[{"publisher":"IOP Publishing","oa_version":"Published Version","type":"journal_article","year":"2026","day":"01","intvolume":"       996","OA_type":"gold","status":"public","article_number":"69","fulldoi":"https://doi.org/10.3847/1538-4357/ae18c8","has_accepted_license":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"file":[{"success":1,"file_id":"21733","content_type":"application/pdf","date_updated":"2026-04-13T08:36:50Z","checksum":"65a8237a519188af83b6dc4d47ad85fa","relation":"main_file","creator":"dernst","file_size":19310053,"access_level":"open_access","file_name":"2026_AstrophysicalJournal_Miller.pdf","date_created":"2026-04-13T08:36:50Z"}],"quality_controlled":"1","volume":996,"abstract":[{"lang":"eng","text":"The initial–final mass relation (IFMR) links a star’s birth mass to the mass of its white dwarf (WD) remnant, providing key constraints on stellar evolution. Open clusters offer the most straightforward way to empirically determine the IFMR, as their well-defined ages allow for direct progenitor lifetime estimates. We construct the most comprehensive open cluster WD IFMR to date by combining new spectroscopy of 22 WDs with an extensive literature review of WDs with strong cluster associations. To minimize systematics, we restrict our analysis to spectroscopically confirmed hydrogen-atmosphere (DA) WDs consistent with single-stellar origins. We separately analyze a subset with reliable Gaia-based astrometric membership assessments, as well as a full sample that adds WDs with strong cluster associations whose membership cannot be reliably assessed with Gaia. The Gaia-based sample includes 69 spectroscopically confirmed DA WDs, more than doubling the sample size of previous Gaia-based open cluster IFMRs. The full sample, which includes 53 additional literature WDs,\r\nincreases the total number of cluster WDs by over 50% relative to earlier works. We provide functional forms for both the Gaia-based and full-sample IFMRs. The Gaia-based result useful for Mi � 2.67 M⊙ is Mf = [0.179 0.100H (Mi 3.84 M )] × (Mi 3.84 M ) + 0.628 M , where H(x) is the Heaviside step function. Comparing our IFMR to recent literature, we identify significant deviations from best-fit IFMRs derived from both Gaia-based volume-limited samples of field WDs and double WD binaries, with the largest discrepancy occurring for initial masses of about 5 M⊙."}],"doi":"10.3847/1538-4357/ae18c8","publication":"The Astrophysical Journal","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"_id":"21725","publication_status":"published","DOAJ_listed":"1","external_id":{"arxiv":["2510.24877"]},"acknowledgement":"The authors would like to thank the anonymous referee for their constructive feedback, which helped improve the clarify of the manuscript. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada Discovery grants Nos. DG-RGPIN-2022-03051 and DG-RGPIN-2023-04486. This research received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program number 101002408 (MOS100PC). This work includes results based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the 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. Gemini spectra were processed using the DRAGONS package (K. Labrie et al. 2023). LRIS spectra were reduced using the Lpipe pipeline (D. A. Perley 2019).\r\n\r\nFacilities: Gaia - (DR2 & DR3), Gemini:Gillett - Gillett Gemini North Telescope (GMOS-N), Gemini:South - Gemini South Telescope (GMOS-S), Keck:I - KECK I Telescope (LRIS).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2013,2018, 2022), emcee (D. Foreman-Mackey et al. 2013).","article_type":"original","keyword":["White dwarf stars","Open star clusters","Compact objects","Stellar evolution"],"language":[{"iso":"eng"}],"date_created":"2026-04-12T22:01:52Z","article_processing_charge":"Yes","title":"The White Dwarf initial–final mass relation from open clusters in Gaia DR3","department":[{"_id":"IlCa"}],"file_date_updated":"2026-04-13T08:36:50Z","scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"author":[{"last_name":"Miller","first_name":"David R.","full_name":"Miller, David R."},{"id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","first_name":"Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo"},{"last_name":"Heyl","full_name":"Heyl, Jeremy","first_name":"Jeremy"},{"last_name":"Richer","first_name":"Harvey B.","full_name":"Richer, Harvey B."},{"full_name":"Hollands, Mark A.","first_name":"Mark A.","last_name":"Hollands"},{"first_name":"Pier Emmanuel","full_name":"Tremblay, Pier Emmanuel","last_name":"Tremblay"},{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P.","last_name":"Vanderbosch"}],"date_updated":"2026-04-13T08:39:39Z","arxiv":1,"OA_place":"publisher","issue":"1","citation":{"chicago":"Miller, David R., Ilaria Caiazzo, Jeremy Heyl, Harvey B. Richer, Mark A. Hollands, Pier Emmanuel Tremblay, Kareem El-Badry, Antonio C. Rodriguez, and Zachary P. Vanderbosch. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” <i>The Astrophysical Journal</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">https://doi.org/10.3847/1538-4357/ae18c8</a>.","ista":"Miller DR, Caiazzo I, Heyl J, Richer HB, Hollands MA, Tremblay PE, El-Badry K, Rodriguez AC, Vanderbosch ZP. 2026. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. The Astrophysical Journal. 996(1), 69.","ieee":"D. R. Miller <i>et al.</i>, “The White Dwarf initial–final mass relation from open clusters in Gaia DR3,” <i>The Astrophysical Journal</i>, vol. 996, no. 1. IOP Publishing, 2026.","short":"D.R. Miller, I. Caiazzo, J. Heyl, H.B. Richer, M.A. Hollands, P.E. Tremblay, K. El-Badry, A.C. Rodriguez, Z.P. Vanderbosch, The Astrophysical Journal 996 (2026).","apa":"Miller, D. R., Caiazzo, I., Heyl, J., Richer, H. B., Hollands, M. A., Tremblay, P. E., … Vanderbosch, Z. P. (2026). The White Dwarf initial–final mass relation from open clusters in Gaia DR3. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">https://doi.org/10.3847/1538-4357/ae18c8</a>","ama":"Miller DR, Caiazzo I, Heyl J, et al. The White Dwarf initial–final mass relation from open clusters in Gaia DR3. <i>The Astrophysical Journal</i>. 2026;996(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">10.3847/1538-4357/ae18c8</a>","mla":"Miller, David R., et al. “The White Dwarf Initial–Final Mass Relation from Open Clusters in Gaia DR3.” <i>The Astrophysical Journal</i>, vol. 996, no. 1, 69, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/1538-4357/ae18c8\">10.3847/1538-4357/ae18c8</a>."