani, Themiya Nanayakkara, Maruša Bradač, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1837.","ieee":"N. Dalmasso et al., “Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2. Oxford University Press, pp. 1915–1925, 2025.","ama":"Dalmasso N, Watson PJ, Treu T, et al. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. Monthly Notices of the Royal Astronomical Society. 2025;544(2):1915-1925. doi:10.1093/mnras/staf1837","mla":"Dalmasso, Nicolò, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” Monthly Notices of the Royal Astronomical Society, vol. 544, no. 2, Oxford University Press, 2025, pp. 1915–25, doi:10.1093/mnras/staf1837."},"tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"intvolume":" 544","type":"journal_article","day":"01","DOAJ_listed":"1","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. ","arxiv":1,"doi":"10.1093/mnras/staf1837","date_created":"2025-11-23T23:01:38Z","status":"public","has_accepted_license":"1","ddc":["520"],"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"OA_type":"gold","title":"Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies","issue":"2"},{"article_type":"original","page":"788-808","oa":1,"_id":"21063","oa_version":"Published Version","PlanS_conform":"1","department":[{"_id":"JoMa"}],"author":[{"last_name":"Herard-Demanche","first_name":"Thomas","full_name":"Herard-Demanche, Thomas"},{"last_name":"Bouwens","first_name":"Rychard J","full_name":"Bouwens, Rychard J"},{"full_name":"Oesch, Pascal A","last_name":"Oesch","first_name":"Pascal A"},{"first_name":"Rohan P","last_name":"Naidu","full_name":"Naidu, Rohan P"},{"full_name":"Decarli, Roberto","first_name":"Roberto","last_name":"Decarli"},{"full_name":"Nelson, Erica J","first_name":"Erica J","last_name":"Nelson"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Weibel, Andrea","last_name":"Weibel","first_name":"Andrea"},{"last_name":"Xiao","first_name":"Mengyuan","full_name":"Xiao, Mengyuan"},{"last_name":"Stefanon","first_name":"Mauro","full_name":"Stefanon, Mauro"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Meyer","first_name":"Romain A","full_name":"Meyer, Romain A"},{"last_name":"Wuyts","first_name":"Stijn","full_name":"Wuyts, Stijn"},{"last_name":"Reddy","first_name":"Naveen","full_name":"Reddy, Naveen"},{"full_name":"Rowland, Lucie","first_name":"Lucie","last_name":"Rowland"},{"last_name":"van Leeuwen","first_name":"Ivana","full_name":"van Leeuwen, Ivana"},{"first_name":"Pablo Arrabal","last_name":"Haro","full_name":"Haro, Pablo Arrabal"},{"full_name":"Dannerbauer, Helmut","first_name":"Helmut","last_name":"Dannerbauer"},{"first_name":"Alice E","last_name":"Shapley","full_name":"Shapley, Alice E"},{"full_name":"Chisholm, John","first_name":"John","last_name":"Chisholm"},{"last_name":"van Dokkum","first_name":"Pieter","full_name":"van Dokkum, Pieter"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"first_name":"Garth","last_name":"Illingworth","full_name":"Illingworth, Garth"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"first_name":"Irene","last_name":"Shivaei","full_name":"Shivaei, Irene"}],"external_id":{"arxiv":["2309.04525"]},"abstract":[{"lang":"eng","text":"We report the detection of a 13σ Hα emission line from HDF850.1 at z = 5.188 ± 0.001 using the FRESCO (First Reionization Era SpectroscopicallyComplete Observations) NIRCam F444W grism observations. Detection of Hα in HDF850.1 is noteworthy, given its high far-infrared (IR) luminosity, substantial dust obscuration, and the historical challenges in deriving its redshift.\r\nHDF850.1 shows a clear detection in the F444W imaging data, distributed between a northern and southern component, mirroring that seen in [C II] from the Plateau de Bure Interferometer. Modelling the spectral energy distribution of each component separately, we find that the northern component has a higher mass, star formation rate (SFR), and dust extinction than the southern component. The observed Hα emission appears to arise entirely from the less-obscured southern component and shows a similar \u0004v∼ + 130 km s −1 velocity offset to that seen for [C II] relative to the source systemic redshift. Leveraging Hα-derived redshiftsfrom FRESCO observations, we find that HDF850.1 isforming in one of the richest environments identified to date at z > 5, with 100 z = 5.17–5.20 galaxies distributed across 13 smaller structures and a ∼(15 cMpc)3 volume. Based on the evolution of analogous structures in cosmological simulations, the z = 5.17–5.20 structures seem likely to collapse into\r\na single > 1014M cluster by z ∼ 0. Comparing galaxy properties forming within this overdensity with those outside, we find the masses, SFRs, and UV luminosities inside the overdensity to be clearly higher. The prominence of Hα line emission from HDF850.1 and other known highly obscured z > 5 galaxies illustrates the potential of NIRCam-grism programs to map both\r\nthe early build-up of IR-luminous galaxies and overdense structures."