[{"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","language":[{"iso":"eng"}],"issue":"2","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.","file":[{"file_id":"20063","relation":"main_file","file_size":4451937,"creator":"dernst","success":1,"access_level":"open_access","date_updated":"2025-07-22T07:02:02Z","content_type":"application/pdf","checksum":"abedbbce98d448f374dc922dad9133fc","file_name":"2025_MonthlyNoticesRAS_Duncan.pdf","date_created":"2025-07-22T07:02:02Z"}],"file_date_updated":"2025-07-22T07:02:02Z","citation":{"apa":"Duncan, K. J., Mcleod, D. J., Best, P. N., Pirie, C. A., Clausen, M., Cochrane, R. K., … Swinbank, A. M. (2025). The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1061\">https://doi.org/10.1093/mnras/staf1061</a>","short":"K.J. Duncan, D.J. Mcleod, P.N. Best, C.A. Pirie, M. Clausen, R.K. Cochrane, J.S. Dunlop, S.R. Flury, J.E. Geach, N.A. Grogin, C.L. Hale, E. Ibar, R. Kondapally, Z. Li, J.J. Matthee, R.J. Mclure, L. Ossa-Fuentes, A.L. Patrick, I. Smail, D. Sobral, H.M.O. Stephenson, J.P. Stott, A.M. Swinbank, Monthly Notices of the Royal Astronomical Society 541 (2025) 1329–1347.","ieee":"K. J. Duncan <i>et al.</i>, “The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2. Oxford University Press, pp. 1329–1347, 2025.","chicago":"Duncan, K. J., D. J. Mcleod, P. N. Best, C. A. Pirie, M. Clausen, R. K. Cochrane, J. S. Dunlop, et al. “The JWST Emission-Line Survey: Extending Rest-Optical Narrow-Band Emission-Line Selection into the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1061\">https://doi.org/10.1093/mnras/staf1061</a>.","ama":"Duncan KJ, Mcleod DJ, Best PN, et al. The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;541(2):1329-1347. doi:<a href=\"https://doi.org/10.1093/mnras/staf1061\">10.1093/mnras/staf1061</a>","ista":"Duncan KJ, Mcleod DJ, Best PN, Pirie CA, Clausen M, Cochrane RK, Dunlop JS, Flury SR, Geach JE, Grogin NA, Hale CL, Ibar E, Kondapally R, Li Z, Matthee JJ, Mclure RJ, Ossa-Fuentes L, Patrick AL, Smail I, Sobral D, Stephenson HMO, Stott JP, Swinbank AM. 2025. The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization. Monthly Notices of the Royal Astronomical Society. 541(2), 1329–1347.","mla":"Duncan, K. J., et al. “The JWST Emission-Line Survey: Extending Rest-Optical Narrow-Band Emission-Line Selection into the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 541, no. 2, Oxford University Press, 2025, pp. 1329–47, doi:<a href=\"https://doi.org/10.1093/mnras/staf1061\">10.1093/mnras/staf1061</a>."},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":541,"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."}],"day":"01","article_type":"original","scopus_import":"1","license":"https://creativecommons.org/licenses/by/4.0/","publication":"Monthly Notices of the Royal Astronomical Society","ddc":["520"],"page":"1329-1347","type":"journal_article","date_published":"2025-08-01T00:00:00Z","DOAJ_listed":"1","arxiv":1,"fulldoi":"https://doi.org/10.1093/mnras/staf1061","OA_type":"gold","department":[{"_id":"JoMa"}],"article_processing_charge":"Yes","month":"08","OA_place":"publisher","publication_status":"published","date_created":"2025-07-20T22:02:00Z","external_id":{"arxiv":["2410.09000"],"isi":["001527085900001"]},"_id":"20028","PlanS_conform":"1","isi":1,"doi":"10.1093/mnras/staf1061","title":"The JWST Emission-Line Survey: Extending rest-optical narrow-band emission-line selection into the Epoch of Reionization","year":"2025","date_updated":"2025-09-30T14:03:01Z","quality_controlled":"1","status":"public","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publisher":"Oxford University Press","intvolume":"       541","author":[{"full_name":"Duncan, K. J.","last_name":"Duncan","first_name":"K. J."},{"last_name":"Mcleod","full_name":"Mcleod, D. J.","first_name":"D. J."},{"last_name":"Best","full_name":"Best, P. N.","first_name":"P. N."},{"first_name":"C. A.","full_name":"Pirie, C. A.","last_name":"Pirie"},{"first_name":"M.","last_name":"Clausen","full_name":"Clausen, M."},{"first_name":"R. K.","full_name":"Cochrane, R. K.","last_name":"Cochrane"},{"full_name":"Dunlop, J. S.","last_name":"Dunlop","first_name":"J. S."},{"first_name":"S. R.","full_name":"Flury, S. R.","last_name":"Flury"},{"last_name":"Geach","full_name":"Geach, J. E.","first_name":"J. E."},{"first_name":"N. A.","last_name":"Grogin","full_name":"Grogin, N. A."},{"last_name":"Hale","full_name":"Hale, C. L.","first_name":"C. L."},{"first_name":"E.","last_name":"Ibar","full_name":"Ibar, E."},{"full_name":"Kondapally, R.","last_name":"Kondapally","first_name":"R."},{"first_name":"Zefeng","last_name":"Li","full_name":"Li, Zefeng"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"R. J.","last_name":"Mclure","full_name":"Mclure, R. J."},{"full_name":"Ossa-Fuentes, Luis","last_name":"Ossa-Fuentes","first_name":"Luis"},{"last_name":"Patrick","full_name":"Patrick, A. L.","first_name":"A. L."},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"first_name":"H. M.O.","last_name":"Stephenson","full_name":"Stephenson, H. M.O."},{"last_name":"Stott","full_name":"Stott, J. P.","first_name":"J. P."},{"first_name":"A. M.","last_name":"Swinbank","full_name":"Swinbank, A. M."}],"oa":1},{"arxiv":1,"type":"journal_article","date_published":"2025-09-01T00:00:00Z","DOAJ_listed":"1","fulldoi":"https://doi.org/10.1093/mnras/staf1269","publication_status":"published","department":[{"_id":"ZoHa"}],"OA_type":"gold","OA_place":"publisher","article_processing_charge":"Yes","month":"09","external_id":{"isi":["001553472000001"],"arxiv":["2501.12986"]},"date_created":"2025-08-31T22:01:31Z","PlanS_conform":"1","_id":"20250","isi":1,"quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","status":"public","has_accepted_license":"1","doi":"10.1093/mnras/staf1269","date_updated":"2025-09-30T14:28:05Z","year":"2025","title":"Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?","author":[{"last_name":"Sullivan","full_name":"Sullivan, James","first_name":"James"},{"orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"last_name":"Kulkarni","full_name":"Kulkarni, Mihir","first_name":"Mihir"},{"first_name":"Eli","full_name":"Visbal, Eli","last_name":"Visbal"}],"oa":1,"publisher":"Oxford University Press","intvolume":"       542","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","issue":"2","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.","language":[{"iso":"eng"}],"file_date_updated":"2025-09-03T05:44:47Z","file":[{"file_size":2780496,"relation":"main_file","file_id":"20279","creator":"dernst","access_level":"open_access","success":1,"date_updated":"2025-09-03T05:44:47Z","content_type":"application/pdf","file_name":"2025_MonthlyNoticesRAS_Sullivan.pdf","checksum":"2a06796b27da0b33d479dba170ba4b3f","date_created":"2025-09-03T05:44:47Z"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"ieee":"J. Sullivan, Z. Haiman, M. Kulkarni, and E. Visbal, “Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 542, no. 2. Oxford University Press, pp. 822–838, 2025.","chicago":"Sullivan, James, Zoltán Haiman, Mihir Kulkarni, and Eli Visbal. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1269\">https://doi.org/10.1093/mnras/staf1269</a>.","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., &#38; Visbal, E. (2025). Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1269\">https://doi.org/10.1093/mnras/staf1269</a>","mla":"Sullivan, James, et al. “Can Supermassive Stars Form in Protogalaxies Due to Internal Lyman-Werner Feedback?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 542, no. 2, Oxford University Press, 2025, pp. 822–38, doi:<a href=\"https://doi.org/10.1093/mnras/staf1269\">10.1093/mnras/staf1269</a>.","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.","ama":"Sullivan J, Haiman Z, Kulkarni M, Visbal E. Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback? <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;542(2):822-838. doi:<a href=\"https://doi.org/10.1093/mnras/staf1269\">10.1093/mnras/staf1269</a>"},"article_type":"original","day":"01","scopus_import":"1","volume":542,"abstract":[{"text":"Population III stars are possible precursors to early supermassive black holes (BHs). The presence of soft UV Lyman–Werner (LW) background radiation can suppress Population III star formation in minihaloes and allow them to form in pristine atomic-cooling haloes. In the absence of molecular hydrogen (⁠H2⁠) cooling, atomic-cooling haloes enable rapid collapse with suppressed fragmentation. High background LW fluxes from preceding star-formation have been proposed to dissociate H2⁠. This flux can be supplemented by LW radiation from one or more Population III star(s) in the same halo, reducing the necessary background level. Here, we consider atomic-cooling haloes in which multiple protostellar cores form close to one another nearly simultaneously. We assess whether the first star’s LW radiation can dissociate nearby \r\n⁠, enabling rapid accretion on to a nearby protostellar core, and the prompt formation of a second, supermassive star (SMS) from warm, atomically-cooled gas. We use a set of hydrodynamical simulations with the code enzo, with identical LW backgrounds centred on a halo with two adjacent collapsing gas clumps. When an additional large local LW flux is introduced, we observe immediate reductions in both the accretion rates and the stellar masses that form within these clumps. While the LW flux reduces the H2 fraction and increases the gas temperature, the halo core’s potential well is too shallow to promptly heat the gas to >1000 K and increase the second protostar’s accretion rate. We conclude that this internal LW feedback scenario is unlikely to facilitate SMS or massive BH seed formation.","lang":"eng"}],"page":"822-838","publication":"Monthly Notices of the Royal Astronomical Society","ddc":["520"]},{"isi":1,"_id":"20545","PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","status":"public","quality_controlled":"1","date_updated":"2025-12-01T15:07:43Z","year":"2025","title":"The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy","doi":"10.1093/mnras/staf1622","author":[{"full_name":"Komori, Fuga","last_name":"Komori","first_name":"Fuga"},{"first_name":"Akio K","full_name":"Inoue, Akio K","last_name":"Inoue"},{"first_name":"Ken","full_name":"Mawatari, Ken","last_name":"Mawatari"},{"first_name":"Yuma","full_name":"Sugahara, Yuma","last_name":"Sugahara"},{"full_name":"Umehata, Hideki","last_name":"Umehata","first_name":"Hideki"},{"last_name":"Shimakawa","full_name":"Shimakawa, Rhythm","first_name":"Rhythm"},{"full_name":"Yamanaka, Satoshi","last_name":"Yamanaka","first_name":"Satoshi"},{"first_name":"Takuya","last_name":"Hashimoto","full_name":"Hashimoto, Takuya"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Misawa","full_name":"Misawa, Toru","first_name":"Toru"}],"oa":1,"publisher":"Oxford University Press","intvolume":"       543","DOAJ_listed":"1","date_published":"2025-09-25T00:00:00Z","type":"journal_article","fulldoi":"https://doi.org/10.1093/mnras/staf1622","publication_status":"published","OA_place":"publisher","article_processing_charge":"Yes","month":"09","OA_type":"gold","department":[{"_id":"JoMa"}],"external_id":{"isi":["001592326700001"]},"date_created":"2025-10-27T08:18:07Z","scopus_import":"1","article_type":"original","day":"25","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."}],"volume":543,"page":"2943-2957","publication":"Monthly Notices of the Royal Astronomical Society","ddc":["520"],"oa_version":"Published Version","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"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.","issue":"3","language":[{"iso":"eng"}],"file_date_updated":"2025-10-27T09:06:51Z","file":[{"content_type":"application/pdf","date_created":"2025-10-27T09:06:51Z","file_name":"2025_MonthlyNoticesRAS_Komori.pdf","checksum":"d3190e974ce771e96c4c16ee98abb82a","creator":"dernst","file_size":4864160,"relation":"main_file","file_id":"20549","date_updated":"2025-10-27T09:06:51Z","access_level":"open_access","success":1}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"apa":"Komori, F., Inoue, A. K., Mawatari, K., Sugahara, Y., Umehata, H., Shimakawa, R., … Misawa, T. (2025). The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1622\">https://doi.org/10.1093/mnras/staf1622</a>","short":"F. Komori, A.K. Inoue, K. Mawatari, Y. Sugahara, H. Umehata, R. Shimakawa, S. Yamanaka, T. Hashimoto, J.J. Matthee, T. Misawa, Monthly Notices of the Royal Astronomical Society 543 (2025) 2943–2957.","chicago":"Komori, Fuga, Akio K Inoue, Ken Mawatari, Yuma Sugahara, Hideki Umehata, Rhythm Shimakawa, Satoshi Yamanaka, Takuya Hashimoto, Jorryt J Matthee, and Toru Misawa. “The First Direct Imaging of the Silhouette of a Damped Lyman α System along the Line-of-Sight to a Background Galaxy.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1622\">https://doi.org/10.1093/mnras/staf1622</a>.","ieee":"F. Komori <i>et al.</i>, “The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3. Oxford University Press, pp. 2943–2957, 2025.","ama":"Komori F, Inoue AK, Mawatari K, et al. The first direct imaging of the silhouette of a damped Lyman α system along the line-of-sight to a background galaxy. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;543(3):2943-2957. doi:<a href=\"https://doi.org/10.1093/mnras/staf1622\">10.1093/mnras/staf1622</a>","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.","mla":"Komori, Fuga, et al. “The First Direct Imaging of the Silhouette of a Damped Lyman α System along the Line-of-Sight to a Background Galaxy.