},"ddc":["520"],"date_published":"2026-01-01T00:00:00Z","PlanS_conform":"1","month":"01"},{"day":"09","type":"journal_article","year":"2026","publisher":"Oxford University Press","oa_version":"Published Version","article_number":"stag673","fulldoi":"https://doi.org/10.1093/mnras/stag673","OA_type":"gold","status":"public","intvolume":"       548","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","volume":548,"file":[{"file_name":"2026_MNRAS_Green.pdf","access_level":"open_access","file_size":3960296,"date_created":"2026-05-21T06:37:42Z","content_type":"application/pdf","file_id":"21903","success":1,"creator":"dernst","relation":"main_file","checksum":"2c4463926c5cb84ce555ef2005b52ddd","date_updated":"2026-05-21T06:37:42Z"}],"quality_controlled":"1","oa":1,"publication_status":"published","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"_id":"21897","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"Ultracompact binary systems, consisting of two compact objects in an orbit $\\lesssim 0.5 {\\rm R}_\\odot$, should exhibit measurable rates of orbital period change ($\\dot{P} \\ne 0$) due to the emission of gravitational waves (GWs). Measurements of $\\dot{P}$ have so far been limited to the shortest-period ultracompact binaries ($\\lesssim 20$  min). Among the AM CVn-type subclass, several works have proposed the presence of extra angular momentum loss beyond GW emission, with magnetic braking being a widely discussed mechanism. If present, this magnetic braking would dominate the angular momentum loss of AM CVn-type binaries with orbital periods $\\gtrsim 30$ min. In this work, we present a long-term eclipse timing study of two AM CVn-type binaries, YZ LMi and Gaia14aae, with respective orbital periods of 28.3 min and 49.7 min and continuous observations since 2006 and 2015. Both systems show $\\dot{P}$ consistent with zero within $2\\sigma$. Their $3\\sigma$ upper limits are $1.1 \\times 10^{-13}\\, {\\rm s \\, s}^{-1}$ and $9.7 \\times 10^{-14}\\, {\\rm s \\, s}^{-1}$, respectively. These non-detections are most simply explained by a scenario in which secular angular momentum loss is not substantially stronger than GW emission at all orbital periods, but is combined with deviations from the secular $\\dot{P}$ whose time-scales span decades but whose amplitude is $\\lesssim 10^{-13}\\, {\\rm s \\, s}^{-1}$. Our non-detections of $\\dot{P}$ represent a limit on the strength of any enhanced angular momentum loss beyond pure GW emission.","lang":"eng"}],"doi":"10.1093/mnras/stag673","DOAJ_listed":"1","acknowledgement":"We are grateful to the anonymousreferee fortheirinsightful comments. MJG thanks Mitch Begelman and the JILA department at the University of Colorado, Boulder, for providing office space at which much of this paper was written. This work is supported in part by the United States National Aeronautics and Space Administration (NASA) under grants\r\n80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380, and the United States National Science Foundation (NSF) under grant AST-2508429. VSD and HiPERCAM are funded by the Science and Technology Facilities Council (grant ST/Z000033/1). IP acknowledges support from the Royal Society through a University Research Fellowship (URF\\R1\\231496). This project has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement numbers 101002408 – MOS100PC). CMC receives funding from United Kingdom Research and Innovation grant numbers ST/X005933/1 and ST/W001934/1. This article is based in part on observations made in the Observatorios de Canarias del Instituto de Astrofísica de Canarias (IAC) with the the William Herschel Telescope (WHT) operated on the island of La Palma by the Isaac Newton Group (ING) in the Observatorio del Roque de los Muchachos. It is also based in part on observations made with the Gran Telescopio Canarias (GTC) under proposal ID GTC18-24A, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Further data were obtained using the 2.4 m Thai National Telescope (TNT) operated by the National Astronomy Research Institute of Thailand\r\n(NARIT), and the 200-inch Hale Telescope at Palomar Observatory operated by the California Institute of Technology. Software packages used in this work include the ultracam and hipercam reduction pipelines, lcurve (C. M. Copperwheat et al. 2010), numpy, astropy, matplotlib, and emcee (D. Foreman-Mackey et al. 2013).","external_id":{"arxiv":["2604.06460"]},"article_type":"original","date_created":"2026-05-20T14:34:03Z","language":[{"iso":"eng"}],"keyword":["binaries: close – stars","dwarf novae – novae","cataclysmic variables – white dwarfs"],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","department":[{"_id":"IlCa"}],"file_date_updated":"2026-05-21T06:37:42Z","title":"No period change in two long-period AM CVn binaries","article_processing_charge":"Yes","date_updated":"2026-05-21T06:41:41Z","author":[{"last_name":"Green","full_name":"Green, Matthew J","first_name":"Matthew J"},{"first_name":"Thomas R","full_name":"Marsh, Thomas R","last_name":"Marsh"},{"last_name":"van Roestel","first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","full_name":"van Roestel, Joannes C"},{"last_name":"Wong","full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny"},{"first_name":"Diogo","full_name":"Belloni, Diogo","last_name":"Belloni"},{"full_name":"Kilic, Mukremin","first_name":"Mukremin","last_name":"Kilic"},{"last_name":"Breedt","first_name":"Elmé","full_name":"Breedt, Elmé"},{"full_name":"Brown, Alex","first_name":"Alex","last_name":"Brown"},{"first_name":"Chris M","full_name":"Copperwheat, Chris M","last_name":"Copperwheat"},{"first_name":"Anurak","full_name":"Chakpor, Anurak","last_name":"Chakpor"},{"full_name":"Dhillon, V S","first_name":"V S","last_name":"Dhillon"},{"first_name":"Noel Castro","full_name":"Segura, Noel Castro","last_name":"Segura"},{"last_name":"Dyer","first_name":"Martin J","full_name":"Dyer, Martin J"},{"last_name":"Garbutt","first_name":"James","full_name":"Garbutt, James"},{"first_name":"Dan","full_name":"Jarvis, Dan","last_name":"Jarvis"},{"last_name":"Kengkriangkrai","full_name":"Kengkriangkrai, Vasu","first_name":"Vasu"},{"last_name":"Kennedy","full_name":"Kennedy, Mark R","first_name":"Mark R"},{"last_name":"Kerry","first_name":"Paul","full_name":"Kerry, Paul"},{"last_name":"Kupfer","full_name":"Kupfer, Thomas","first_name":"Thomas"},{"full_name":"Littlefair, S P","first_name":"S P","last_name":"Littlefair"},{"first_name":"James","full_name":"McCormac, James","last_name":"McCormac"},{"last_name":"Munday","full_name":"Munday, James","first_name":"James"},{"last_name":"Parsons","full_name":"Parsons, Steven G","first_name":"Steven G"},{"first_name":"Eleanor","full_name":"Pike, Eleanor","last_name":"Pike"},{"last_name":"Pelisoli","full_name":"Pelisoli, Ingrid","first_name":"Ingrid"},{"full_name":"Rodríguez-Gil, Pablo","first_name":"Pablo","last_name":"Rodríguez-Gil"},{"last_name":"Sahman","full_name":"Sahman, David I","first_name":"David I"},{"last_name":"Yates","full_name":"Yates, Amalie","first_name":"Amalie"}],"citation":{"apa":"Green, M. J., Marsh, T. R., van Roestel, J. C., Wong, T. L. S., Belloni, D., Kilic, M., … Yates, A. (2026). No period change in two long-period AM CVn binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stag673\">https://doi.org/10.1093/mnras/stag673</a>","ama":"Green MJ, Marsh TR, van Roestel JC, et al. No period change in two long-period AM CVn binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. 2026;548(3). doi:<a href=\"https://doi.org/10.1093/mnras/stag673\">10.1093/mnras/stag673</a>","mla":"Green, Matthew J., et al. “No Period Change in Two Long-Period AM CVn Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 548, no. 3, stag673, Oxford University Press, 2026, doi:<a href=\"https://doi.org/10.1093/mnras/stag673\">10.1093/mnras/stag673</a>.","ieee":"M. J. Green <i>et al.</i>, “No period change in two long-period AM CVn binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 548, no. 3. Oxford University Press, 2026.","chicago":"Green, Matthew J, Thomas R Marsh, Joannes C van Roestel, Tin Long Sunny Wong, Diogo Belloni, Mukremin Kilic, Elmé Breedt, et al. “No Period Change in Two Long-Period AM CVn Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2026. <a href=\"https://doi.org/10.1093/mnras/stag673\">https://doi.org/10.1093/mnras/stag673</a>.","ista":"Green MJ, Marsh TR, van Roestel JC, Wong TLS, Belloni D, Kilic M, Breedt E, Brown A, Copperwheat CM, Chakpor A, Dhillon VS, Segura NC, Dyer MJ, Garbutt J, Jarvis D, Kengkriangkrai V, Kennedy MR, Kerry P, Kupfer T, Littlefair SP, McCormac J, Munday J, Parsons SG, Pike E, Pelisoli I, Rodríguez-Gil P, Sahman DI, Yates A. 2026. No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. 