}],"file_date_updated":"2026-02-09T08:39:19Z","date_updated":"2026-02-09T08:50:55Z","volume":537,"year":"2025","publication_status":"published","file":[{"file_name":"2025_MonthlyNoticesRAS_HerardDemanche.pdf","date_updated":"2026-02-09T08:39:19Z","file_size":2787493,"relation":"main_file","file_id":"21169","content_type":"application/pdf","access_level":"open_access","success":1,"creator":"dernst","checksum":"4cbade43244eaa8b60bb05a90ae613da","date_created":"2026-02-09T08:39:19Z"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2025-02-01T00:00:00Z","citation":{"ista":"Herard-Demanche T, Bouwens RJ, Oesch PA, Naidu RP, Decarli R, Nelson EJ, Brammer G, Weibel A, Xiao M, Stefanon M, Walter F, Matthee JJ, Meyer RA, Wuyts S, Reddy N, Rowland L, van Leeuwen I, Haro PA, Dannerbauer H, Shapley AE, Chisholm J, van Dokkum P, Labbe I, Illingworth G, Schaerer D, Shivaei I. 2025. Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. 537(2), 788–808.","apa":"Herard-Demanche, T., Bouwens, R. J., Oesch, P. A., Naidu, R. P., Decarli, R., Nelson, E. J., … Shivaei, I. (2025). Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf030","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.","ama":"Herard-Demanche T, Bouwens RJ, Oesch PA, et al. Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures. Monthly Notices of the Royal Astronomical Society. 2025;537(2):788-808. doi:10.1093/mnras/staf030","chicago":"Herard-Demanche, Thomas, Rychard J Bouwens, Pascal A Oesch, Rohan P Naidu, Roberto Decarli, Erica J Nelson, Gabriel Brammer, et al. “Mapping Dusty Galaxy Growth at z > 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf030.","ieee":"T. Herard-Demanche et al., “Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures,” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 2. Oxford University Press, pp. 788–808, 2025.","mla":"Herard-Demanche, Thomas, et al. “Mapping Dusty Galaxy Growth at z > 5 with FRESCO: Detection of Hα in Submm Galaxy HDF850.1 and the Surrounding Overdense Structures.” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 2, Oxford University Press, 2025, pp. 788–808, doi:10.1093/mnras/staf030."},"intvolume":" 537","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"language":[{"iso":"eng"}],"OA_place":"publisher","publisher":"Oxford University Press","month":"02","publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","ddc":["520"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"OA_type":"gold","issue":"2","title":"Mapping dusty galaxy growth at z > 5 with FRESCO: Detection of Hα in submm galaxy HDF850.1 and the surrounding overdense structures","DOAJ_listed":"1","acknowledgement":"We are grateful to Roberto Neri and collaborators for providing us with spatially resolved information on both the dust-continuum and [C ii] line emission from their high spatial resolution PdBI observations. This project was made possible in part by the Leiden University Fund/Bouwens Astrophysics Fund. RJB acknowledges support from NWO grants 600.065.140.11N211 (vrij competitie) and TOP grant TOP1.16.057. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. Support for this work was provided by NASA through grant JWST-GO-01895 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. RPN acknowledges funding from JWST programs GO-1933 and GO-2279. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the CIDEGENT/2021/059 grant, from project PID2019-109592GB-I00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación. This study forms part of the Astrophysics and High Energy Physics programme and was supported by MCIN with funding from European Union NextGenerationEU (PRTR-C17.I1) and by Generalitat Valenciana under the project n. ASFAE/2022/025. RAM acknowledges support from the ERC Advanced Grant 740246 (Cosmic_Gas) and the Swiss National Science Foundation through project grant 200020_207349.\r\n\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–03127 for JWST. These observations are associated with program no. 1895.\r\n\r\nThis paper made use of several publicly available software packages. We are indebted to the respective authors for their work: ipython (Pérez & Granger 2007), matplotlib (Hunter 2007), numpy (Oliphant 2006), scipy (Virtanen et al. 2020), jupyter (Kluyver et al. 2016), astropy (Astropy Collaboration 2013, 2018), grizli (v1.7.11; Brammer 2018; Brammer et al. 2022), eazy (Brammer, van Dokkum & Coppi 2008), and SExtractor (Bertin & Arnouts 1996).","day":"01","type":"journal_article","has_accepted_license":"1","status":"public","doi":"10.1093/mnras/staf030","arxiv":1,"date_created":"2026-01-28T15:25:53Z"},{"OA_type":"gold","issue":"3","title":"Thermal X-ray signatures in late-stage unequal-mass massive black hole binary mergers","ddc":["520"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"has_accepted_license":"1","status":"public","date_created":"2026-01-31T09:28:28Z","arxiv":1,"doi":"10.1093/mnras/staf1583","DOAJ_listed":"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).","type":"journal_article","day":"01","intvolume":" 543","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2025-11-01T00:00:00Z","citation":{"mla":"Krauth, Luke Major, et al. “Thermal X-Ray Signatures in Late-Stage Unequal-Mass Massive Black Hole Binary Mergers.” Monthly Notices of the Royal Astronomical Society, vol. 543, no. 3, Oxford University Press, 2025, pp. 2670–85, doi:10.1093/mnras/staf1583.","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,” Monthly Notices of the Royal Astronomical Society, vol. 543, no. 3. Oxford University Press, pp. 2670–2685, 2025.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf1583.","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. Monthly Notices of the Royal Astronomical Society. 2025;543(3):2670-2685. doi:10.1093/mnras/staf1583","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.","apa":"Krauth, L. M., Davelaar, J., Haiman, Z., Westernacher-Schneider, J. R., 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. Oxford University Press. https://doi.org/10.1093/mnras/staf1583","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."},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"Yes","quality_controlled":"1","language":[{"iso":"eng"}],"publisher":"Oxford University Press","OA_place":"publisher","month":"11","date_updated":"2026-02-10T07:10:21Z","file_date_updated":"2026-02-10T07:07:17Z","file":[{"access_level":"open_access","creator":"dernst","success":1,"date_created":"2026-02-10T07:07:17Z","checksum":"f9b4c6a606df9493f6eb6af5ebcca6db","file_name":"2025_MonthlyNoticesRAS_Krauth.pdf","date_updated":"2026-02-10T07:07:17Z","file_size":3689696,"file_id":"21203","content_type":"application/pdf","relation":"main_file"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":543,"year":"2025","publication_status":"published","_id":"21122","oa_version":"Published Version","article_type":"original","page":"2670-2685","oa":1,"author":[{"full_name":"Krauth, Luke Major","last_name":"Krauth","first_name":"Luke Major"},{"last_name":"Davelaar","first_name":"Jordy","full_name":"Davelaar, Jordy"},{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"full_name":"Westernacher-Schneider, John Ryan","last_name":"Westernacher-Schneider","first_name":"John Ryan"},{"last_name":"Zrake","first_name":"Jonathan","full_name":"Zrake, Jonathan"},{"last_name":"MacFadyen","first_name":"Andrew","full_name":"MacFadyen, Andrew"}],"external_id":{"arxiv":["2503.01494"]},"abstract":[{"lang":"eng","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."}],"PlanS_conform":"1","department":[{"_id":"ZoHa"}]},{"_id":"21127","oa_version":"Published Version","article_type":"original","page":"11-30","oa":1,"external_id":{"arxiv":["2409.12250"]},"author":[{"full_name":"Su, Kung-Yi","last_name":"Su","first_name":"Kung-Yi"},{"full_name":"Bryan, Greg L","first_name":"Greg L","last_name":"Bryan"},{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"}],"extern":"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."