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 543, no. 3, Oxford University Press, 2025, pp. 2943–57, doi:<a href=\"https://doi.org/10.1093/mnras/staf1622\">10.1093/mnras/staf1622</a>."}},{"intvolume":"       544","publisher":"Oxford University Press","oa":1,"author":[{"first_name":"H. M.O.","full_name":"Stephenson, H. M.O.","last_name":"Stephenson"},{"first_name":"J. P.","full_name":"Stott, J. P.","last_name":"Stott"},{"full_name":"Pirie, C. A.","last_name":"Pirie","first_name":"C. A."},{"first_name":"K. J.","full_name":"Duncan, K. J.","last_name":"Duncan"},{"full_name":"Mcleod, D. J.","last_name":"Mcleod","first_name":"D. J."},{"first_name":"P. N.","last_name":"Best","full_name":"Best, P. N."},{"first_name":"M.","last_name":"Brinch","full_name":"Brinch, M."},{"full_name":"Clausen, M.","last_name":"Clausen","first_name":"M."},{"last_name":"Cochrane","full_name":"Cochrane, R. K.","first_name":"R. K."},{"first_name":"J. S.","full_name":"Dunlop, J. S.","last_name":"Dunlop"},{"first_name":"S. R.","full_name":"Flury, S. R.","last_name":"Flury"},{"last_name":"Geach","full_name":"Geach, J. E.","first_name":"J. E."},{"last_name":"Hale","full_name":"Hale, C. L.","first_name":"C. L."},{"first_name":"E.","last_name":"Ibar","full_name":"Ibar, E."},{"first_name":"Zefeng","last_name":"Li","full_name":"Li, Zefeng"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Mclure","full_name":"Mclure, R. J.","first_name":"R. J."},{"full_name":"Ossa-Fuentes, L.","last_name":"Ossa-Fuentes","first_name":"L."},{"first_name":"A. L.","full_name":"Patrick, A. L.","last_name":"Patrick"},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"full_name":"Swinbank, A. M.","last_name":"Swinbank","first_name":"A. M."}],"isi":1,"_id":"20660","PlanS_conform":"1","title":"The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization","date_updated":"2025-12-01T15:25:11Z","year":"2025","doi":"10.1093/mnras/staf1725","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","has_accepted_license":"1","quality_controlled":"1","month":"12","article_processing_charge":"Yes","OA_place":"publisher","department":[{"_id":"JoMa"}],"OA_type":"gold","publication_status":"published","date_created":"2025-11-23T23:01:37Z","external_id":{"isi":["001611415800001"]},"DOAJ_listed":"1","type":"journal_article","date_published":"2025-12-01T00:00:00Z","fulldoi":"https://doi.org/10.1093/mnras/staf1725","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","page":"1412-1431","abstract":[{"text":"We used observations from the JWST Emission Line Survey (JELS) to measure the half-light radii (re) of 23 Hα-emitting starforming (SF) galaxies at z = 6.1 in the PRIMER/COSMOS field. Galaxy sizes were measured in JWST near-infrared camera observations in rest-frame Hα (tracing recent star formation) with the F466N and F470N narrow-band filters from JELS, and\r\ncompared against rest-R- and V -band (tracing established stellar populations) and near-ultraviolet sizes. We find a size–stellar mass(re − M∗) relationship with a slope that is consistent with literature values at lower redshifts, though offset to lowersizes. We observe a large scatter in re at low stellar mass (M∗ < 10^8.4 Mo) which we believe is the result of bursty star formation histories (SFHs) of SF galaxies at the Epoch of Reionization (EoR). We find that the stellar and ionized gas components are similar in size at z = 6.1. The evidence of already-established stellar components in these Hα emitters (HAEs) indicates previous episodes of star formation have occurred. As such, following other JELS studies finding our HAEs are undergoing a current burst of star formation, we believe our results indicate that SF galaxies at the end of the EoR have already experienced a bursty SFH. From our re − M∗ relationship, we find re,F444W = 0.76 ± 0.46 kpc for fixed stellar mass M∗ = 10^9.25 M, which is in agreement with other observations and simulations of SF galaxies in the literature. We find a close-pair (major) merger fraction of (fmaj. merger =0.44 ± 0.22) fmerger = 0.43 ± 0.11 for galaxy separations d <~ 25 kpc, which is in agreement with other z ≈ 6 studies.","lang":"eng"}],"volume":544,"scopus_import":"1","day":"01","article_type":"original","file":[{"success":1,"access_level":"open_access","date_updated":"2025-11-24T10:35:15Z","file_id":"20678","relation":"main_file","file_size":3625308,"creator":"dernst","checksum":"ddb3f429d2246bbf536efb4b0e52f3a8","file_name":"2025_MonthlyNoticesRAS_Stephenson.pdf","date_created":"2025-11-24T10:35:15Z","content_type":"application/pdf"}],"file_date_updated":"2025-11-24T10:35:15Z","citation":{"ieee":"H. M. O. Stephenson <i>et al.</i>, “The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2. Oxford University Press, pp. 1412–1431, 2025.","chicago":"Stephenson, H. M.O., J. P. Stott, C. A. Pirie, K. J. Duncan, D. J. Mcleod, P. N. Best, M. Brinch, et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1725\">https://doi.org/10.1093/mnras/staf1725</a>.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1725\">https://doi.org/10.1093/mnras/staf1725</a>","mla":"Stephenson, H. M. O., et al. “The JWST Emission Line Survey (JELS): The Sizes and Merger Fraction of Star-Forming Galaxies during the Epoch of Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2, Oxford University Press, 2025, pp. 1412–31, doi:<a href=\"https://doi.org/10.1093/mnras/staf1725\">10.1093/mnras/staf1725</a>.","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.","ama":"Stephenson HMO, Stott JP, Pirie CA, et al. The JWST Emission Line Survey (JELS): The sizes and merger fraction of star-forming galaxies during the Epoch of Reionization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;544(2):1412-1431. doi:<a href=\"https://doi.org/10.1093/mnras/staf1725\">10.1093/mnras/staf1725</a>"},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa_version":"Published Version","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"language":[{"iso":"eng"}],"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.","issue":"2"},{"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"citation":{"ama":"Dalmasso N, Watson PJ, Treu T, et al. Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. 2025;544(2):1915-1925. doi:<a href=\"https://doi.org/10.1093/mnras/staf1837\">10.1093/mnras/staf1837</a>","mla":"Dalmasso, Nicolò, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2, Oxford University Press, 2025, pp. 1915–25, doi:<a href=\"https://doi.org/10.1093/mnras/staf1837\">10.1093/mnras/staf1837</a>.","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.","apa":"Dalmasso, N., Watson, P. J., Treu, T., Trenti, M., Vulcani, B., Nanayakkara, T., … Pentericci, L. (2025). Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staf1837\">https://doi.org/10.1093/mnras/staf1837</a>","chicago":"Dalmasso, Nicolò, Peter J. Watson, Tommaso Treu, Michele Trenti, Benedetta Vulcani, Themiya Nanayakkara, Maruša Bradač, et al. “Quantifying Spectroscopic Flux Variations between JWST NIRISS and NIRSpec: Slit Losses in Emission Line Measurements of z ∼ 1-3 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2025. <a href=\"https://doi.org/10.1093/mnras/staf1837\">https://doi.org/10.1093/mnras/staf1837</a>.","ieee":"N. Dalmasso <i>et al.</i>, “Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 544, no. 2. Oxford University Press, pp. 1915–1925, 2025."},"file_date_updated":"2025-11-24T09:02:04Z","file":[{"content_type":"application/pdf","date_created":"2025-11-24T09:02:04Z","checksum":"2caff0a3b81fed114408377323298b43","file_name":"2025_MonthlyNoticesRAS_Dalmasso.pdf","creator":"dernst","relation":"main_file","file_id":"20674","file_size":1952887,"date_updated":"2025-11-24T09:02:04Z","success":1,"access_level":"open_access"}],"issue":"2","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. ","language":[{"iso":"eng"}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","page":"1915-1925","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","day":"01","article_type":"original","scopus_import":"1","volume":544,"abstract":[{"lang":"eng","text":"We analyse James Webb Space Telescope (JWST) Near Infrared Imager and Slitless Spectrograph (NIRISS) and Near Infrared Spectrograph (NIRSpec) spectroscopic observations in the Abell 2744 galaxy cluster field. From approximately 120 candidates, we identify 12 objects with at least two prominent emission lines among [O II] λ3727, H β λ4861, [O III] λ4959, [O III] λ5007, and H α λ6563 that are spectroscopically confirmed by both instruments. Our key findings reveal systematic differences between the two spectrographs based on source morphology and shutter aperture placement. Compact objects show comparable or higher\r\nintegrated flux in NIRSpec relative to NIRISS (within 1σ uncertainties), while extended sources consistently display higher flux in NIRISS measurements. This pattern reflects NIRSpec’s optimal coverage for compact objects while potentially undersampling extended sources. Quantitative analysis demonstrates that NIRSpec recovers at least 63 per cent of NIRISS-measured flux when the slit covers >15 per cent of the source or when Re < 1 kpc. For lower coverage or larger effective radii, the recovered flux varies from 24 per cent to 63 per cent. When studying the H α λ6563/[O III] λ5007 emission line ratio, we observe that\r\nmeasurements from these different spectrographs can vary by up to ∼0.3 dex, with significant implications for metallicity and star formation rate characterizations for individual galaxies. These results highlight the importance of considering instrumental effects when combining multi-instrument spectroscopic data and demonstrate that source morphology critically influences flux\r\nrecovery between slit-based and slitless spectroscopic modes in JWST observations."}],"external_id":{"isi":["001615620500001"],"arxiv":["2510.27036"]},"date_created":"2025-11-23T23:01:38Z","publication_status":"published","department":[{"_id":"JoMa"}],"OA_type":"gold","month":"12","OA_place":"publisher","article_processing_charge":"Yes","fulldoi":"https://doi.org/10.1093/mnras/staf1837","arxiv":1,"date_published":"2025-12-01T00:00:00Z","type":"journal_article","DOAJ_listed":"1","oa":1,"author":[{"full_name":"Dalmasso, Nicolò","last_name":"Dalmasso","first_name":"Nicolò"},{"last_name":"Watson","full_name":"Watson, Peter J.","first_name":"Peter J."},{"first_name":"Tommaso","full_name":"Treu, Tommaso","last_name":"Treu"},{"first_name":"Michele","full_name":"Trenti, Michele","last_name":"Trenti"},{"first_name":"Benedetta","full_name":"Vulcani, Benedetta","last_name":"Vulcani"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"first_name":"Maruša","last_name":"Bradač","full_name":"Bradač, Maruša"},{"first_name":"Tucker","last_name":"Jones","full_name":"Jones, Tucker"},{"first_name":"Kristan","last_name":"Boyett","full_name":"Boyett, Kristan"},{"first_name":"Xin","last_name":"Wang","full_name":"Wang, Xin"},{"full_name":"Mascia, Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara"},{"last_name":"Pentericci","full_name":"Pentericci, Laura","first_name":"Laura"}],"intvolume":"       544","publisher":"Oxford University Press","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","status":"public","doi":"10.1093/mnras/staf1837","year":"2025","date_updated":"2025-12-01T15:23:21Z","title":"Quantifying spectroscopic flux variations between JWST NIRISS and NIRSpec: Slit losses in emission line measurements of z ∼ 1-3 galaxies","PlanS_conform":"1","_id":"20661","isi":1},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","doi":"10.1093/mnras/stae012","title":"A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary","year":"2024","date_updated":"2024-04-02T06:50:01Z","_id":"15189","author":[{"last_name":"Galiullin","full_name":"Galiullin, Ilkham","first_name":"Ilkham"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C","first_name":"Antonio C"},{"last_name":"Kulkarni","full_name":"Kulkarni, Shrinivas R","first_name":"Shrinivas R"},{"last_name":"Sunyaev","full_name":"Sunyaev, Rashid","first_name":"Rashid"},{"last_name":"Gilfanov","full_name":"Gilfanov, Marat","first_name":"Marat"},{"first_name":"Ilfan","full_name":"Bikmaev, Ilfan","last_name":"Bikmaev"},{"first_name":"Lev","last_name":"Yungelson","full_name":"Yungelson, Lev"},{"last_name":"van Roestel","full_name":"van Roestel, Jan","first_name":"Jan"},{"first_name":"Boris T","full_name":"Gänsicke, Boris T","last_name":"Gänsicke"},{"first_name":"Irek","last_name":"Khamitov","full_name":"Khamitov, Irek"},{"last_name":"Szkody","full_name":"Szkody, Paula","first_name":"Paula"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Suslikov","full_name":"Suslikov, Mikhail","first_name":"Mikhail"},{"first_name":"Thomas A","last_name":"Prince","full_name":"Prince, Thomas A"},{"first_name":"Mikhail","last_name":"Buntov","full_name":"Buntov, Mikhail"},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria"},{"full_name":"Gorbachev, Mark","last_name":"Gorbachev","first_name":"Mark"},{"first_name":"Matthew J","last_name":"Graham","full_name":"Graham, Matthew J"},{"last_name":"Gumerov","full_name":"Gumerov, Rustam","first_name":"Rustam"},{"first_name":"Eldar","last_name":"Irtuganov","full_name":"Irtuganov, Eldar"},{"first_name":"Russ R","last_name":"Laher","full_name":"Laher, Russ R"},{"first_name":"Pavel","full_name":"Medvedev, Pavel","last_name":"Medvedev"},{"first_name":"Reed","full_name":"Riddle, Reed","last_name":"Riddle"},{"full_name":"Rusholme, Ben","last_name":"Rusholme","first_name":"Ben"},{"first_name":"Nail","full_name":"Sakhibullin, Nail","last_name":"Sakhibullin"},{"full_name":"Sklyanov, Alexander","last_name":"Sklyanov","first_name":"Alexander"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P","first_name":"Zachary P"}],"oa":1,"publisher":"Oxford University Press","intvolume":"       528","extern":"1","fulldoi":"https://doi.org/10.1093/mnras/stae012","arxiv":1,"date_published":"2024-01-04T00:00:00Z","type":"journal_article","external_id":{"arxiv":["2401.04178"]},"date_created":"2024-03-26T09:43:55Z","publication_status":"published","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stae012","open_access":"1"}],"month":"01","article_processing_charge":"No","day":"04","article_type":"original","scopus_import":"1","volume":528,"abstract":[{"lang":"eng","text":"Cataclysmic variables (CVs) that have evolved past the period minimum during their lifetimes are predicted to be systems with a brown dwarf donor. While population synthesis models predict that around 40–70 per cent of the Galactic CVs are post-period minimum systems referred to as ‘period bouncers’, only a few dozen confirmed systems are known. We report the study and characterization of a new eclipsing CV, SRGeJ041130.3+685350 (SRGeJ0411), discovered from a joint SRG/eROSITA and ZTF programme. The optical spectrum of SRGeJ0411 shows prominent hydrogen and helium emission lines, typical for CVs. We obtained optical high-speed photometry to confirm the eclipse of SRGeJ0411 and determine the orbital period to be Porb ≈ 97.530 min. The spectral energy distribution suggests that the donor has an effective temperature of ≲ 1800 K. We constrain the donor mass with the period–density relationship for Roche lobe-filling stars and find that Mdonor ≲ 0.04 M⊙. The binary parameters are consistent with evolutionary models for post-period minimum CVs, suggesting that SRGeJ0411 is a new period bouncer. The optical emission lines of SRGeJ0411 are single-peaked despite the system being eclipsing, which is typically only seen due to stream-fed accretion in polars. X-ray spectroscopy hints that the white dwarf in SRGeJ0411 could be magnetic, but verifying the magnetic nature of SRGeJ0411 requires further investigation. The lack of optical outbursts has made SRGeJ0411 elusive in previous surveys, and joint X-ray and optical surveys highlight the potential for discovering similar systems in the near future."}],"page":"676-692","publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","language":[{"iso":"eng"}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"citation":{"ieee":"I. Galiullin <i>et al.</i>, “A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 528, no. 1. Oxford University Press, pp. 676–692, 2024.","chicago":"Galiullin, Ilkham, Antonio C Rodriguez, Shrinivas R Kulkarni, Rashid Sunyaev, Marat Gilfanov, Ilfan Bikmaev, Lev Yungelson, et al. “A Joint SRG/EROSITA + ZTF Search: Discovery of a 97-Min Period Eclipsing Cataclysmic Variable with Evidence of a Brown Dwarf Secondary.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae012\">https://doi.org/10.1093/mnras/stae012</a>.","short":"I. Galiullin, A.C. Rodriguez, S.R. Kulkarni, R. Sunyaev, M. Gilfanov, I. Bikmaev, L. Yungelson, J. van Roestel, B.T. Gänsicke, I. Khamitov, P. Szkody, K. El-Badry, M. Suslikov, T.A. Prince, M. Buntov, I. Caiazzo, M. Gorbachev, M.J. Graham, R. Gumerov, E. Irtuganov, R.R. Laher, P. Medvedev, R. Riddle, B. Rusholme, N. Sakhibullin, A. Sklyanov, Z.P. Vanderbosch, Monthly Notices of the Royal Astronomical Society 528 (2024) 676–692.","apa":"Galiullin, I., Rodriguez, A. C., Kulkarni, S. R., Sunyaev, R., Gilfanov, M., Bikmaev, I., … Vanderbosch, Z. P. (2024). A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae012\">https://doi.org/10.1093/mnras/stae012</a>","mla":"Galiullin, Ilkham, et al. “A Joint SRG/EROSITA + ZTF Search: Discovery of a 97-Min Period Eclipsing Cataclysmic Variable with Evidence of a Brown Dwarf Secondary.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 528, no. 1, Oxford University Press, 2024, pp. 676–92, doi:<a href=\"https://doi.org/10.1093/mnras/stae012\">10.1093/mnras/stae012</a>.","ista":"Galiullin I, Rodriguez AC, Kulkarni SR, Sunyaev R, Gilfanov M, Bikmaev I, Yungelson L, van Roestel J, Gänsicke BT, Khamitov I, Szkody P, El-Badry K, Suslikov M, Prince TA, Buntov M, Caiazzo I, Gorbachev M, Graham MJ, Gumerov R, Irtuganov E, Laher RR, Medvedev P, Riddle R, Rusholme B, Sakhibullin N, Sklyanov A, Vanderbosch ZP. 2024. A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. Monthly Notices of the Royal Astronomical Society. 528(1), 676–692.","ama":"Galiullin I, Rodriguez AC, Kulkarni SR, et al. A joint SRG/eROSITA + ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;528(1):676-692. doi:<a href=\"https://doi.org/10.1093/mnras/stae012\">10.1093/mnras/stae012</a>"}},{"date_created":"2024-01-22T08:22:17Z","external_id":{"isi":["001133672400004"],"arxiv":["2305.07044"]},"dataavailabilitystatement":"Raw MUSE data cubes are available from the ESO Science Archive Facility.2 The MUSE-Wide data from the first data release, which covers 44 fields in GOODS-S/CDFS, are available on the MUSE-Wide project page.3 The MUSE HUDF data from the second data release are available via the Advanced MUSE Data products (AMUSED) web interface.4 The stacked spectra in a machine-readable format and the spectral line measurements will be shared upon request to the corresponding author.","department":[{"_id":"GradSch"},{"_id":"JoMa"}],"article_processing_charge":"Yes","month":"02","publication_status":"published","das_tickbox":"1","fulldoi":"https://doi.org/10.1093/mnras/stad3853","type":"journal_article","date_published":"2024-02-01T00:00:00Z","DOAJ_listed":"1","arxiv":1,"publisher":"Oxford University Press","intvolume":"       527","author":[{"last_name":"Kramarenko","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","orcid":"0000-0001-5346-6048"},{"first_name":"J","full_name":"Kerutt, J","last_name":"Kerutt"},{"full_name":"Verhamme, A","last_name":"Verhamme","first_name":"A"},{"first_name":"P A","full_name":"Oesch, P A","last_name":"Oesch"},{"full_name":"Barrufet, L","last_name":"Barrufet","first_name":"L"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"H","last_name":"Kusakabe","full_name":"Kusakabe, H"},{"full_name":"Goovaerts, I","last_name":"Goovaerts","first_name":"I"},{"first_name":"T T","last_name":"Thai","full_name":"Thai, T T"}],"corr_author":"1","oa":1,"doi":"10.1093/mnras/stad3853","year":"2024","date_updated":"2026-10-02T11:29:18Z","title":"Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","has_accepted_license":"1","quality_controlled":"1","status":"public","_id":"14852","isi":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"citation":{"ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871.","mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>.","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;527(4):9853-9871. doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>","chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>.","ieee":"I. Kramarenko <i>et al.</i>, “Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>","short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871."},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"file":[{"creator":"dernst","file_size":4521738,"file_id":"14879","relation":"main_file","date_updated":"2024-01-23T12:30:45Z","access_level":"open_access","success":1,"content_type":"application/pdf","date_created":"2024-01-23T12:30:45Z","file_name":"2024_MNAstronomSoc_Kramarenko.pdf","checksum":"9d02df4035c4951cf63dee0db1e462e9"}],"file_date_updated":"2024-01-23T12:30:45Z","language":[{"iso":"eng"}],"issue":"4","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","page":"9853-9871","volume":527,"supplementarymaterial":"no","abstract":[{"text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &amp;lt; z &amp;lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization.","lang":"eng"}],"day":"01","article_type":"original","scopus_import":"1","researchdata_availability":"upon request"},{"external_id":{"arxiv":["2305.15346"],"isi":["001188770300019"]},"dataavailabilitystatement":"The MUSE data in the UDF-MXDF region underlying this work is available through the website https://amused.univ-lyon1.fr/. The catalogue of galaxies in the MUSE Wide region is available through https://musewide.aip.de/. The transmission spectrum measured in this paper will be available online through the publisher.","date_created":"2024-03-31T22:01:12Z","publication_status":"published","article_processing_charge":"Yes","month":"04","OA_place":"publisher","OA_type":"gold","department":[{"_id":"JoMa"}],"fulldoi":"https://doi.org/10.1093/mnras/stae673","das_tickbox":"1","arxiv":1,"DOAJ_listed":"1","date_published":"2024-04-01T00:00:00Z","type":"journal_article","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Christopher","last_name":"Golling","full_name":"Golling, Christopher"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"full_name":"Lilly, Simon","last_name":"Lilly","first_name":"Simon"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"first_name":"Michael V.","last_name":"Maseda","full_name":"Maseda, Michael V."},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"full_name":"Bouché, Nicolas F.","last_name":"Bouché","first_name":"Nicolas F."},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"oa":1,"corr_author":"1","intvolume":"       529","publisher":"Oxford University Press","has_accepted_license":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","status":"public","quality_controlled":"1","year":"2024","title":"Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field","date_updated":"2026-10-15T09:19:25Z","doi":"10.1093/mnras/stae673","isi":1,"_id":"15249","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"short":"J.J. Matthee, C. Golling, R. Mackenzie, G. Pezzulli, S. Lilly, J. Schaye, R. Bacon, H. Kusakabe, T. Urrutia, L. Boogaard, J. Brinchmann, M.V. Maseda, T. Garel, N.F. Bouché, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 529 (2024) 2794–2806.","apa":"Matthee, J. J., Golling, C., Mackenzie, R., Pezzulli, G., Lilly, S., Schaye, J., … Wisotzki, L. (2024). Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae673\">https://doi.org/10.1093/mnras/stae673</a>","ieee":"J. J. Matthee <i>et al.</i>, “Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 529, no. 3. Oxford University Press, pp. 2794–2806, 2024.","chicago":"Matthee, Jorryt J, Christopher Golling, Ruari Mackenzie, Gabriele Pezzulli, Simon Lilly, Joop Schaye, Roland Bacon, et al. “Large-Scale Excess H I Absorption around z ≈ 4 Galaxies Detected in a Background Galaxy Spectrum in the MUSE EXtremely Deep Field.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae673\">https://doi.org/10.1093/mnras/stae673</a>.","ama":"Matthee JJ, Golling C, Mackenzie R, et al. Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;529(3):2794-2806. doi:<a href=\"https://doi.org/10.1093/mnras/stae673\">10.1093/mnras/stae673</a>","mla":"Matthee, Jorryt J., et al. “Large-Scale Excess H I Absorption around z ≈ 4 Galaxies Detected in a Background Galaxy Spectrum in the MUSE EXtremely Deep Field.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 529, no. 3, Oxford University Press, 2024, pp. 2794–806, doi:<a href=\"https://doi.org/10.1093/mnras/stae673\">10.1093/mnras/stae673</a>.","ista":"Matthee JJ, Golling C, Mackenzie R, Pezzulli G, Lilly S, Schaye J, Bacon R, Kusakabe H, Urrutia T, Boogaard L, Brinchmann J, Maseda MV, Garel T, Bouché NF, Wisotzki L. 2024. Large-scale excess H I absorption around z ≈ 4 galaxies detected in a background galaxy spectrum in the MUSE eXtremely deep field. Monthly Notices of the Royal Astronomical Society. 529(3), 2794–2806."},"file_date_updated":"2024-04-02T08:42:17Z","file":[{"access_level":"open_access","success":1,"date_updated":"2024-04-02T08:42:17Z","file_size":2626735,"file_id":"15255","relation":"main_file","creator":"dernst","file_name":"2024_MonthlyNRoyalAstronSoc_Matthee.pdf","checksum":"1e65c40a71e565eebdc4c5ff11822ba2","date_created":"2024-04-02T08:42:17Z","content_type":"application/pdf"}],"acknowledgement":"We thank the referee for constructive comments that helped improving the paper. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. GP acknowledges support from the Netherlands Research School for Astronomy (Nederlandse Onderzoekschool Voor Astronomie, NOVA). JB acknowledges financial support from the Fundação para a Ciência e a Tecnologia (FCT) through national funds PTDC/FIS-AST/4862/2020, work contract 2020.03379.CEECIND, and research grants UIDB/04434/2020 and UIDP/04434/2020. TU and LW acknowledge funding by the European Research Council through ERC-AdG SPECMAP-CGM, GA 101020943. TG is supported by the ERC Starting grant 757258 ‘TRIPLE’.","issue":"3","language":[{"iso":"eng"}],"oa_version":"Published Version","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"page":"2794-2806","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","day":"01","article_type":"original","abstract":[{"lang":"eng","text":"Observationally mapping the relation between galaxies and the intergalactic medium (IGM) is of key interest for studies of cosmic reionization. Diffuse hydrogen gas has typically been observed in H I Lyman-α (Lyα) absorption in the spectra of bright background quasars. However, it is important to extend these measurements to background galaxies as quasars become increasingly rare at high redshift and rarely probe closely separated sight lines. Here, we use deep integral field spectroscopy in the MUSE eXtremely Deep Field to demonstrate the measurement of the Lyα transmission at z ≈ 4 in absorption to a background galaxy at z = 4.77. The H I transmission is consistent with independent quasar sight lines at similar redshifts. Exploiting the high number of spectroscopic redshifts of faint galaxies (500 between z = 4.0–4.7 within a radius of 8 arcmin) that are tracers of the density field, we show that Lyα transmission is inversely correlated with galaxy density, i.e. transparent regions in the Lyα forest mark underdense regions at z ≈ 4. Due to large-scale clustering, galaxies are surrounded by excess H I absorption over the cosmic mean out to 4 cMpc/h70. We also find that redshifts from the peak of the Lyα line are typically offset from the systemic redshift by +170 km s−1. This work extends results from z ≈ 2–3 to higher redshifts and demonstrates the power of deep integral field spectroscopy to simultaneously measure the ionization structure of the IGM and the large-scale density field in the early Universe."}],"supplementarymaterial":"yes","volume":529,"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224","name":"Young galaxies as tracers and agents of cosmic reionization"}],"researchdata_availability":"yes"},{"quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","status":"public","has_accepted_license":"1","doi":"10.1093/mnras/stae2353","title":"JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 < z < 9.0 in the GOODS fields","date_updated":"2026-10-15T09:36:43Z","year":"2024","isi":1,"_id":"18585","oa":1,"author":[{"full_name":"Meyer, R. A.","last_name":"Meyer","first_name":"R. A."},{"first_name":"P. A.","last_name":"Oesch","full_name":"Oesch, P. A."},{"first_name":"E.","full_name":"Giovinazzo, E.","last_name":"Giovinazzo"},{"full_name":"Weibel, A.","last_name":"Weibel","first_name":"A."},{"full_name":"Brammer, G.","last_name":"Brammer","first_name":"G."},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"R. P.","last_name":"Naidu","full_name":"Naidu, R. P."},{"first_name":"R. J.","full_name":"Bouwens, R. J.","last_name":"Bouwens"},{"first_name":"J.","last_name":"Chisholm","full_name":"Chisholm, J."},{"last_name":"Covelo-Paz","full_name":"Covelo-Paz, A.","first_name":"A."},{"first_name":"Y.","full_name":"Fudamoto, Y.","last_name":"Fudamoto"},{"first_name":"M.","full_name":"Maseda, M.","last_name":"Maseda"},{"last_name":"Nelson","full_name":"Nelson, E.","first_name":"E."},{"first_name":"I.","full_name":"Shivaei, I.","last_name":"Shivaei"},{"first_name":"M.","full_name":"Xiao, M.","last_name":"Xiao"},{"first_name":"T.","last_name":"Herard-Demanche","full_name":"Herard-Demanche, T."},{"first_name":"G. D.","last_name":"Illingworth","full_name":"Illingworth, G. D."},{"first_name":"J.","full_name":"Kerutt, J.","last_name":"Kerutt"},{"full_name":"Kramarenko, Ivan","last_name":"Kramarenko","orcid":"0000-0001-5346-6048","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"last_name":"Labbe","full_name":"Labbe, I.","first_name":"I."},{"first_name":"E.","full_name":"Leonova, E.","last_name":"Leonova"},{"last_name":"Magee","full_name":"Magee, D.","first_name":"D."},{"first_name":"J.","last_name":"Matharu","full_name":"Matharu, J."},{"full_name":"Prieto Lyon, G.","last_name":"Prieto Lyon","first_name":"G."},{"first_name":"N.","full_name":"Reddy, N.","last_name":"Reddy"},{"full_name":"Schaerer, D.","last_name":"Schaerer","first_name":"D."},{"full_name":"Shapley, A.","last_name":"Shapley","first_name":"A."},{"first_name":"M.","last_name":"Stefanon","full_name":"Stefanon, M."},{"first_name":"M. A.","last_name":"Wozniak","full_name":"Wozniak, M. A."},{"full_name":"Wuyts, S.","last_name":"Wuyts","first_name":"S."}],"publisher":"Oxford University Press","intvolume":"       535","fulldoi":"https://doi.org/10.1093/mnras/stae2353","das_tickbox":"1","date_published":"2024-11-01T00:00:00Z","type":"journal_article","DOAJ_listed":"1","external_id":{"isi":["001348009500001"]},"dataavailabilitystatement":"The results presented in this work are mostly based on public JWST GO1 data (Programme #1895), reduced with the publicly-available code GRIZLI (grizli.readthedocs.io). The reduced imaging data is publicly available at https://s3.amazonaws.com/grizli-v2/JwstMosaics/v7/index.html or through MAST: https://archive.stsci.edu/hlsp/fresco (DOI:10.17909/gdyc-7g80). The [\r\n] emitters catalogues presented in this work, as well as subsequent updates, is publicly available at the following link https://github.com/rameyer/fresco/.","date_created":"2024-11-24T23:01:49Z","publication_status":"published","OA_type":"gold","department":[{"_id":"JoMa"}],"article_processing_charge":"Yes","month":"11","OA_place":"publisher","article_type":"original","day":"01","scopus_import":"1","supplementarymaterial":"yes","volume":535,"abstract":[{"text":"We present the census of Hβ+[OIII] 4960,5008 Åemitters at 6.8<z<9.0 from the JWST FRESCO survey over 124 arcmin2 in the GOODS-North and GOODS-South fields. Our unbiased spectroscopic search results in 137 spectroscopically-confirmed galaxies at 6.8<z<9.0 with observed [OIII] fluxes f[OIII]≳1×10−18 ergs s−1 cm−2. The rest-frame optical line ratios of the median stacked spectrum (median MUV=−19.65+0.59−1.05) indicate negligible dust attenuation, low metallicity (12+log(O/H)=7.2−7.7) and a high ionisation parameter log10U≃−2.5. We find a factor ×1.3 difference in the number density of 6.8<z<9.0 galaxies between GOODS-South and GOODS-North, which is caused by a single overdensity at 7.0<z<7.2 in GOODS-North. The bright end of the UV luminosity function of spectroscopically-confirmed [OIII] emitters is in good agreement with HST dropout-selected samples. Discrepancies between the observed [OIII] LF, [OIII]/UV ratio and [OIII] equivalent widths, and that predicted by theoretical models, suggest burstier star-formation histories and/or more heterogeneous metallicity and ionising conditions in z>7 galaxies. We report a rapid decline of the [OIII] luminosity density at z≳6−7 which cannot be explained by the evolution of the cosmic star-formation rate density. Finally we find that FRESCO detects in only 2h galaxies likely accounting for ∼10−20% of the ionising budget at z=7−8 (assuming an escape fraction of 10%), raising the prospect of directly detecting a significant fraction of the sources of reionisation with JWST.","lang":"eng"}],"researchdata_availability":"yes","page":"1067-1094","publication":"Monthly Notices of the Royal Astronomical Society","ddc":["520"],"issue":"1","acknowledgement":"The authors thank the anonymous referee for comments and suggestions which improved this paper. RAM thanks R. Kannan for sharing emission line luminosities from THESAN and H. Katz for similar data from an early version of the SPHINX20 data release (we use the final data release in this paper). The authors thank the CONGRESS team for proposing and designing their program with a zero exclusive access period.\r\nRAM, PA, ACP, and AW acknowledge support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. PA, AW, EG, and MX acknowledge support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072. YF acknowledges support by JSPS KAKENHI grant number JP22K21349 and JP23K13149. RPN acknowledges support for this work provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MS acknowledges support from the European Research Commission Grant 101088789 (SFEER), from the CIDEGENT/2021/059 grant by Generalitat Valenciana, and from project PID2019-109592GB-I00/AEI/10.13039/501100011033 by the Spanish Ministerio de Ciencia e Innovación - Agencia Estatal de Investigación. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program. RJB and MS acknowledges support from NWO grant TOP1.16.057.\r\nThis work is based on observations made with the NASA/ESA/CSA JWST. The raw data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.","language":[{"iso":"eng"}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"mla":"Meyer, R. A., et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1, Oxford University Press, 2024, pp. 1067–94, doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>.","ista":"Meyer RA, Oesch PA, Giovinazzo E, Weibel A, Brammer G, Matthee JJ, Naidu RP, Bouwens RJ, Chisholm J, Covelo-Paz A, Fudamoto Y, Maseda M, Nelson E, Shivaei I, Xiao M, Herard-Demanche T, Illingworth GD, Kerutt J, Kramarenko I, Labbe I, Leonova E, Magee D, Matharu J, Prieto Lyon G, Reddy N, Schaerer D, Shapley A, Stefanon M, Wozniak MA, Wuyts S. 2024. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. Monthly Notices of the Royal Astronomical Society. 535(1), 1067–1094.","ama":"Meyer RA, Oesch PA, Giovinazzo E, et al. JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;535(1):1067-1094. doi:<a href=\"https://doi.org/10.1093/mnras/stae2353\">10.1093/mnras/stae2353</a>","ieee":"R. A. Meyer <i>et al.</i>, “JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 535, no. 1. Oxford University Press, pp. 1067–1094, 2024.","chicago":"Meyer, R. A., P. A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, Jorryt J Matthee, R. P. Naidu, et al. “JWST FRESCO: A Comprehensive Census of H β + [O Iii] Emitters at 6.8 &#60; z &#60; 9.0 in the GOODS Fields.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>.","short":"R.A. Meyer, P.A. Oesch, E. Giovinazzo, A. Weibel, G. Brammer, J.J. Matthee, R.P. Naidu, R.J. Bouwens, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, M. Maseda, E. Nelson, I. Shivaei, M. Xiao, T. Herard-Demanche, G.D. Illingworth, J. Kerutt, I. Kramarenko, I. Labbe, E. Leonova, D. Magee, J. Matharu, G. Prieto Lyon, N. Reddy, D. Schaerer, A. Shapley, M. Stefanon, M.A. Wozniak, S. Wuyts, Monthly Notices of the Royal Astronomical Society 535 (2024) 1067–1094.","apa":"Meyer, R. A., Oesch, P. A., Giovinazzo, E., Weibel, A., Brammer, G., Matthee, J. J., … Wuyts, S. (2024). JWST FRESCO: A comprehensive census of H β + [O iii] emitters at 6.8 &#60; z &#60; 9.0 in the GOODS fields. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2353\">https://doi.org/10.1093/mnras/stae2353</a>"},"file_date_updated":"2024-12-03T12:52:13Z","file":[{"creator":"dernst","file_size":29476699,"file_id":"18613","relation":"main_file","date_updated":"2024-12-03T12:52:13Z","access_level":"open_access","success":1,"content_type":"application/pdf","date_created":"2024-12-03T12:52:13Z","file_name":"2024_MonthlyNRoyalAstronSoc_Meyer.pdf","checksum":"efe0ce3580e01459f3be78eb111b35a9"}]},{"date_published":"2024-11-01T00:00:00Z","type":"journal_article","DOAJ_listed":"1","das_tickbox":"1","fulldoi":"https://doi.org/10.1093/mnras/stae2307","OA_type":"gold","department":[{"_id":"JoMa"}],"article_processing_charge":"Yes","month":"11","OA_place":"publisher","publication_status":"published","date_created":"2024-11-10T23:01:58Z","external_id":{"isi":["001335663900008"]},"dataavailabilitystatement":"The derived data generated in this research will be shared on reasonable requests to the corresponding author.","isi":1,"_id":"18523","doi":"10.1093/mnras/stae2307","date_updated":"2026-10-15T09:35:12Z","title":"A unified model for the clustering of quasars and galaxies at z ≈ 6","year":"2024","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","quality_controlled":"1","status":"public","has_accepted_license":"1","publisher":"Oxford University Press","intvolume":"       534","oa":1,"author":[{"first_name":"Elia","last_name":"Pizzati","full_name":"Pizzati, Elia"},{"last_name":"Hennawi","full_name":"Hennawi, Joseph F.","first_name":"Joseph F."},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"last_name":"Schaller","full_name":"Schaller, Matthieu","first_name":"Matthieu"},{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"first_name":"Feige","last_name":"Wang","full_name":"Wang, Feige"},{"last_name":"Frenk","full_name":"Frenk, Carlos S.","first_name":"Carlos S."},{"full_name":"Elbers, Willem","last_name":"Elbers","first_name":"Willem"},{"first_name":"John C.","full_name":"Helly, John C.","last_name":"Helly"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Rongmon","last_name":"Bordoloi","full_name":"Bordoloi, Rongmon"},{"first_name":"Daichi","last_name":"Kashino","full_name":"Kashino, Daichi"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"full_name":"Yue, Minghao","last_name":"Yue","first_name":"Minghao"}],"tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","language":[{"iso":"eng"}],"issue":"4","acknowledgement":"We are grateful to Junya Arita and the SHELLQs team for sharing their data on the quasar autocorrelation function and to Jan-Torge Schindler for discussion on the QLF. We acknowledge helpful conversations with the ENIGMA group at UC Santa Barbara and Leiden University. EP is grateful to Rob McGibbon and Victor Forouhar Moreno for help with the simulation outputs, and to Timo Kist, Jiamu Huang, and Vikram Khaire for comments on an early version of the manuscript. JFH and EP acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 885301). This work is partly supported by funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No 860744 (BiD4BESt). FW acknowledges support from NSF grant AST-2308258. This work used the DiRAC Memory Intensive service (Cosma8) at the University of Durham, which is part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). Access to DiRAC resources was granted through a Director’s Discretionary Time allocation in 2023/24, under the auspices of the UKRI-funded\r\nDiRAC Federation Project. The equipment was funded by BEIS capital funding via STFC capital grants ST/K00042X/1, ST/P002293/1, ST/R002371/1, and ST/S002502/1, Durham University, and STFC operations grant ST/R000832/1. DiRAC is part of the National e-Infrastructure.","file":[{"creator":"dernst","file_id":"18542","relation":"main_file","file_size":2954312,"date_updated":"2024-11-12T07:17:26Z","success":1,"access_level":"open_access","content_type":"application/pdf","date_created":"2024-11-12T07:17:26Z","checksum":"9ea6285dd1d04d7a9e7b40a4c9e11edb","file_name":"2024_MonthlyNRoyalAstronSoc_Pizzati.pdf"}],"file_date_updated":"2024-11-12T07:17:26Z","citation":{"ama":"Pizzati E, Hennawi JF, Schaye J, et al. A unified model for the clustering of quasars and galaxies at z ≈ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;534(4):3155-3175. doi:<a href=\"https://doi.org/10.1093/mnras/stae2307\">10.1093/mnras/stae2307</a>","ista":"Pizzati E, Hennawi JF, Schaye J, Schaller M, Eilers AC, Wang F, Frenk CS, Elbers W, Helly JC, Mackenzie R, Matthee JJ, Bordoloi R, Kashino D, Naidu RP, Yue M. 2024. A unified model for the clustering of quasars and galaxies at z ≈ 6. Monthly Notices of the Royal Astronomical Society. 