548(3), stag673.","short":"M.J. Green, T.R. Marsh, J.C. van Roestel, T.L.S. Wong, D. Belloni, M. Kilic, E. Breedt, A. Brown, C.M. Copperwheat, A. Chakpor, V.S. Dhillon, N.C. Segura, M.J. Dyer, J. Garbutt, D. Jarvis, V. Kengkriangkrai, M.R. Kennedy, P. Kerry, T. Kupfer, S.P. Littlefair, J. McCormac, J. Munday, S.G. Parsons, E. Pike, I. Pelisoli, P. Rodríguez-Gil, D.I. Sahman, A. Yates, Monthly Notices of the Royal Astronomical Society 548 (2026)."},"issue":"3","OA_place":"publisher","arxiv":1,"date_published":"2026-04-09T00:00:00Z","ddc":["520"],"month":"04","PlanS_conform":"1"},{"researchdata_availability":"no","day":"30","type":"journal_article","year":"2026","oa_version":"Published Version","publisher":"Maynooth Academic Publishing","fulldoi":"https://doi.org/10.33232/001c.164326","OA_type":"gold","status":"public","intvolume":"         9","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","volume":9,"quality_controlled":"1","file":[{"content_type":"application/pdf","file_id":"22282","success":1,"creator":"dernst","relation":"main_file","checksum":"6320fd19e5ea3399f332be5aab022736","date_updated":"2026-07-13T09:05:36Z","file_name":"2026_OpenJourAstrophysics_ElBadry.pdf","access_level":"open_access","file_size":1994596,"date_created":"2026-07-13T09:05:36Z"}],"oa":1,"_id":"22270","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"publication_status":"published","publication":"The Open Journal of Astrophysics","doi":"10.33232/001c.164326","abstract":[{"text":"The explosion of a white dwarf (WD) in a close binary can launch a surviving runaway star at\r\nvelocities of ≳ 1000 km s−1\r\n. Such runaways provide a direct probe of thermonuclear supernovae (SNe)\r\nin double-degenerate binaries. Several candidate runaways are known, but their evolutionary states\r\nand the demographics of the broader population are uncertain. To enable robust population inference,\r\nwe carry out a systematic survey for hypervelocity runaways with a simple selection function, selecting\r\ncandidates based on large Gaia-inferred tangential velocities and blue colors. We classify 100% of the\r\nresulting 92 candidates using a combination of spectroscopic follow-up and archival data. The search\r\nyields ten suspected D6\r\nstars and three LP 40-365 stars. Three D6\r\nstars are new discoveries, including\r\ntwo hot (Teff ≳ 50,000 K) objects and one cool (Teff ≈ 7,000 K) object. We forward-model our survey\r\nunder several proposed D6\r\nstar evolutionary models, coupling each to a Galactic model and the survey\r\nselection function. No single model reproduces the observed diversity of D6\r\nstars, which likely reflects\r\na range of remnant masses, ages, and heating mechanisms. Models in which runaway companions\r\nare heated by SN shocks alone are too faint and short-lived to explain most of the observed sample,\r\nwhile fully reheated models are too luminous and long-lived. Models with intermediate heating,\r\nas occurs in some simulations of violent mergers and partially disrupted remnants, best match the\r\nobserved magnitude, distance, and kinematic-age distributions. The inferred D6\r\nstar birth rate is\r\nmodel dependent, but the models that best match the observed population require rates of only a\r\nfew percent of the Galactic SN Ia rate, perhaps implying that most SNe Ia result from WD binaries\r\nin which both components explode. If most SNe Ia do produce surviving runaways, these must be\r\nfainter or shorter-lived than the currently known runaways.","lang":"eng"}],"DOAJ_listed":"1","acknowledgement":"We thank Lars Bildsten, Evan Bauer, Ruediger Pakmor, Jim Fuller, Logan Proust, Abinaya Rajamuthukumar, and Stephan Geier for useful discussion related to\r\nthis work.\r\nThis work was supported by NSF grants AST-2508988\r\nand AST-2205631, NASA/ESA Hubble Space Telescope\r\nprogram No. 17441, and Scialog grant #SA-LSST-2024-\r\n114c from the Research Corporation for Science Advancement. The Kavli Institute for Theoretical Physics\r\n(KITP) hosted the program, “White Dwarfs as Probes of\r\nthe Evolution of Planets, Stars, the Milky Way, and the\r\nExpanding Universe,” during which this project was initiated. This research was supported in part by the U.S.\r\nNational Science Foundation (NSF) under grants PHY1748958. This research benefited from discussions that\r\nwere funded by the Gordon and Betty Moore Foundation\r\nthrough Grant GBMF5076.\r\nWe thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the observatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","external_id":{"arxiv":["2606.11293"]},"dataavailabilitystatement":"We thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the\r\nobservatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","article_type":"original","date_created":"2026-07-12T22:02:19Z","language":[{"iso":"eng"}],"keyword":["white dwarfs","binaries: close","stars: chemically peculiar"],"publication_identifier":{"eissn":["2565-6120"]},"scopus_import":"1","department":[{"_id":"IlCa"}],"file_date_updated":"2026-07-13T09:05:36Z","article_processing_charge":"No","title":"A systematic survey for hypervelocity runaways from thermonuclear supernovae","date_updated":"2026-07-13T09:09:34Z","supplementarymaterial":"no","author":[{"last_name":"El-Badry","first_name":"Kareem","full_name":"El-Badry, Kareem"},{"first_name":"Klaus","full_name":"Werner, Klaus","last_name":"Werner"},{"last_name":"Shen","first_name":"Ken J.","full_name":"Shen, Ken J."},{"full_name":"Strader, Jay","first_name":"Jay","last_name":"Strader"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"full_name":"Han, Jiwon Jesse","first_name":"Jiwon Jesse","last_name":"Han"},{"first_name":"Vedant","full_name":"Chandra, Vedant","last_name":"Chandra"},{"last_name":"Chomiuk","first_name":"Laura","full_name":"Chomiuk, Laura"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P."},{"first_name":"Lisa","full_name":"Blomberg, Lisa","last_name":"Blomberg"},{"first_name":"Natsuko","full_name":"Yamaguchi, Natsuko","last_name":"Yamaguchi"},{"first_name":"Pranav","full_name":"Nagarajan, Pranav","last_name":"Nagarajan"},{"last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","first_name":"Ilaria"},{"id":"4d122fc8-6083-11f0-87a5-97d68b860333","first_name":"Joannes C","full_name":"van Roestel, Joannes C","last_name":"van Roestel"},{"full_name":"Glanz, Hila","first_name":"Hila","last_name":"Glanz"},{"first_name":"Tin Long Sunny","full_name":"Wong, Tin Long Sunny","last_name":"Wong"},{"first_name":"Aakash","full_name":"Bhat, Aakash","last_name":"Bhat"},{"last_name":"Hollands","first_name":"Mark A.","full_name":"Hollands, Mark A."}],"citation":{"ama":"El-Badry K, Werner K, Shen KJ, et al. A systematic survey for hypervelocity runaways from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>. 