}],"PlanS_conform":"1","date_updated":"2026-02-10T08:36:54Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2025","volume":538,"publication_status":"published","intvolume":" 538","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"citation":{"mla":"Su, Kung-Yi, et al. “Self-Regulation of High-Redshift Black Hole Accretion via Jets: Challenges for SMBH Formation.” Monthly Notices of the Royal Astronomical Society, vol. 538, no. 1, Oxford University Press, 2025, pp. 11–30, doi:10.1093/mnras/staf228.","ama":"Su K-Y, Bryan GL, Haiman Z. Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation. Monthly Notices of the Royal Astronomical Society. 2025;538(1):11-30. doi:10.1093/mnras/staf228","ieee":"K.-Y. Su, G. L. Bryan, and Z. Haiman, “Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation,” Monthly Notices of the Royal Astronomical Society, vol. 538, no. 1. Oxford University Press, pp. 11–30, 2025.","chicago":"Su, Kung-Yi, Greg L Bryan, and Zoltán Haiman. “Self-Regulation of High-Redshift Black Hole Accretion via Jets: Challenges for SMBH Formation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf228.","short":"K.-Y. Su, G.L. Bryan, Z. Haiman, Monthly Notices of the Royal Astronomical Society 538 (2025) 11–30.","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.","apa":"Su, K.-Y., Bryan, G. L., & Haiman, Z. (2025). Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staf228"},"date_published":"2025-03-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","OA_place":"publisher","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"03","title":"Self-regulation of high-redshift black hole accretion via jets: Challenges for SMBH formation","issue":"1","OA_type":"gold","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"ddc":["520"],"has_accepted_license":"1","status":"public","doi":"10.1093/mnras/staf228","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staf228","open_access":"1"}],"date_created":"2026-01-31T09:29:59Z","DOAJ_listed":"1","day":"01","type":"journal_article"},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"ddc":["520"],"title":"Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes","issue":"4","OA_type":"gold","DOAJ_listed":"1","day":"01","type":"journal_article","status":"public","has_accepted_license":"1","main_file_link":[{"url":"https://doi.org/10.1093/mnras/staf237","open_access":"1"}],"arxiv":1,"doi":"10.1093/mnras/staf237","date_created":"2026-01-31T09:30:19Z","citation":{"short":"M. Epstein-Martin, H. Tagawa, Z. Haiman, R. Perna, Monthly Notices of the Royal Astronomical Society 537 (2025) 3396–3420.","apa":"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. Oxford University Press. https://doi.org/10.1093/mnras/staf237","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.","mla":"Epstein-Martin, Marguerite, et al. “Time-Dependent Models of AGN Discs with Radiation from Embedded Stellar-Mass Black Holes.” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 4, Oxford University Press, 2025, pp. 3396–420, doi:10.1093/mnras/staf237.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2025. https://doi.org/10.1093/mnras/staf237.","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,” Monthly Notices of the Royal Astronomical Society, vol. 537, no. 4. Oxford University Press, pp. 3396–3420, 2025.","ama":"Epstein-Martin M, Tagawa H, Haiman Z, Perna R. Time-dependent models of AGN discs with radiation from embedded stellar-mass black holes. Monthly Notices of the Royal Astronomical Society. 2025;537(4):3396-3420. doi:10.1093/mnras/staf237"},"date_published":"2025-03-01T00:00:00Z","intvolume":" 537","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"OA_place":"publisher","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"03","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","article_processing_charge":"Yes","date_updated":"2026-02-10T09:00:44Z","volume":537,"year":"2025","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_type":"original","page":"3396-3420","oa":1,"_id":"21128","oa_version":"Published Version","PlanS_conform":"1","external_id":{"arxiv":["2405.09380"]},"author":[{"full_name":"Epstein-Martin, Marguerite","first_name":"Marguerite","last_name":"Epstein-Martin"},{"full_name":"Tagawa, Hiromichi","last_name":"Tagawa","first_name":"Hiromichi"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Perna, Rosalba","last_name":"Perna","first_name":"Rosalba"}],"abstract":[{"lang":"eng","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."}],"extern":"1"}]