534(4), 3155–3175.","mla":"Pizzati, Elia, et al. “A Unified Model for the Clustering of Quasars and Galaxies at z ≈ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 4, Oxford University Press, 2024, pp. 3155–75, doi:<a href=\"https://doi.org/10.1093/mnras/stae2307\">10.1093/mnras/stae2307</a>.","apa":"Pizzati, E., Hennawi, J. F., Schaye, J., Schaller, M., Eilers, A. C., Wang, F., … Yue, M. (2024). A unified model for the clustering of quasars and galaxies at z ≈ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2307\">https://doi.org/10.1093/mnras/stae2307</a>","short":"E. Pizzati, J.F. Hennawi, J. Schaye, M. Schaller, A.C. Eilers, F. Wang, C.S. Frenk, W. Elbers, J.C. Helly, R. Mackenzie, J.J. Matthee, R. Bordoloi, D. Kashino, R.P. Naidu, M. Yue, Monthly Notices of the Royal Astronomical Society 534 (2024) 3155–3175.","chicago":"Pizzati, Elia, Joseph F. Hennawi, Joop Schaye, Matthieu Schaller, Anna Christina Eilers, Feige Wang, Carlos S. Frenk, et al. “A Unified Model for the Clustering of Quasars and Galaxies at z ≈ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2307\">https://doi.org/10.1093/mnras/stae2307</a>.","ieee":"E. Pizzati <i>et al.</i>, “A unified model for the clustering of quasars and galaxies at z ≈ 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 4. Oxford University Press, pp. 3155–3175, 2024."},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"researchdata_availability":"upon request","volume":534,"supplementarymaterial":"yes","abstract":[{"lang":"eng","text":"Recent observations from the EIGER JWST program have measured for the first time the quasar–galaxy cross-correlation function at z ≈ 6. The autocorrelation function of faint z ≈ 6 quasars was also recently estimated. These measurements provide key insights into the properties of quasars and galaxies at high redshift and their relation with the host dark matter haloes. In this work, we interpret these data building upon an empirical quasar population model that has been applied successfully to quasar clustering and demographic measurements at z ≈ 2–4. We use a new, large-volume N-body simulation with more than a trillion particles, FLAMINGO-10k, to model quasars and galaxies simultaneously. We successfully reproduce observations of z ≈ 6 quasars and galaxies (i.e. their clustering properties and luminosity functions), and infer key quantities such as their luminosity–halo mass relation, the mass function of their host haloes, and their duty cycle/occupation fraction. Our key findings\r\nare (i) quasars reside on average in ≈ 1012.5 M haloes (corresponding to ≈ 5σ fluctuations in the initial conditions of the linear density field), but the distribution of host halo masses is quite broad; (ii) the duty cycle of (UV-bright) quasar activity is relatively low (≈ 1 per cent); (iii) galaxies (that are bright in [O III]) live in much smaller haloes (≈ 1010.9 M) and have a larger duty cycle (occupation fraction) of ≈ 13 per cent. Finally, we focus on the inferred properties of quasars and present a homogeneous analysis of their evolution with redshift. The picture that emerges reveals a strong evolution of the host halo mass and duty cycle of quasars at z ≈ 2–6, and calls for new investigations of the role of quasar activity across cosmic time."}],"day":"01","article_type":"original","scopus_import":"1","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","page":"3155-3175"},{"date_created":"2024-10-06T22:01:11Z","external_id":{"isi":["001320536900011"],"arxiv":["2409.01157"]},"dataavailabilitystatement":"Table 1 is available at the CDS. Light curves used in this work are available at Mikulski Archive for Space Telescopes at the Space Telescope Science Institute (MAST)1. Other intermediate data products will be made available upon reasonable request.","OA_type":"gold","department":[{"_id":"LiBu"}],"month":"10","OA_place":"publisher","article_processing_charge":"Yes","publication_status":"published","das_tickbox":"1","fulldoi":"https://doi.org/10.1093/mnras/stae2053","type":"journal_article","date_published":"2024-10-01T00:00:00Z","DOAJ_listed":"1","arxiv":1,"intvolume":"       534","publisher":"Oxford University Press","oa":1,"author":[{"first_name":"Emily J.","last_name":"Hatt","full_name":"Hatt, Emily J."},{"first_name":"J. M.Joel","full_name":"Ong, J. M.Joel","last_name":"Ong"},{"last_name":"Nielsen","full_name":"Nielsen, Martin B.","first_name":"Martin B."},{"first_name":"William J.","last_name":"Chaplin","full_name":"Chaplin, William J."},{"first_name":"Guy R.","full_name":"Davies, Guy R.","last_name":"Davies"},{"first_name":"Sébastien","last_name":"Deheuvels","full_name":"Deheuvels, Sébastien"},{"first_name":"Jérôme","full_name":"Ballot, Jérôme","last_name":"Ballot"},{"first_name":"Gang","full_name":"Li, Gang","last_name":"Li"},{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"}],"doi":"10.1093/mnras/stae2053","title":"Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants","date_updated":"2026-10-16T08:52:08Z","year":"2024","status":"public","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","quality_controlled":"1","has_accepted_license":"1","_id":"18172","isi":1,"PlanS_conform":"1","citation":{"ieee":"E. J. Hatt <i>et al.</i>, “Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2. Oxford University Press, pp. 1060–1076, 2024.","chicago":"Hatt, Emily J., J. M.Joel Ong, Martin B. Nielsen, William J. Chaplin, Guy R. Davies, Sébastien Deheuvels, Jérôme Ballot, Gang Li, and Lisa Annabelle Bugnet. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>.","short":"E.J. Hatt, J.M.J. Ong, M.B. Nielsen, W.J. Chaplin, G.R. Davies, S. Deheuvels, J. Ballot, G. Li, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 534 (2024) 1060–1076.","apa":"Hatt, E. J., Ong, J. M. J., Nielsen, M. B., Chaplin, W. J., Davies, G. R., Deheuvels, S., … Bugnet, L. A. (2024). Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stae2053\">https://doi.org/10.1093/mnras/stae2053</a>","mla":"Hatt, Emily J., et al. “Asteroseismic Signatures of Core Magnetism and Rotation in Hundreds of Low-Luminosity Red Giants.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 534, no. 2, Oxford University Press, 2024, pp. 1060–76, doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>.","ista":"Hatt EJ, Ong JMJ, Nielsen MB, Chaplin WJ, Davies GR, Deheuvels S, Ballot J, Li G, Bugnet LA. 2024. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. Monthly Notices of the Royal Astronomical Society. 534(2), 1060–1076.","ama":"Hatt EJ, Ong JMJ, Nielsen MB, et al. Asteroseismic signatures of core magnetism and rotation in hundreds of low-luminosity red giants. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;534(2):1060-1076. doi:<a href=\"https://doi.org/10.1093/mnras/stae2053\">10.1093/mnras/stae2053</a>"},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"file":[{"file_name":"2024_MonthlyNRoyalAstronSoc_Hatt.pdf","checksum":"b79f3c6a5991516abbcc8d34fa4bfb5f","date_created":"2024-10-07T09:14:03Z","content_type":"application/pdf","access_level":"open_access","success":1,"date_updated":"2024-10-07T09:14:03Z","file_size":2813008,"relation":"main_file","file_id":"18182","creator":"dernst"}],"file_date_updated":"2024-10-07T09:14:03Z","language":[{"iso":"eng"}],"issue":"2","acknowledgement":"EJH, WJC, and GRD acknowledge the support of Science and Technology Facilities Council. MBN acknowledges support from the UK Space Agency. JMJO acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001, awarded by STScI (Space Telescope Science Institute), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The authors acknowledge use of the Blue-BEAR HPC service at the University of Birmingham. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission was provided by the NASA Science Mission Directorate. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/web/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC was provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (CartographY GA. 804752). SD and JB acknowledge support from the Centre National d’Etudes Spatiales (CNES).","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"oa_version":"Published Version","ddc":["520"],"publication":"Monthly Notices of the Royal Astronomical Society","page":"1060-1076","volume":534,"supplementarymaterial":"yes","abstract":[{"text":"Red Giant stars host solar-like oscillations which have mixed character, being sensitive to conditions both in the outer convection zone and deep within the interior. The properties of these modes are sensitive to both core rotation and magnetic fields. While asteroseismic studies of the former have been done on a large scale, studies of the latter are currently limited to tens of stars. We aim to produce the first large catalogue of both magnetic and rotational perturbations. We jointly constrain these parameters by devising an automated method for fitting the power spectra directly. We successfully apply the method to 302 low-luminosity red giants. We find a clear bimodality in core rotation rate. The primary peak is at δνrot = 0.32 μHz, and the secondary at δνrot = 0.47 μHz. Combining our results with literature values, we find that the percentage of stars rotating much more rapidly than the population average increases with evolutionary state. We measure magnetic splittings of 2σ significance in 23 stars. While the most extreme magnetic splitting values appear in stars with masses > 1.1M⊙, implying they formerly hosted a convective core, a small but statistically significant magnetic splitting is measured at lower masses. Asymmetry between the frequencies of a rotationally split multiplet has previously been used to diagnose the presence of a magnetic perturbation. We find that of the stars with a significant detection of magnetic perturbation, 43\\% do not show strong asymmetry. We find no strong evidence of correlation between the rotation and magnetic parameters.","lang":"eng"}],"article_type":"original","day":"01","scopus_import":"1","researchdata_availability":"yes"},{"external_id":{"arxiv":["2305.07337"]},"date_created":"2023-08-21T10:13:56Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2305.07337"}],"publication_status":"published","month":"09","article_processing_charge":"No","fulldoi":"https://doi.org/10.1093/mnras/stad1977","arxiv":1,"type":"journal_article","date_published":"2023-09-01T00:00:00Z","oa":1,"author":[{"first_name":"R","full_name":"Farmer, R","last_name":"Farmer"},{"first_name":"M","last_name":"Renzo","full_name":"Renzo, M"},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg"},{"first_name":"E","full_name":"Bellinger, E","last_name":"Bellinger"},{"first_name":"S","last_name":"Justham","full_name":"Justham, S"},{"first_name":"S E","full_name":"de Mink, S E","last_name":"de Mink"}],"intvolume":"       524","publisher":"Oxford University Press","extern":"1","quality_controlled":"1","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Observational predictions for Thorne–Żytkow objects","year":"2023","date_updated":"2023-08-21T12:12:48Z","doi":"10.1093/mnras/stad1977","_id":"14104","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"ama":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;524(2):1692-1709. doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>","mla":"Farmer, R., et al. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2, Oxford University Press, 2023, pp. 1692–709, doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>.","ista":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. 2023. Observational predictions for Thorne–Żytkow objects. Monthly Notices of the Royal Astronomical Society. 524(2), 1692–1709.","short":"R. Farmer, M. Renzo, Y.L.L. Götberg, E. Bellinger, S. Justham, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 524 (2023) 1692–1709.","apa":"Farmer, R., Renzo, M., Götberg, Y. L. L., Bellinger, E., Justham, S., &#38; de Mink, S. E. (2023). Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>","ieee":"R. Farmer, M. Renzo, Y. L. L. Götberg, E. Bellinger, S. Justham, and S. E. de Mink, “Observational predictions for Thorne–Żytkow objects,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2. Oxford University Press, pp. 1692–1709, 2023.","chicago":"Farmer, R, M Renzo, Ylva Louise Linsdotter Götberg, E Bellinger, S Justham, and S E de Mink. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"issue":"2","language":[{"iso":"eng"}],"oa_version":"Preprint","page":"1692-1709","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","day":"01","article_type":"original","abstract":[{"text":"Thorne–Żytkow objects (TŻO) are potential end products of the merger of a neutron star with a non-degenerate star. In this work, we have computed the first grid of evolutionary models of TŻOs with the MESA stellar evolution code. With these models, we predict several observational properties of TŻOs, including their surface temperatures and luminosities, pulsation periods, and nucleosynthetic products. We expand the range of possible TŻO solutions to cover 3.45≲log(Teff/K)≲3.65 and 4.85≲log(L/L⊙)≲5.5⁠. Due to the much higher densities our TŻOs reach compared to previous models, if TŻOs form we expect them to be stable over a larger mass range than previously predicted, without exhibiting a gap in their mass distribution. Using the GYRE stellar pulsation code we show that TŻOs should have fundamental pulsation periods of 1000–2000 d, and period ratios of ≈0.2–0.3. Models computed with a large 399 isotope fully coupled nuclear network show a nucleosynthetic signal that is different to previously predicted. We propose a new nucleosynthetic signal to determine a star’s status as a TŻO: the isotopologues 44TiO2 and 44TiO⁠, which will have a shift in their spectral features as compared to stable titanium-containing molecules. We find that in the local Universe (∼SMC metallicities and above) TŻOs show little heavy metal enrichment, potentially explaining the difficulty in finding TŻOs to-date.","lang":"eng"}],"volume":524},{"publication":"Monthly Notices of the Royal Astronomical Society","page":"12219-12231","abstract":[{"lang":"eng","text":"We report on IXPE, NICER, and XMM–Newton observations of the magnetar 1E 2259+586. We find that the source is significantly polarized at about or above 20  per cent for all phases except for the secondary peak where it is more weakly polarized. The polarization degree is strongest during the primary minimum which is also the phase where an absorption feature has been identified previously. The polarization angle of the photons are consistent with a rotating vector model with a mode switch between the primary minimum and the rest of the rotation of the neutron star. We propose a scenario in which the emission at the source is weakly polarized (as in a condensed surface) and, as the radiation passes through a plasma arch, resonant cyclotron scattering off of protons produces the observed polarized radiation. This confirms the magnetar nature of the source with a surface field greater than about 1015 G."}],"volume":527,"scopus_import":"1","article_type":"original","day":"01","citation":{"ieee":"J. Heyl <i>et al.</i>, “The detection of polarized X-ray emission from the magnetar 1E 2259+586,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 12219–12231, 2023.","chicago":"Heyl, Jeremy, Roberto Taverna, Roberto Turolla, Gian Luca Israel, Mason Ng, Demet Kırmızıbayrak, Denis González-Caniulef, et al. “The Detection of Polarized X-Ray Emission from the Magnetar 1E 2259+586.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad3680\">https://doi.org/10.1093/mnras/stad3680</a>.","apa":"Heyl, J., Taverna, R., Turolla, R., Israel, G. L., Ng, M., Kırmızıbayrak, D., … Xie, F. (2023). The detection of polarized X-ray emission from the magnetar 1E 2259+586. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3680\">https://doi.org/10.1093/mnras/stad3680</a>","short":"J. Heyl, R. Taverna, R. Turolla, G.L. Israel, M. Ng, D. Kırmızıbayrak, D. González-Caniulef, I. Caiazzo, S. Zane, S.R. Ehlert, M. Negro, I. Agudo, L.A. Antonelli, M. Bachetti, L. Baldini, W.H. Baumgartner, R. Bellazzini, S. Bianchi, S.D. Bongiorno, R. Bonino, A. Brez, N. Bucciantini, F. Capitanio, S. Castellano, E. Cavazzuti, C.-T. Chen, S. Ciprini, E. Costa, A. De Rosa, E. Del Monte, L. Di Gesu, N. Di Lalla, A. Di Marco, I. Donnarumma, V. Doroshenko, M. Dovčiak, T. Enoto, Y. Evangelista, S. Fabiani, R. Ferrazzoli, J.A. Garcia, S. Gunji, K. Hayashida, W. Iwakiri, S.G. Jorstad, P. Kaaret, V. Karas, F. Kislat, T. Kitaguchi, J.J. Kolodziejczak, H. Krawczynski, F.L. Monaca, L. Latronico, I. Liodakis, S. Maldera, A. Manfreda, F. Marin, A. Marinucci, A.P. Marscher, H.L. Marshall, F. Massaro, G. Matt, I. Mitsuishi, T. Mizuno, F. Muleri, C.-Y. Ng, S.L. O’Dell, N. Omodei, C. Oppedisano, A. Papitto, G.G. Pavlov, A.L. Peirson, M. Perri, M. Pesce-Rollins, P.-O. Petrucci, M. Pilia, A. Possenti, J. Poutanen, S. Puccetti, B.D. Ramsey, J. Rankin, A. Ratheesh, O.J. Roberts, R.W. Romani, C. Sgrò, P. Slane, P. Soffitta, G. Spandre, D.A. Swartz, T. Tamagawa, F. Tavecchio, Y. Tawara, A.F. Tennant, N.E. Thomas, F. Tombesi, A. Trois, S.S. Tsygankov, J. Vink, M.C. Weisskopf, K. Wu, F. Xie, Monthly Notices of the Royal Astronomical Society 527 (2023) 12219–12231.","ista":"Heyl J et al. 2023. The detection of polarized X-ray emission from the magnetar 1E 2259+586. Monthly Notices of the Royal Astronomical Society. 527(4), 12219–12231.","mla":"Heyl, Jeremy, et al. “The Detection of Polarized X-Ray Emission from the Magnetar 1E 2259+586.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2023, pp. 12219–31, doi:<a href=\"https://doi.org/10.1093/mnras/stad3680\">10.1093/mnras/stad3680</a>.","ama":"Heyl J, Taverna R, Turolla R, et al. The detection of polarized X-ray emission from the magnetar 1E 2259+586. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;527(4):12219-12231. doi:<a href=\"https://doi.org/10.1093/mnras/stad3680\">10.1093/mnras/stad3680</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"language":[{"iso":"eng"}],"issue":"4","oa_version":"Published Version","tmp":{"short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png"},"intvolume":"       527","publisher":"Oxford University Press","author":[{"first_name":"Jeremy","last_name":"Heyl","full_name":"Heyl, Jeremy"},{"last_name":"Taverna","full_name":"Taverna, Roberto","first_name":"Roberto"},{"first_name":"Roberto","full_name":"Turolla, Roberto","last_name":"Turolla"},{"first_name":"Gian Luca","full_name":"Israel, Gian Luca","last_name":"Israel"},{"first_name":"Mason","full_name":"Ng, Mason","last_name":"Ng"},{"full_name":"Kırmızıbayrak, Demet","last_name":"Kırmızıbayrak","first_name":"Demet"},{"first_name":"Denis","full_name":"González-Caniulef, Denis","last_name":"González-Caniulef"},{"first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria"},{"first_name":"Silvia","last_name":"Zane","full_name":"Zane, Silvia"},{"first_name":"Steven R","last_name":"Ehlert","full_name":"Ehlert, Steven R"},{"last_name":"Negro","full_name":"Negro, Michela","first_name":"Michela"},{"full_name":"Agudo, Iván","last_name":"Agudo","first_name":"Iván"},{"first_name":"Lucio Angelo","full_name":"Antonelli, Lucio Angelo","last_name":"Antonelli"},{"last_name":"Bachetti","full_name":"Bachetti, Matteo","first_name":"Matteo"},{"full_name":"Baldini, Luca","last_name":"Baldini","first_name":"Luca"},{"first_name":"Wayne H","full_name":"Baumgartner, Wayne H","last_name":"Baumgartner"},{"first_name":"Ronaldo","full_name":"Bellazzini, Ronaldo","last_name":"Bellazzini"},{"full_name":"Bianchi, Stefano","last_name":"Bianchi","first_name":"Stefano"},{"full_name":"Bongiorno, Stephen D","last_name":"Bongiorno","first_name":"Stephen D"},{"first_name":"Raffaella","full_name":"Bonino, Raffaella","last_name":"Bonino"},{"first_name":"Alessandro","last_name":"Brez","full_name":"Brez, Alessandro"},{"full_name":"Bucciantini, Niccolò","last_name":"Bucciantini","first_name":"Niccolò"},{"last_name":"Capitanio","full_name":"Capitanio, Fiamma","first_name":"Fiamma"},{"full_name":"Castellano, Simone","last_name":"Castellano","first_name":"Simone"},{"last_name":"Cavazzuti","full_name":"Cavazzuti, Elisabetta","first_name":"Elisabetta"},{"last_name":"Chen","full_name":"Chen, Chien-Ting","first_name":"Chien-Ting"},{"last_name":"Ciprini","full_name":"Ciprini, Stefano","first_name":"Stefano"},{"first_name":"Enrico","last_name":"Costa","full_name":"Costa, Enrico"},{"first_name":"Alessandra","last_name":"De Rosa","full_name":"De Rosa, Alessandra"},{"full_name":"Del Monte, Ettore","last_name":"Del Monte","first_name":"Ettore"},{"first_name":"Laura","full_name":"Di Gesu, Laura","last_name":"Di Gesu"},{"first_name":"Niccolò","last_name":"Di Lalla","full_name":"Di Lalla, Niccolò"},{"full_name":"Di Marco, Alessandro","last_name":"Di Marco","first_name":"Alessandro"},{"last_name":"Donnarumma","full_name":"Donnarumma, Immacolata","first_name":"Immacolata"},{"last_name":"Doroshenko","full_name":"Doroshenko, Victor","first_name":"Victor"},{"first_name":"Michal","last_name":"Dovčiak","full_name":"Dovčiak, Michal"},{"full_name":"Enoto, Teruaki","last_name":"Enoto","first_name":"Teruaki"},{"first_name":"Yuri","full_name":"Evangelista, Yuri","last_name":"Evangelista"},{"first_name":"Sergio","last_name":"Fabiani","full_name":"Fabiani, Sergio"},{"first_name":"Riccardo","last_name":"Ferrazzoli","full_name":"Ferrazzoli, Riccardo"},{"first_name":"Javier A","full_name":"Garcia, Javier A","last_name":"Garcia"},{"first_name":"Shuichi","full_name":"Gunji, Shuichi","last_name":"Gunji"},{"full_name":"Hayashida, Kiyoshi","last_name":"Hayashida","first_name":"Kiyoshi"},{"full_name":"Iwakiri, Wataru","last_name":"Iwakiri","first_name":"Wataru"},{"first_name":"Svetlana G","last_name":"Jorstad","full_name":"Jorstad, Svetlana G"},{"last_name":"Kaaret","full_name":"Kaaret, Philip","first_name":"Philip"},{"first_name":"Vladimir","full_name":"Karas, Vladimir","last_name":"Karas"},{"last_name":"Kislat","full_name":"Kislat, Fabian","first_name":"Fabian"},{"first_name":"Takao","last_name":"Kitaguchi","full_name":"Kitaguchi, Takao"},{"last_name":"Kolodziejczak","full_name":"Kolodziejczak, Jeffery J","first_name":"Jeffery J"},{"full_name":"Krawczynski, Henric","last_name":"Krawczynski","first_name":"Henric"},{"full_name":"Monaca, Fabio La","last_name":"Monaca","first_name":"Fabio La"},{"first_name":"Luca","full_name":"Latronico, Luca","last_name":"Latronico"},{"last_name":"Liodakis","full_name":"Liodakis, Ioannis","first_name":"Ioannis"},{"first_name":"Simone","last_name":"Maldera","full_name":"Maldera, Simone"},{"full_name":"Manfreda, Alberto","last_name":"Manfreda","first_name":"Alberto"},{"first_name":"Frédéric","full_name":"Marin, Frédéric","last_name":"Marin"},{"first_name":"Andrea","full_name":"Marinucci, Andrea","last_name":"Marinucci"},{"last_name":"Marscher","full_name":"Marscher, Alan P","first_name":"Alan P"},{"first_name":"Herman L","full_name":"Marshall, Herman L","last_name":"Marshall"},{"first_name":"Francesco","full_name":"Massaro, Francesco","last_name":"Massaro"},{"full_name":"Matt, Giorgio","last_name":"Matt","first_name":"Giorgio"},{"first_name":"Ikuyuki","last_name":"Mitsuishi","full_name":"Mitsuishi, Ikuyuki"},{"full_name":"Mizuno, Tsunefumi","last_name":"Mizuno","first_name":"Tsunefumi"},{"first_name":"Fabio","last_name":"Muleri","full_name":"Muleri, Fabio"},{"first_name":"C-Y","full_name":"Ng, C-Y","last_name":"Ng"},{"first_name":"Stephen L","full_name":"O’Dell, Stephen L","last_name":"O’Dell"},{"first_name":"Nicola","last_name":"Omodei","full_name":"Omodei, Nicola"},{"last_name":"Oppedisano","full_name":"Oppedisano, Chiara","first_name":"Chiara"},{"first_name":"Alessandro","last_name":"Papitto","full_name":"Papitto, Alessandro"},{"last_name":"Pavlov","full_name":"Pavlov, George G","first_name":"George G"},{"first_name":"Abel Lawrence","full_name":"Peirson, Abel Lawrence","last_name":"Peirson"},{"full_name":"Perri, Matteo","last_name":"Perri","first_name":"Matteo"},{"first_name":"Melissa","full_name":"Pesce-Rollins, Melissa","last_name":"Pesce-Rollins"},{"last_name":"Petrucci","full_name":"Petrucci, Pierre-Olivier","first_name":"Pierre-Olivier"},{"first_name":"Maura","full_name":"Pilia, Maura","last_name":"Pilia"},{"full_name":"Possenti, Andrea","last_name":"Possenti","first_name":"Andrea"},{"full_name":"Poutanen, Juri","last_name":"Poutanen","first_name":"Juri"},{"first_name":"Simonetta","last_name":"Puccetti","full_name":"Puccetti, Simonetta"},{"last_name":"Ramsey","full_name":"Ramsey, Brian D","first_name":"Brian D"},{"first_name":"John","last_name":"Rankin","full_name":"Rankin, John"},{"first_name":"Ajay","full_name":"Ratheesh, Ajay","last_name":"Ratheesh"},{"first_name":"Oliver J","last_name":"Roberts","full_name":"Roberts, Oliver J"},{"full_name":"Romani, Roger W","last_name":"Romani","first_name":"Roger W"},{"last_name":"Sgrò","full_name":"Sgrò, Carmelo","first_name":"Carmelo"},{"first_name":"Patrick","last_name":"Slane","full_name":"Slane, Patrick"},{"last_name":"Soffitta","full_name":"Soffitta, Paolo","first_name":"Paolo"},{"first_name":"Gloria","full_name":"Spandre, Gloria","last_name":"Spandre"},{"first_name":"Douglas A","full_name":"Swartz, Douglas A","last_name":"Swartz"},{"first_name":"Toru","last_name":"Tamagawa","full_name":"Tamagawa, Toru"},{"full_name":"Tavecchio, Fabrizio","last_name":"Tavecchio","first_name":"Fabrizio"},{"last_name":"Tawara","full_name":"Tawara, Yuzuru","first_name":"Yuzuru"},{"first_name":"Allyn F","full_name":"Tennant, Allyn F","last_name":"Tennant"},{"first_name":"Nicholas E","full_name":"Thomas, Nicholas