2026;9. doi:<a href=\"https://doi.org/10.33232/001c.164326\">10.33232/001c.164326</a>","mla":"El-Badry, Kareem, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>, vol. 9, Maynooth Academic Publishing, 2026, doi:<a href=\"https://doi.org/10.33232/001c.164326\">10.33232/001c.164326</a>.","apa":"El-Badry, K., Werner, K., Shen, K. J., Strader, J., Rodriguez, A. C., Han, J. J., … Hollands, M. A. (2026). A systematic survey for hypervelocity runaways from thermonuclear supernovae. <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing. <a href=\"https://doi.org/10.33232/001c.164326\">https://doi.org/10.33232/001c.164326</a>","short":"K. El-Badry, K. Werner, K.J. Shen, J. Strader, A.C. Rodriguez, J.J. Han, V. Chandra, L. Chomiuk, Z.P. Vanderbosch, L. Blomberg, N. Yamaguchi, P. Nagarajan, I. Caiazzo, J.C. van Roestel, H. Glanz, T.L.S. Wong, A. Bhat, M.A. Hollands, The Open Journal of Astrophysics 9 (2026).","ieee":"K. El-Badry <i>et al.</i>, “A systematic survey for hypervelocity runaways from thermonuclear supernovae,” <i>The Open Journal of Astrophysics</i>, vol. 9. Maynooth Academic Publishing, 2026.","ista":"El-Badry K, Werner K, Shen KJ, Strader J, Rodriguez AC, Han JJ, Chandra V, Chomiuk L, Vanderbosch ZP, Blomberg L, Yamaguchi N, Nagarajan P, Caiazzo I, van Roestel JC, Glanz H, Wong TLS, Bhat A, Hollands MA. 2026. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 9.","chicago":"El-Badry, Kareem, Klaus Werner, Ken J. Shen, Jay Strader, Antonio C. Rodriguez, Jiwon Jesse Han, Vedant Chandra, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” <i>The Open Journal of Astrophysics</i>. Maynooth Academic Publishing, 2026. <a href=\"https://doi.org/10.33232/001c.164326\">https://doi.org/10.33232/001c.164326</a>."},"OA_place":"publisher","arxiv":1,"date_published":"2026-06-30T00:00:00Z","ddc":["520"],"PlanS_conform":"1","month":"06","das_tickbox":"1"},{"ddc":["520"],"date_published":"2026-06-01T00:00:00Z","PlanS_conform":"1","month":"06","das_tickbox":"1","date_updated":"2026-07-13T14:36:24Z","author":[{"last_name":"Perley","full_name":"Perley, Daniel A","first_name":"Daniel A"},{"last_name":"Ho","first_name":"Anna Y Q","full_name":"Ho, Anna Y Q"},{"last_name":"McGrath","full_name":"McGrath, Zoë","first_name":"Zoë"},{"first_name":"Michael","full_name":"Camilo, Michael","last_name":"Camilo"},{"full_name":"Sevilla, Cassie","first_name":"Cassie","last_name":"Sevilla"},{"first_name":"Ping","full_name":"Chen, Ping","last_name":"Chen"},{"first_name":"Genevieve","full_name":"Schroeder, Genevieve","last_name":"Schroeder"},{"first_name":"Taya","full_name":"Govreen-Segal, Taya","last_name":"Govreen-Segal"},{"first_name":"Aleksandra","full_name":"Bochenek, Aleksandra","last_name":"Bochenek"},{"last_name":"Qin","first_name":"Yu-Jing","full_name":"Qin, Yu-Jing"},{"last_name":"Gillanders","full_name":"Gillanders, James H","first_name":"James H"},{"last_name":"Amend","first_name":"Benjamin","full_name":"Amend, Benjamin"},{"last_name":"Anderson","first_name":"Joseph P","full_name":"Anderson, Joseph P"},{"last_name":"Andreoni","first_name":"Igor","full_name":"Andreoni, Igor"},{"full_name":"Aryan, Amar","first_name":"Amar","last_name":"Aryan"},{"last_name":"Bellm","full_name":"Bellm, Eric C","first_name":"Eric C"},{"first_name":"Joshua S","full_name":"Bloom, Joshua S","last_name":"Bloom"},{"full_name":"de Boer, Thomas","first_name":"Thomas","last_name":"de Boer"},{"first_name":"Jonathan","full_name":"Carney, Jonathan","last_name":"Carney"},{"full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388","last_name":"Caiazzo"},{"last_name":"Chambers","first_name":"Ken C","full_name":"Chambers, Ken C"},{"last_name":"Charalampopoulos","first_name":"Panos","full_name":"Charalampopoulos, Panos"},{"first_name":"Ting-Wan","full_name":"Chen, Ting-Wan","last_name":"Chen"},{"last_name":"Chen","full_name":"Chen, Tracy X","first_name":"Tracy X"},{"first_name":"Eric R","full_name":"Coughlin, Eric R","last_name":"Coughlin"},{"last_name":"Coughlin","full_name":"Coughlin, Michael","first_name":"Michael"},{"last_name":"Dennefeld","full_name":"Dennefeld, Michel","first_name":"Michel"},{"first_name":"Georgios","full_name":"Dimitriadis, Georgios","last_name":"Dimitriadis"},{"last_name":"Fremling","full_name":"Fremling, Christoffer","first_name":"Christoffer"},{"last_name":"Frostig","first_name":"Danielle","full_name":"Frostig, Danielle"},{"full_name":"Gal-Yam, Avishay","first_name":"Avishay","last_name":"Gal-Yam"},{"last_name":"Galbany","full_name":"Galbany, Lluís","first_name":"Lluís"},{"last_name":"Gangopadhyay","first_name":"Anjashay","full_name":"Gangopadhyay, Anjashay"},{"first_name":"Melzie","full_name":"Ghendrih, Melzie","last_name":"Ghendrih"},{"last_name":"Graham","first_name":"Matthew J","full_name":"Graham, Matthew J"},{"first_name":"Mariusz","full_name":"Gromadzki, Mariusz","last_name":"Gromadzki"},{"full_name":"Groom, Steven L","first_name":"Steven L","last_name":"Groom"},{"last_name":"Gutiérrez","full_name":"Gutiérrez, Claudia P","first_name":"Claudia P"},{"full_name":"Hinds, K -Ryan","first_name":"K -Ryan","last_name":"Hinds"},{"last_name":"Huber","full_name":"Huber, Mark E","first_name":"Mark E"},{"full_name":"Inserra, Cosimo","first_name":"Cosimo","last_name":"Inserra"},{"first_name":"Benjamin C","full_name":"Kaiser, Benjamin C","last_name":"Kaiser"},{"first_name":"Mansi M","full_name":"Kasliwal, Mansi M","last_name":"Kasliwal"},{"last_name":"Koivisto","full_name":"Koivisto, Niilo E","first_name":"Niilo E"},{"first_name":"Chien-Cheng","full_name":"Lin, Chien-Cheng","last_name":"Lin"},{"full_name":"Liu, Chang","first_name":"Chang","last_name":"Liu"},{"last_name":"Lowe","full_name":"Lowe, Thomas B","first_name":"Thomas B"},{"full_name":"Magnier, Eugene","first_name":"Eugene","last_name":"Magnier"},{"last_name":"Mahabal","full_name":"Mahabal, Ashish A","first_name":"Ashish A"},{"first_name":"Andrew","full_name":"Milligan, Andrew","last_name":"Milligan"},{"last_name":"Minguez","full_name":"Minguez, Paloma","first_name":"Paloma"},{"first_name":"Geoffrey","full_name":"Mo, Geoffrey","last_name":"Mo"},{"last_name":"Müller-Bravo","full_name":"Müller-Bravo, Tomás E","first_name":"Tomás E"},{"last_name":"Nicholl","full_name":"Nicholl, Matt","first_name":"Matt"},{"last_name":"Pessi","full_name":"Pessi, Priscila J","first_name":"Priscila J"},{"last_name":"Pignata","first_name":"Giuliano","full_name":"Pignata, Giuliano"},{"first_name":"Josiah","full_name":"Purdum, Josiah","last_name":"Purdum"},{"last_name":"Rehemtulla","first_name":"Nabeel","full_name":"Rehemtulla, Nabeel"},{"full_name":"Rich, R Michael","first_name":"R Michael","last_name":"Rich"},{"full_name":"Sahu, Anwesha","first_name":"Anwesha","last_name":"Sahu"},{"last_name":"Singh","full_name":"Singh, Avinash","first_name":"Avinash"},{"last_name":"Smartt","full_name":"Smartt, Stephen J","first_name":"Stephen J"},{"last_name":"Smith","full_name":"Smith, Ian A","first_name":"Ian A"},{"last_name":"Sollerman","first_name":"Jesper","full_name":"Sollerman, Jesper"},{"last_name":"Srinivasaragavan","full_name":"Srinivasaragavan, Gokul","first_name":"Gokul"},{"last_name":"Srivastav","full_name":"Srivastav, Shubham","first_name":"Shubham"},{"first_name":"Robert D","full_name":"Stein, Robert D","last_name":"Stein"},{"last_name":"Schulze","full_name":"Schulze, Steve","first_name":"Steve"},{"full_name":"Tweddle, Jack W","first_name":"Jack W","last_name":"Tweddle"},{"last_name":"Wainscoat","first_name":"Richard","full_name":"Wainscoat, Richard"},{"last_name":"Wise","full_name":"Wise, Jacob L","first_name":"Jacob L"},{"last_name":"Yan","first_name":"Lin","full_name":"Yan, Lin"},{"last_name":"Young","first_name":"David R","full_name":"Young, David R"}],"supplementarymaterial":"yes","citation":{"short":"D.A. Perley, A.Y.Q. Ho, Z. McGrath, M. Camilo, C. Sevilla, P. Chen, G. Schroeder, T. Govreen-Segal, A. Bochenek, Y.-J. Qin, J.H. Gillanders, B. Amend, J.P. Anderson, I. Andreoni, A. Aryan, E.C. Bellm, J.S. Bloom, T. de Boer, J. Carney, I. Caiazzo, K.C. Chambers, P. Charalampopoulos, T.-W. Chen, T.X. Chen, E.R. Coughlin, M. Coughlin, M. Dennefeld, G. Dimitriadis, C. Fremling, D. Frostig, A. Gal-Yam, L. Galbany, A. Gangopadhyay, M. Ghendrih, M.J. Graham, M. Gromadzki, S.L. Groom, C.P. Gutiérrez, K.-R. Hinds, M.E. Huber, C. Inserra, B.C. Kaiser, M.M. Kasliwal, N.E. Koivisto, C.-C. Lin, C. Liu, T.B. Lowe, E. Magnier, A.A. Mahabal, A. Milligan, P. Minguez, G. Mo, T.E. Müller-Bravo, M. Nicholl, P.J. Pessi, G. Pignata, J. Purdum, N. Rehemtulla, R.M. Rich, A. Sahu, A. Singh, S.J. Smartt, I.A. Smith, J. Sollerman, G. Srinivasaragavan, S. Srivastav, R.D. Stein, S. Schulze, J.W. Tweddle, R. Wainscoat, J.L. Wise, L. Yan, D.R. Young, Monthly Notices of the Royal Astronomical Society 549 (2026).","chicago":"Perley, Daniel A, Anna Y Q Ho, Zoë McGrath, Michael Camilo, Cassie Sevilla, Ping Chen, Genevieve Schroeder, et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2026. <a href=\"https://doi.org/10.1093/mnras/stag678\">https://doi.org/10.1093/mnras/stag678</a>.","ista":"Perley DA, Ho AYQ, McGrath Z, Camilo M, Sevilla C, Chen P, Schroeder G, Govreen-Segal T, Bochenek A, Qin Y-J, Gillanders JH, Amend B, Anderson JP, Andreoni I, Aryan A, Bellm EC, Bloom JS, de Boer T, Carney J, Caiazzo I, Chambers KC, Charalampopoulos P, Chen T-W, Chen TX, Coughlin ER, Coughlin M, Dennefeld M, Dimitriadis G, Fremling C, Frostig D, Gal-Yam A, Galbany L, Gangopadhyay A, Ghendrih M, Graham MJ, Gromadzki M, Groom SL, Gutiérrez CP, Hinds K-R, Huber ME, Inserra C, Kaiser BC, Kasliwal MM, Koivisto NE, Lin C-C, Liu C, Lowe TB, Magnier E, Mahabal AA, Milligan A, Minguez P, Mo G, Müller-Bravo TE, Nicholl M, Pessi PJ, Pignata G, Purdum J, Rehemtulla N, Rich RM, Sahu A, Singh A, Smartt SJ, Smith IA, Sollerman J, Srinivasaragavan G, Srivastav S, Stein RD, Schulze S, Tweddle JW, Wainscoat R, Wise JL, Yan L, Young DR. 2026. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. 549(1), stag678.","ieee":"D. A. Perley <i>et al.</i>, “AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 549, no. 1. Oxford University Press, 2026.","ama":"Perley DA, Ho AYQ, McGrath Z, et al. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. <i>Monthly Notices of the Royal Astronomical Society</i>. 2026;549(1). doi:<a href=\"https://doi.org/10.1093/mnras/stag678\">10.1093/mnras/stag678</a>","mla":"Perley, Daniel A., et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 549, no. 1, stag678, Oxford University Press, 2026, doi:<a href=\"https://doi.org/10.1093/mnras/stag678\">10.1093/mnras/stag678</a>.","apa":"Perley, D. A., Ho, A. Y. Q., McGrath, Z., Camilo, M., Sevilla, C., Chen, P., … Young, D. R. (2026). AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stag678\">https://doi.org/10.1093/mnras/stag678</a>"},"arxiv":1,"OA_place":"publisher","issue":"1","language":[{"iso":"eng"}],"date_created":"2026-07-13T10:50:10Z","keyword":["stars: black holes","supernovae: individual: AT2024wpp","radio continuum: transients"],"scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole","article_processing_charge":"Yes","file_date_updated":"2026-07-13T14:35:34Z","department":[{"_id":"IlCa"}],"acknowledgement":"We thank Eliot Quataert, Luc Dessart, Ben Margalit, Ross Ferguson, Aaron Tohuvavohu, Brad Cenko, and Jamie Kennea for useful discussions. We thank the referee for helpful suggestions that improved the manuscript.\r\n\r\nBased on observations obtained with the Samuel Oschin Telescope 48-in. and the 60-in. Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant no. AST-2034437 and a collaboration including Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThe Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.\r\n\r\nBased on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The NOT data were obtained under program ID 68–501.\r\n\r\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We are grateful to Phil Evans, Aaron Tohuvavohu, and Jamie Kennea for advice on the Swift/XRT data reduction.\r\n\r\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. 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 indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\r\n\r\nSome observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.\r\n\r\nThe National Radio Astronomy Observatory and Green Bank Observatory are facilities of the U.S. National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA no. 2023.1.01730.T ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSTC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 2114.D-5014(E). We thank John Pritchard and Paula Sanchez Saez, and the entire observatory staff, for their excellent support.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey – PI: Inserra). ePESSTO+ observations were obtained under ESO program ID 112.25JQ.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with programs 16714, 17477, and 17889.\r\n\r\nBased on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).\r\n\r\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.\r\n\r\nThis research made use of ccdproc, an astropy package for image reduction (M. Craig et al. 2025).\r\n\r\nGS and AYQH acknowledge support in part from a Sloan Research Fellowship (award no. FG-2024-21320) from the Alfred P. Sloan Foundation. CS and AYQH acknowledge support in part from National Aeronautics and Space Administration (NASA) grant 80NSSC24K0377, from HST grant HST-GO-17477.006-A, and from a Scialog award from the Research Corporation for Science Advancement (‘Early Science with the LSST’).\r\n\r\nPC acknowledges support from the Zhejiang Provincial Top-Level Research Support Program.\r\n\r\nIA and JC are supported by the National Science Foundation award AST 2505775, NASA grant 24-ADAP24-0159, Scialog award SA-LSST-2024-102a, and the Discovery Alliance Catalyst Fellowship Mentors award 2025-62192-CM-19\r\n\r\nAA acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nT-WC acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nERC acknowledges support from the National Aeronautics and Space Administration through the Astrophysics Theory Program, grant 80NSSC24K0897.\r\n\r\nGD acknowledges support from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 101199369.\r\n\r\nDF’s contribution to this material is based upon work supported by the National Science Foundation under award no. AST-2401779.\r\n\r\nAGY’s research is supported by ISF, IMOS, and BSF grants, as well as the André Deloro Institute for Space and Optics Research, the Center for Experimental Physics, a WIS-MIT Sagol grant, the Norman E Alexander Family M Foundation ULTRASAT Data Center Fund, and Yeda-Sela; AGY is the incumbent of the The Arlyn Imberman Professorial Chair.\r\n\r\nLG acknowledges financial support from AGAUR, CSIC, MCIN, and AEI 10.13039/501100011033 under projects PID2023-151307NB-I00, PIE 20215AT016, and CEX2020-001058-M.\r\n\r\nMG acknowledges support from an STFC PhD studentship and from the Faculty of Science and Technology at Lancaster University.\r\n\r\nCPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant.\r\n\r\nCL is supported by DoE award no.  DE-SC0025599.