E","last_name":"Thomas"},{"full_name":"Tombesi, Francesco","last_name":"Tombesi","first_name":"Francesco"},{"last_name":"Trois","full_name":"Trois, Alessio","first_name":"Alessio"},{"last_name":"Tsygankov","full_name":"Tsygankov, Sergey S","first_name":"Sergey S"},{"full_name":"Vink, Jacco","last_name":"Vink","first_name":"Jacco"},{"first_name":"Martin C","last_name":"Weisskopf","full_name":"Weisskopf, Martin C"},{"full_name":"Wu, Kinwah","last_name":"Wu","first_name":"Kinwah"},{"first_name":"Fei","full_name":"Xie, Fei","last_name":"Xie"}],"oa":1,"extern":"1","date_updated":"2024-04-02T06:51:04Z","title":"The detection of polarized X-ray emission from the magnetar 1E 2259+586","year":"2023","doi":"10.1093/mnras/stad3680","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","status":"public","_id":"15190","date_created":"2024-03-26T09:44:24Z","external_id":{"arxiv":["2311.03637"]},"article_processing_charge":"No","month":"12","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stad3680"}],"fulldoi":"https://doi.org/10.1093/mnras/stad3680","date_published":"2023-12-01T00:00:00Z","type":"journal_article","arxiv":1},{"publisher":"Oxford University Press","intvolume":"       520","author":[{"last_name":"Fleury","full_name":"Fleury, Leesa","first_name":"Leesa"},{"last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"first_name":"Jeremy","last_name":"Heyl","full_name":"Heyl, Jeremy"}],"oa":1,"extern":"1","date_updated":"2024-04-02T07:13:10Z","title":"The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3","year":"2023","doi":"10.1093/mnras/stad068","quality_controlled":"1","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"15199","date_created":"2024-03-26T09:48:27Z","external_id":{"arxiv":["2205.01015"]},"month":"01","article_processing_charge":"No","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2205.01015"}],"fulldoi":"https://doi.org/10.1093/mnras/stad068","type":"journal_article","date_published":"2023-01-12T00:00:00Z","arxiv":1,"publication":"Monthly Notices of the Royal Astronomical Society","page":"364-374","abstract":[{"text":"Gaia Data Release 2 revealed a population of ultramassive white dwarfs on the Q branch that are moving anomalously fast for a local disc population with their young photometric ages. As the velocity dispersion of stars in the local disc increases with age, a proposed explanation of these white dwarfs is that they experience a cooling delay that causes current cooling models to infer photometric ages much younger than their true ages. To explore this explanation, we investigate the kinematics of ultramassive white dwarfs within 200 pc of the Sun using the improved Gaia Early Data Release 3 observations. We analyse the transverse motions of 0.95–1.25 M⊙ white dwarfs, subdivided by mass and age, and determine the distributions of the three-dimensional components of the transverse velocities. The results are compared to expectations based on observed kinematics of local main-sequence stars. We find a population of photometrically young (∼0.5–1.5 Gyr) ultramassive (∼1.15–1.25 M⊙) white dwarfs for which the transverse velocity component in the direction of Galactic rotation is more dispersed than for local disc stars of any age; thus, it is too dispersed to be explained by any cooling delay in white dwarfs originating from the local disc. Furthermore, the dispersion ratio of the velocity components in the Galactic plane for this population is also inconsistent with a local disc origin. We discuss some possible explanations of this kinematically anomalous population, such as a halo origin or production through dynamical effects of stellar triple systems.","lang":"eng"}],"volume":520,"scopus_import":"1","article_type":"original","day":"12","citation":{"apa":"Fleury, L., Caiazzo, I., &#38; Heyl, J. (2023). The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad068\">https://doi.org/10.1093/mnras/stad068</a>","short":"L. Fleury, I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 520 (2023) 364–374.","ieee":"L. Fleury, I. Caiazzo, and J. Heyl, “The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 520, no. 1. Oxford University Press, pp. 364–374, 2023.","chicago":"Fleury, Leesa, Ilaria Caiazzo, and Jeremy Heyl. “The Origin of Ultramassive White Dwarfs: Hints from <i>Gaia</i> EDR3.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad068\">https://doi.org/10.1093/mnras/stad068</a>.","ama":"Fleury L, Caiazzo I, Heyl J. The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;520(1):364-374. doi:<a href=\"https://doi.org/10.1093/mnras/stad068\">10.1093/mnras/stad068</a>","ista":"Fleury L, Caiazzo I, Heyl J. 2023. The origin of ultramassive white dwarfs: hints from <i>Gaia</i> EDR3. Monthly Notices of the Royal Astronomical Society. 520(1), 364–374.","mla":"Fleury, Leesa, et al. “The Origin of Ultramassive White Dwarfs: Hints from <i>Gaia</i> EDR3.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 520, no. 1, Oxford University Press, 2023, pp. 364–74, doi:<a href=\"https://doi.org/10.1093/mnras/stad068\">10.1093/mnras/stad068</a>."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"language":[{"iso":"eng"}],"issue":"1","oa_version":"Preprint"},{"external_id":{"arxiv":["2204.00140"]},"date_created":"2024-03-26T09:49:52Z","main_file_link":[{"url":"https://arxiv.org/abs/2204.00140","open_access":"1"}],"publication_status":"published","article_processing_charge":"No","month":"01","fulldoi":"https://doi.org/10.1093/mnras/stad033","arxiv":1,"date_published":"2023-01-16T00:00:00Z","type":"journal_article","author":[{"last_name":"González-Caniulef","full_name":"González-Caniulef, Denis","first_name":"Denis"},{"last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"full_name":"Heyl, Jeremy","last_name":"Heyl","first_name":"Jeremy"}],"oa":1,"publisher":"Oxford University Press","intvolume":"       519","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","title":"Unbinned likelihood analysis for X-ray polarization","year":"2023","date_updated":"2024-04-02T07:14:49Z","doi":"10.1093/mnras/stad033","_id":"15201","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"citation":{"apa":"González-Caniulef, D., Caiazzo, I., &#38; Heyl, J. (2023). Unbinned likelihood analysis for X-ray polarization. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad033\">https://doi.org/10.1093/mnras/stad033</a>","short":"D. González-Caniulef, I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 519 (2023) 5902–5912.","chicago":"González-Caniulef, Denis, Ilaria Caiazzo, and Jeremy Heyl. “Unbinned Likelihood Analysis for X-Ray Polarization.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad033\">https://doi.org/10.1093/mnras/stad033</a>.","ieee":"D. González-Caniulef, I. Caiazzo, and J. Heyl, “Unbinned likelihood analysis for X-ray polarization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 519, no. 4. Oxford University Press, pp. 5902–5912, 2023.","ama":"González-Caniulef D, Caiazzo I, Heyl J. Unbinned likelihood analysis for X-ray polarization. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;519(4):5902-5912. doi:<a href=\"https://doi.org/10.1093/mnras/stad033\">10.1093/mnras/stad033</a>","ista":"González-Caniulef D, Caiazzo I, Heyl J. 2023. Unbinned likelihood analysis for X-ray polarization. Monthly Notices of the Royal Astronomical Society. 519(4), 5902–5912.","mla":"González-Caniulef, Denis, et al. “Unbinned Likelihood Analysis for X-Ray Polarization.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 519, no. 4, Oxford University Press, 2023, pp. 5902–12, doi:<a href=\"https://doi.org/10.1093/mnras/stad033\">10.1093/mnras/stad033</a>."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"issue":"4","language":[{"iso":"eng"}],"oa_version":"Preprint","page":"5902-5912","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","day":"16","article_type":"original","abstract":[{"text":"We present a systematic study of the unbinned, photon-by-photon likelihood technique which can be used as an alternative method to analyse phase-dependent, X-ray spectro-polarimetric observations obtained with IXPE and other photoelectric polarimeters. We apply the unbinned technique to models of the luminous X-ray pulsar Hercules X-1, for which we produce simulated observations using the IXPEOBSSIM package. We consider minimal knowledge about the actual physical process responsible for the polarized emission from the accreting pulsar and assume that the observed phase-dependent polarization angle can be described by the rotating vector model. Using the unbinned technique, the detector’s modulation factor, and the polarization information alone, we found that both the rotating vector model and the underlying spectro-polarimetry model can reconstruct equally well the geometric configuration angles of the accreting pulsar. However, the measured polarization fraction becomes biased with respect to the underlying model unless the energy dispersion and effective area of the detector are also taken into account. To this end, we present an energy-dispersed likelihood estimator that is proved to be unbiased. For different analyses, we obtain posterior distributions from multiple IXPEOBSSIM realizations and show that the unbinned technique yields \r\n smaller error bars than the binned technique. We also discuss alternative sources, such as magnetars, in which the unbinned technique and the rotating vector model might be applied.","lang":"eng"}],"volume":519},{"fulldoi":"https://doi.org/10.1093/mnras/stac801","type":"journal_article","date_published":"2022-06-01T00:00:00Z","arxiv":1,"date_created":"2022-07-07T09:21:30Z","external_id":{"arxiv":["2110.11967"]},"month":"06","article_processing_charge":"No","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2110.11967","open_access":"1"}],"doi":"10.1093/mnras/stac801","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","year":"2022","date_updated":"2024-10-14T11:32:26Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","_id":"11521","publisher":"Oxford University Press","intvolume":"       512","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Pascal A.","last_name":"Oesch","full_name":"Oesch, Pascal A."},{"last_name":"Hayes","full_name":"Hayes, Matthew","first_name":"Matthew"},{"first_name":"Dawn","last_name":"Erb","full_name":"Erb, Dawn"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Ricardo","full_name":"Amorín, Ricardo","last_name":"Amorín"},{"first_name":"Sandro","full_name":"Tacchella, Sandro","last_name":"Tacchella"},{"full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","last_name":"Ana Paulino-Afonso","first_name":"Ana Paulino-Afonso"},{"last_name":"Llerena","full_name":"Llerena, Mario","first_name":"Mario"},{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"}],"oa":1,"extern":"1","language":[{"iso":"eng"}],"issue":"4","acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","oa_version":"Preprint","keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"citation":{"ieee":"J. J. Matthee <i>et al.</i>, “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>.","apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>.","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;512(4):5960-5977. doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>"},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":512,"abstract":[{"text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (⁠fesc=50 per cent⁠, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism.","lang":"eng"}],"day":"01","article_type":"original","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"5960-5977"},{"page":"2028-2055","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","article_type":"original","day":"01","abstract":[{"lang":"eng","text":"Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes."}],"volume":517,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"chicago":"Keszthelyi, Z, A de Koter, Ylva Louise Linsdotter Götberg, G Meynet, S A Brands, V Petit, M Carrington, et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>.","ieee":"Z. Keszthelyi <i>et al.</i>, “The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2. Oxford University Press, pp. 2028–2055, 2022.","apa":"Keszthelyi, Z., de Koter, A., Götberg, Y. L. L., Meynet, G., Brands, S. A., Petit, V., … ud-Doula, A. (2022). The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>","short":"Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit, M. Carrington, A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J. Ramalatswa, M.E. Shultz, A. ud-Doula, Monthly Notices of the Royal Astronomical Society 517 (2022) 2028–2055.","ista":"Keszthelyi Z, de Koter A, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington M, David-Uraz A, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME, ud-Doula A. 2022. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.","mla":"Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2, Oxford University Press, 2022, pp. 2028–55, doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>.","ama":"Keszthelyi Z, de Koter A, Götberg YLL, et al. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(2):2028-2055. doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"issue":"2","language":[{"iso":"eng"}],"oa_version":"Preprint","oa":1,"author":[{"first_name":"Z","full_name":"Keszthelyi, Z","last_name":"Keszthelyi"},{"full_name":"de Koter, A","last_name":"de Koter","first_name":"A"},{"full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter"},{"full_name":"Meynet, G","last_name":"Meynet","first_name":"G"},{"full_name":"Brands, S A","last_name":"Brands","first_name":"S A"},{"first_name":"V","last_name":"Petit","full_name":"Petit, V"},{"first_name":"M","last_name":"Carrington","full_name":"Carrington, M"},{"full_name":"David-Uraz, A","last_name":"David-Uraz","first_name":"A"},{"full_name":"Geen, S T","last_name":"Geen","first_name":"S T"},{"first_name":"C","last_name":"Georgy","full_name":"Georgy, C"},{"first_name":"R","last_name":"Hirschi","full_name":"Hirschi, R"},{"first_name":"J","full_name":"Puls, J","last_name":"Puls"},{"last_name":"Ramalatswa","full_name":"Ramalatswa, K J","first_name":"K J"},{"first_name":"M E","full_name":"Shultz, M E","last_name":"Shultz"},{"first_name":"A","full_name":"ud-Doula, A","last_name":"ud-Doula"}],"publisher":"Oxford University Press","intvolume":"       517","extern":"1","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","title":"The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities","year":"2022","date_updated":"2023-08-21T12:02:17Z","doi":"10.1093/mnras/stac2598","_id":"13452","external_id":{"arxiv":["2209.06350"]},"date_created":"2023-08-03T10:10:37Z","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2209.06350"}],"month":"12","article_processing_charge":"No","fulldoi":"https://doi.org/10.1093/mnras/stac2598","arxiv":1,"date_published":"2022-12-01T00:00:00Z","type":"journal_article"},{"scopus_import":"1","article_type":"original","day":"01","abstract":[{"lang":"eng","text":"Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes."}],"volume":517,"page":"2028-2055","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Published Version","issue":"2","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"chicago":"Keszthelyi, Z., A. de Koter, Ylva Louise Linsdotter Götberg, G. Meynet, S. A. Brands, V. Petit, M. Carrington, et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford Academic, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>.","ieee":"Z. Keszthelyi <i>et al.</i>, “The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2. Oxford Academic, pp. 2028–2055, 2022.","apa":"Keszthelyi, Z., Koter, A. de, Götberg, Y. L. L., Meynet, G., Brands, S. A., Petit, V., … A. ud-Doula, A. ud-Doula. (2022). The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford Academic. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>","short":"Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit, M. Carrington, A.D.-U. A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J. Ramalatswa, M.E. Shultz, A. ud-Doula A. ud-Doula, Monthly Notices of the Royal Astronomical Society 517 (2022) 2028–2055.","ista":"Keszthelyi Z, Koter A de, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington M, A. David-Uraz AD-U, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME, A. ud-Doula A ud-Doula. 2022. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.","mla":"Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2, Oxford Academic, 2022, pp. 2028–55, doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>.","ama":"Keszthelyi Z, Koter A de, Götberg YLL, et al. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(2):2028-2055. doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>"},"_id":"14098","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","year":"2022","date_updated":"2023-08-22T13:18:34Z","title":"The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities","doi":"10.1093/mnras/stac2598","extern":"1","oa":1,"author":[{"full_name":"Keszthelyi, Z.","last_name":"Keszthelyi","first_name":"Z."},{"first_name":"A. de","full_name":"Koter, A. de","last_name":"Koter"},{"full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter"},{"last_name":"Meynet","full_name":"Meynet, G.","first_name":"G."},{"first_name":"S. A.","last_name":"Brands","full_name":"Brands, S. A."},{"full_name":"Petit, V.","last_name":"Petit","first_name":"V."},{"first_name":"M.","last_name":"Carrington","full_name":"Carrington, M."},{"first_name":"A. David-Uraz","full_name":"A. David-Uraz, A. David-Uraz","last_name":"A. David-Uraz"},{"first_name":"S. T.","full_name":"Geen, S. T.","last_name":"Geen"},{"full_name":"Georgy, C.","last_name":"Georgy","first_name":"C."},{"last_name":"Hirschi","full_name":"Hirschi, R.","first_name":"R."},{"first_name":"J.","full_name":"Puls, J.","last_name":"Puls"},{"first_name":"K. J.","full_name":"Ramalatswa, K. J.","last_name":"Ramalatswa"},{"full_name":"Shultz, M. E.","last_name":"Shultz","first_name":"M. E."},{"full_name":"A. ud-Doula, A. ud-Doula","last_name":"A. ud-Doula","first_name":"A. ud-Doula"}],"publisher":"Oxford Academic","intvolume":"       517","arxiv":1,"type":"journal_article","date_published":"2022-12-01T00:00:00Z","fulldoi":"https://doi.org/10.1093/mnras/stac2598","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stac2598"}],"article_processing_charge":"No","month":"12","external_id":{"arxiv":["2209.06350"]},"date_created":"2023-08-21T10:11:21Z"},{"external_id":{"arxiv":["2107.06828"]},"date_created":"2024-03-26T09:51:55Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2107.06828"}],"publication_status":"published","article_processing_charge":"No","month":"09","fulldoi":"https://doi.org/10.1093/mnras/stac2740","arxiv":1,"type":"journal_article","date_published":"2022-09-28T00:00:00Z","author":[{"first_name":"Katherine","full_name":"Rink, Katherine","last_name":"Rink"},{"last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"first_name":"Jeremy","full_name":"Heyl, Jeremy","last_name":"Heyl"}],"oa":1,"intvolume":"       517","publisher":"Oxford University Press","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","title":"Testing general relativity using quasi-periodic oscillations from X-ray black holes: XTE J1550-564 and GRO J1655-40","year":"2022","date_updated":"2024-04-02T07:18:07Z","doi":"10.1093/mnras/stac2740","_id":"15206","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"short":"K. Rink, I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 517 (2022) 1389–1397.","apa":"Rink, K., Caiazzo, I., &#38; Heyl, J. (2022). Testing general relativity using quasi-periodic oscillations from X-ray black holes: XTE J1550-564 and GRO J1655-40. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac2740\">https://doi.org/10.1093/mnras/stac2740</a>","chicago":"Rink, Katherine, Ilaria Caiazzo, and Jeremy Heyl. “Testing General Relativity Using Quasi-Periodic Oscillations from X-Ray Black Holes: XTE J1550-564 and GRO J1655-40.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2740\">https://doi.org/10.1093/mnras/stac2740</a>.","ieee":"K. Rink, I. Caiazzo, and J. Heyl, “Testing general relativity using quasi-periodic oscillations from X-ray black holes: XTE J1550-564 and GRO J1655-40,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 1. Oxford University Press, pp. 1389–1397, 2022.","ama":"Rink K, Caiazzo I, Heyl J. Testing general relativity using quasi-periodic oscillations from X-ray black holes: XTE J1550-564 and GRO J1655-40. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(1):1389-1397. doi:<a href=\"https://doi.org/10.1093/mnras/stac2740\">10.1093/mnras/stac2740</a>","mla":"Rink, Katherine, et al. “Testing General Relativity Using Quasi-Periodic Oscillations from X-Ray Black Holes: XTE J1550-564 and GRO J1655-40.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 1, Oxford University Press, 2022, pp. 1389–97, doi:<a href=\"https://doi.org/10.1093/mnras/stac2740\">10.1093/mnras/stac2740</a>.","ista":"Rink K, Caiazzo I, Heyl J. 2022. Testing general relativity using quasi-periodic oscillations from X-ray black holes: XTE J1550-564 and GRO J1655-40. Monthly Notices of the Royal Astronomical Society. 517(1), 1389–1397."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"issue":"1","language":[{"iso":"eng"}],"oa_version":"Preprint","page":"1389-1397","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","article_type":"original","day":"28","abstract":[{"lang":"eng","text":"We use the Relativistic Precession Model (RPM) and quasi-periodic oscillation (QPO) observations from the Rossi X-ray Timing Explorer to derive constraints on the properties of the black holes that power these sources and to test general relativity (GR) in the strong field regime. We build upon past techniques by using pairs of simultaneously measured QPOs, rather than triplets, and by including characteristic frequencies from the broad noise components of the power spectra in our fits. We find the inclusion of these broad noise components causes an overestimate in masses and underestimate in spins compared to values derived independently from optical spectra. We extend the underlying space-time metric to constrain potential deviations from the predictions of GR for astrophysical black holes. To do this, we modify the RPM model to a Kerr–Newman–deSitter space-time and model changes in the radial, ecliptic, and vertical frequencies. We compare our models with X-ray data of XTE J1550-564 and GRO J1655-40 using robust statistical techniques to constrain the parameters of the black holes and the deviations from GR. For both sources, using QPO and characteristic frequency data, we constrain particular deviations from GR to be less than one part per thousand."}],"volume":517},{"title":"Probing magnetar emission mechanisms with X-ray spectropolarimetry","year":"2022","date_updated":"2024-10-14T12:32:39Z","doi":"10.1093/mnras/stac1571","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","_id":"15208","publisher":"Oxford University Press","intvolume":"       514","author":[{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria"},{"full_name":"González-Caniulef, Denis","last_name":"González-Caniulef","first_name":"Denis"},{"last_name":"Heyl","full_name":"Heyl, Jeremy","first_name":"Jeremy"},{"last_name":"Fernández","full_name":"Fernández, Rodrigo","first_name":"Rodrigo"}],"oa":1,"extern":"1","fulldoi":"https://doi.org/10.1093/mnras/stac1571","type":"journal_article","date_published":"2022-06-09T00:00:00Z","arxiv":1,"date_created":"2024-03-26T09:52:41Z","external_id":{"arxiv":["2112.03401"]},"article_processing_charge":"No","month":"06","main_file_link":[{"url":"https://arxiv.org/abs/2112.03401","open_access":"1"}],"publication_status":"published","abstract":[{"lang":"eng","text":"This year, a new era of observations of compact objects in X-ray polarization is commencing. Among the key targets for the Imaging X-ray Polarimetry Explorer mission are the magnetars 4U 0142+61 and 1RXS J170849.0-400910. Here, we present detailed predictions of the expected polarization from these sources that incorporate realistic models of emission physics at the surface (gaseous or condensed), the temperature distribution on the surface, general relativity, quantum electrodynamics, and scattering in the magnetosphere, accounting for the broad-band spectral energy distribution from below 1 keV to nearly 100 keV. We find that either atmospheres or condensed surfaces can account for the emission at a few keV. In both cases, either a small hot polar cap or scattering is required to account for the emission at 5–10 keV and, above 10 keV, scattering by a hard population of electrons can account for the rising power in the hard X-rays observed in many magnetars in quiescence. Although these different scenarios result in very similar spectral energy distributions, they generate dramatically different polarization signatures from 2 to 8 keV, which is the range of sensitivity of the Imaging X-ray Polarimetry Explorer. Observations of these sources in X-ray polarization will therefore probe the emission from magnetars in an essentially new way."}],"volume":514,"scopus_import":"1","article_type":"original","day":"09","publication":"Monthly Notices of the Royal Astronomical Society","page":"5024-5034","language":[{"iso":"eng"}],"issue":"4","oa_version":"Preprint","citation":{"short":"I. Caiazzo, D. González-Caniulef, J. Heyl, R. Fernández, Monthly Notices of the Royal Astronomical Society 514 (2022) 5024–5034.","apa":"Caiazzo, I., González-Caniulef, D., Heyl, J., &#38; Fernández, R. (2022). Probing magnetar emission mechanisms with X-ray spectropolarimetry. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac1571\">https://doi.org/10.1093/mnras/stac1571</a>","chicago":"Caiazzo, Ilaria, Denis González-Caniulef, Jeremy Heyl, and Rodrigo Fernández. “Probing Magnetar Emission Mechanisms with X-Ray Spectropolarimetry.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac1571\">https://doi.org/10.1093/mnras/stac1571</a>.","ieee":"I. Caiazzo, D. González-Caniulef, J. Heyl, and R. Fernández, “Probing magnetar emission mechanisms with X-ray spectropolarimetry,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 514, no. 4. Oxford University Press, pp. 5024–5034, 2022.","ama":"Caiazzo I, González-Caniulef D, Heyl J, Fernández R. Probing magnetar emission mechanisms with X-ray spectropolarimetry. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;514(4):5024-5034. doi:<a href=\"https://doi.org/10.1093/mnras/stac1571\">10.1093/mnras/stac1571</a>","mla":"Caiazzo, Ilaria, et al. “Probing Magnetar Emission Mechanisms with X-Ray Spectropolarimetry.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 514, no. 4, Oxford University Press, 2022, pp. 5024–34, doi:<a href=\"https://doi.org/10.1093/mnras/stac1571\">10.1093/mnras/stac1571</a>.","ista":"Caiazzo I, González-Caniulef D, Heyl J, Fernández R. 2022. Probing magnetar emission mechanisms with X-ray spectropolarimetry. Monthly Notices of the Royal Astronomical Society. 514(4), 5024–5034."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]}}]