\r\n\r\nZwicky Transient Facility, W. M. Keck Observatory, and MMT Observatory access was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA).\r\n\r\nAM gratefully acknowledges support from an STFC PhD studentship and the Faculty of Science and Technology at Lancaster University.\r\n\r\nTEMB is funded by Horizon Europe ERC grant no. 101125877.\r\n\r\nMN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381).\r\n\r\nNR is supported by a Northwestern University Presidential Fellowship Award. We gratefully acknowledge the support of the NSF-Simons AI-Institute for the Sky (SkAI) via grants NSF AST-2421845 and Simons Foundation MPS-AI-00010513.\r\n\r\nAS acknowledges the Warwick Astrophysics PhD prize scholarship made possible thanks to a generous philanthropic donation.\r\n\r\nSJS acknowledges funding from STFC grant ST/Y001605/1, a Royal Society Research Professorship and the Hintze Family Charitable Foundation.","external_id":{"arxiv":["2601.03337"]},"article_type":"original","dataavailabilitystatement":"All photometry is provided in the supplementary data files. Spectroscopy will be made available on WISEREP, and is available on request to the lead author.","tmp":{"image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)"},"_id":"22303","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","abstract":[{"lang":"eng","text":"We present the discovery of AT 2024wpp (‘Whippet’), a fast and luminous 18cow-like transient. At a redshift of z = 0 . 0868 , revealed by Keck Cosmic Web Imager spectroscopy of its faint star-forming host, it is the fourth-nearest example of its class to date. Rapid identification of the source in the Zwicky Transient Facility data stream permitted ultraviolet-through- optical observations to be obtained prior to peak, allowing the first determination of the peak bolometric luminosity ( 2 ×1045 erg s−1 ), maximum photospheric radius ( 1015 cm), and total radiated energy ( 1051 erg) of an 18cow-like object. We present results from a comprehensive multiwavelength observing campaign, including a far-ultraviolet spectrum from the Cosmic Origins Spectrograph on the Hubble Space Telescope and deep imaging extending > 100 d post-explosion from the Very Large Telescope, Hubble Space Telescope , Very Large Array, and Atacama Large Millimetre Array. We interpret the observations under a model in which a rapidly accreting central engine blows a fast ( ∼0.2 c ) wind into the surrounding medium and irradiates it with X-rays. The high Doppler velocities and intense ionization within this wind prevent identifiable spectroscopic features from appearing in the ejecta or in the surrounding circumstellar material. Weak H and He signatures do emerge in the spectra after 35 d in the form of double-peaked narrow lines. Each peak is individually narrow (full width δv ∼3000 km s−1 ) but the two components are separated by \u0003v ∼6600 km s−1 , indicating stable structures of denser material, possibly representing streams of tidal ejecta or an ablated companion star."}],"doi":"10.1093/mnras/stag678","DOAJ_listed":"1","volume":549,"oa":1,"file":[{"content_type":"application/pdf","file_id":"22314","success":1,"creator":"dernst","relation":"main_file","date_updated":"2026-07-13T14:35:34Z","checksum":"a5827b9f68f1731b8c8df18142c0ef38","file_name":"2026_MNRAS_Perley.pdf","file_size":6208809,"access_level":"open_access","date_created":"2026-07-13T14:35:34Z"}],"quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","has_accepted_license":"1","researchdata_availability":"upon request","day":"01","publisher":"Oxford University Press","oa_version":"Published Version","type":"journal_article","year":"2026","status":"public","OA_type":"gold","fulldoi":"https://doi.org/10.1093/mnras/stag678","article_number":"stag678","intvolume":"       549"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2110.11967"}],"day":"01","type":"journal_article","year":"2022","publisher":"Oxford University Press","oa_version":"Preprint","fulldoi":"https://doi.org/10.1093/mnras/stac801","status":"public","intvolume":"       512","publication_status":"published","_id":"11521","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"lang":"eng","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."}],"doi":"10.1093/mnras/stac801","volume":512,"quality_controlled":"1","oa":1,"date_created":"2022-07-07T09:21:30Z","language":[{"iso":"eng"}],"keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","article_processing_charge":"No","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.","external_id":{"arxiv":["2110.11967"]},"article_type":"original","date_published":"2022-06-01T00:00:00Z","month":"06","page":"5960-5977","date_updated":"2024-10-14T11:32:26Z","author":[{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"first_name":"Matthew","full_name":"Hayes, Matthew","last_name":"Hayes"},{"full_name":"Erb, Dawn","first_name":"Dawn","last_name":"Erb"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"first_name":"Ricardo","full_name":"Amorín, Ricardo","last_name":"Amorín"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"first_name":"Ana Paulino-Afonso","full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","last_name":"Ana Paulino-Afonso"},{"full_name":"Llerena, Mario","first_name":"Mario","last_name":"Llerena"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"}],"citation":{"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>","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>","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>.","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.","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."},"issue":"4","arxiv":1},{"month":"05","date_published":"2022-05-19T00:00:00Z","arxiv":1,"citation":{"apa":"Dhouib, H., Mathis, S., Bugnet, L. A., Van Reeth, T., &#38; Aerts, C. (2022). Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142956\">https://doi.org/10.1051/0004-6361/202142956</a>","mla":"Dhouib, H., et al. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 661, A133, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142956\">10.1051/0004-6361/202142956</a>.","ama":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. <i>Astronomy &#38; Astrophysics</i>. 2022;661. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142956\">10.1051/0004-6361/202142956</a>","ieee":"H. Dhouib, S. Mathis, L. A. Bugnet, T. Van Reeth, and C. Aerts, “Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field,” <i>Astronomy &#38; Astrophysics</i>, vol. 661. EDP Sciences, 2022.","ista":"Dhouib H, Mathis S, Bugnet LA, Van Reeth T, Aerts C. 2022. Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field. Astronomy &#38; Astrophysics. 661, A133.","chicago":"Dhouib, H., S. Mathis, Lisa Annabelle Bugnet, T. Van Reeth, and C. Aerts. “Detecting Deep Axisymmetric Toroidal Magnetic Fields in Stars: The Traditional Approximation of Rotation for Differentially Rotating Deep Spherical Shells with a General Azimuthal Magnetic Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142956\">https://doi.org/10.1051/0004-6361/202142956</a>.","short":"H. Dhouib, S. Mathis, L.A. Bugnet, T. Van Reeth, C. Aerts, Astronomy &#38; Astrophysics 661 (2022)."},"author":[{"last_name":"Dhouib","first_name":"H.","full_name":"Dhouib, H."},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet"},{"first_name":"T.","full_name":"Van Reeth, T.","last_name":"Van Reeth"},{"full_name":"Aerts, C.","first_name":"C.","last_name":"Aerts"}],"date_updated":"2022-08-22T07:58:54Z","title":"Detecting deep axisymmetric toroidal magnetic fields in stars: The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field","article_processing_charge":"No","scopus_import":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","magnetohydrodynamics (MHD) / waves / stars","rotation / stars: magnetic field / stars","oscillations / methods"],"language":[{"iso":"eng"}],"date_created":"2022-07-19T08:04:15Z","article_type":"original","external_id":{"arxiv":["2202.10026"]},"acknowledgement":"We thank the referee for her/his positive and constructive report, which has allowed us to improve the quality of our article. H.D. and S.M. acknowledge support from the CNES PLATO grant at CEA/DAp. T.V.R. gratefully acknowledges support from the Research Foundation Flanders (FWO) under grant agreement No. 12ZB620N and V414021N. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1748958. C.A. is supported by the KU Leuven Research Council (grant C16/18/005: PARADISE) as well as from the BELgian federal Science Policy Office (BELSPO) through a PLATO PRODEX grant.","abstract":[{"lang":"eng","text":"Context. Asteroseismology has revealed small core-to-surface rotation contrasts in stars in the whole Hertzsprung–Russell diagram. This is the signature of strong transport of angular momentum (AM) in stellar interiors. One of the plausible candidates to efficiently carry AM is magnetic fields with various topologies that could be present in stellar radiative zones. Among them, strong axisymmetric azimuthal (toroidal) magnetic fields have received a lot of interest. Indeed, if they are subject to the so-called Tayler instability, the accompanying triggered Maxwell stresses can transport AM efficiently. In addition, the electromotive force induced by the fluctuations of magnetic and velocity fields could potentially sustain a dynamo action that leads to the regeneration of the initial strong axisymmetric azimuthal magnetic field.\r\n\r\nAims. The key question we aim to answer is whether we can detect signatures of these deep strong azimuthal magnetic fields. The only way to answer this question is asteroseismology, and the best laboratories of study are intermediate-mass and massive stars with external radiative envelopes. Most of these are rapid rotators during their main sequence. Therefore, we have to study stellar pulsations propagating in stably stratified, rotating, and potentially strongly magnetised radiative zones, namely magneto-gravito-inertial (MGI) waves.\r\n\r\nMethods. We generalise the traditional approximation of rotation (TAR) by simultaneously taking general axisymmetric differential rotation and azimuthal magnetic fields into account. Both the Coriolis acceleration and the Lorentz force are therefore treated in a non-perturbative way. Using this new formalism, we derive the asymptotic properties of MGI waves and their period spacings.\r\n\r\nResults. We find that toroidal magnetic fields induce a shift in the period spacings of gravity (g) and Rossby (r) modes. An equatorial azimuthal magnetic field with an amplitude of the order of 105 G leads to signatures that are detectable in period spacings for high-radial-order g and r modes in γ Doradus (γ Dor) and slowly pulsating B (SPB) stars. More complex hemispheric configurations are more difficult to observe, particularly when they are localised out of the propagation region of MGI modes, which can be localised in an equatorial belt.\r\n\r\nConclusions. The magnetic TAR, which takes into account toroidal magnetic fields in a non-perturbative way, is derived. This new formalism allows us to assess the effects of the magnetic field in γ Dor and SPB stars on g and r modes. We find that these effects should be detectable for equatorial fields thanks to modern space photometry using observations from Kepler, TESS CVZ, and PLATO."}],"doi":"10.1051/0004-6361/202142956","_id":"11621","publication":"Astronomy & Astrophysics","publication_status":"published","oa":1,"quality_controlled":"1","volume":661,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       661","status":"public","fulldoi":"https://doi.org/10.1051/0004-6361/202142956","article_number":"A133","publisher":"EDP Sciences","oa_version":"Preprint","type":"journal_article","year":"2022","day":"19","main_file_link":[{"url":"https://arxiv.org/abs/2202.10026","open_access":"1"}]},{"language":[{"iso":"eng"}],"date_created":"2022-07-07T09:30:21Z","extern":"1","keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","article_processing_charge":"No","acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","external_id":{"arxiv":["2004.14496"]},"article_type":"original","date_published":"2021-12-01T00:00:00Z","page":"3697-3709","month":"12","date_updated":"2022-08-18T10:45:56Z","author":[{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"full_name":"Ocvirk, Pierre","first_name":"Pierre","last_name":"Ocvirk"},{"last_name":"Mason","first_name":"Charlotte","full_name":"Mason, Charlotte"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Bosman","full_name":"Bosman, Sarah E I","first_name":"Sarah E I"},{"last_name":"Sorce","full_name":"Sorce, Jenny G","first_name":"Jenny G"},{"full_name":"Lewis, Joseph","first_name":"Joseph","last_name":"Lewis"},{"last_name":"Ahn","full_name":"Ahn, Kyungjin","first_name":"Kyungjin"},{"last_name":"Aubert","full_name":"Aubert, Dominique","first_name":"Dominique"},{"full_name":"Dawoodbhoy, Taha","first_name":"Taha","last_name":"Dawoodbhoy"},{"last_name":"Iliev","first_name":"Ilian T","full_name":"Iliev, Ilian T"},{"last_name":"Shapiro","full_name":"Shapiro, Paul R","first_name":"Paul R"},{"last_name":"Yepes","first_name":"Gustavo","full_name":"Yepes, Gustavo"}],"citation":{"apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>.","ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;508(3):3697-3709. doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>","ieee":"M. Gronke <i>et al.</i>, “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>.","ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709.","short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709."},"arxiv":1,"issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2004.14496","open_access":"1"}],"day":"01","publisher":"Oxford University Press","oa_version":"Preprint","type":"journal_article","year":"2021","status":"public","fulldoi":"https://doi.org/10.1093/mnras/stab2762","intvolume":"       508","_id":"11522","publication":"Monthly Notices of the Royal Astronomical Society","publication_status":"published","abstract":[{"text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations.","lang":"eng"}],"doi":"10.1093/mnras/stab2762","volume":508,"oa":1,"quality_controlled":"1"},{"article_type":"original","external_id":{"arxiv":["2102.07779"]},"acknowledgement":"We thank the referee for constructive comments and suggestions. We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for useful discussions and suggestions. It is a pleasure to thank the ESO User Support, in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and Lowell Tacconi-Garman for assistance in the preparation and execution of the observations. Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413, 091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779, and 102.A-0652. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY, MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of A. C. J.Matthee (1953–2020).","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","article_processing_charge":"No","date_created":"2022-07-07T09:33:39Z","language":[{"iso":"eng"}],"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"citation":{"short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","ieee":"J. J. Matthee <i>et al.</i>, “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.","ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412.","chicago":"Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>.","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>.","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1382-1412. doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>","apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>"},"issue":"1","arxiv":1,"date_updated":"2024-10-14T11:32:39Z","author":[{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Matthew","full_name":"Hayes, Matthew","last_name":"Hayes"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"full_name":"Naidu, Rohan P","first_name":"Rohan P","last_name":"Naidu"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Calhau","first_name":"João","full_name":"Calhau, João"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"first_name":"Sérgio","full_name":"Santos, Sérgio","last_name":"Santos"},{"first_name":"Ricardo","full_name":"Amorín, Ricardo","last_name":"Amorín"}],"month":"07","page":"1382-1412","date_published":"2021-07-01T00:00:00Z","fulldoi":"https://doi.org/10.1093/mnras/stab1304","status":"public","intvolume":"       505","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.07779"}],"year":"2021","type":"journal_article","oa_version":"Preprint","publisher":"Oxford University Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":505,"quality_controlled":"1","oa":1,"publication_status":"published","_id":"11523","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙.","lang":"eng"}],"doi":"10.1093/mnras/stab1304"},{"citation":{"apa":"Bugnet, L. A., Prat, V., Mathis, S., Astoul, A., Augustson, K., García, R. A., … Neiner, C. (2021). Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>","mla":"Bugnet, Lisa Annabelle, et al. “Magnetic Signatures on Mixed-Mode Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 650, A53, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>.","ama":"Bugnet LA, Prat V, Mathis S, et al. Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. 2021;650. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>","ieee":"L. A. Bugnet <i>et al.</i>, “Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 650. EDP Sciences, 2021.","chicago":"Bugnet, Lisa Annabelle, V. Prat, S. Mathis, A. Astoul, K. Augustson, R. A. García, S. Mathur, L. Amard, and C. Neiner. “Magnetic Signatures on Mixed-Mode Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>.","ista":"Bugnet LA, Prat V, Mathis S, Astoul A, Augustson K, García RA, Mathur S, Amard L, Neiner C. 2021. Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. Astronomy &#38; Astrophysics. 650, A53.","short":"L.A. Bugnet, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.A. García, S. Mathur, L. Amard, C. Neiner, Astronomy &#38; Astrophysics 650 (2021)."},"arxiv":1,"date_updated":"2024-10-14T11:39:01Z","author":[{"orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"},{"full_name":"Prat, V.","first_name":"V.","last_name":"Prat"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"first_name":"A.","full_name":"Astoul, A.","last_name":"Astoul"},{"last_name":"Augustson","first_name":"K.","full_name":"Augustson, K."},{"last_name":"García","full_name":"García, R. A.","first_name":"R. A."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"first_name":"L.","full_name":"Amard, L.","last_name":"Amard"},{"last_name":"Neiner","first_name":"C.","full_name":"Neiner, C."}],"month":"06","date_published":"2021-06-07T00:00:00Z","article_type":"original","external_id":{"arxiv":["2102.01216"]},"scopus_import":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_processing_charge":"No","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","language":[{"iso":"eng"}],"date_created":"2022-07-18T12:10:59Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"extern":"1","volume":650,"oa":1,"quality_controlled":"1","_id":"11605","publication_status":"published","publication":"Astronomy & Astrophysics","doi":"10.1051/0004-6361/202039159","abstract":[{"text":"Context. The discovery of moderate differential rotation between the core and the envelope of evolved solar-like stars could be the signature of a strong magnetic field trapped inside the radiative interior. The population of intermediate-mass red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation modes that behave as acoustic modes in their external envelope and as gravity modes in their core) could also arise from the effect of an internal magnetic field. Indeed, stars more massive than about 1.1 solar masses are known to develop a convective core during their main sequence. The field generated by the dynamo triggered by this convection could be the progenitor of a strong fossil magnetic field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims. Observations of mixed modes can constitute an excellent probe of the deepest layers of evolved solar-like stars, and magnetic fields in those regions can impact their propagation. The magnetic perturbation on mixed modes may therefore be visible in asteroseismic data. To unravel which constraints can be obtained from observations, we theoretically investigate the effects of a plausible mixed axisymmetric magnetic field with various amplitudes on the mixed-mode frequencies of evolved solar-like stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric magnetic field were computed for dipolar and quadrupolar mixed modes. These computations were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions. We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the presence of a dynamo in the convective core during the main sequence, provoke significant asymmetries on mixed-mode frequency multiplets during the red giant branch. We provide constraints and methods for the detectability of such magnetic signatures. We show that these signatures may be detectable in asteroseismic data for field amplitudes small enough for the amplitude of the modes not to be affected by the conversion of gravity into Alfvén waves inside the magnetised interior. Finally, we infer an upper limit for the strength of the field and the associated lower limit for the timescale of its action in order to redistribute angular momentum in stellar interiors.","lang":"eng"}],"status":"public","article_number":"A53","fulldoi":"https://doi.org/10.1051/0004-6361/202039159","intvolume":"       650","main_file_link":[{"url":"https://arxiv.org/abs/2102.01216","open_access":"1"}],"day":"07","oa_version":"Preprint","publisher":"EDP Sciences","year":"2021","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"volume":647,"oa":1,"quality_controlled":"1","publication_status":"published","_id":"11606","publication":"Astronomy & Astrophysics","abstract":[{"text":"Context. Our knowledge of the dynamics of stars has undergone a revolution through the simultaneous large amount of high-quality photometric observations collected by space-based asteroseismology and ground-based high-precision spectropolarimetry. They allowed us to probe the internal rotation of stars and their surface magnetism in the whole Hertzsprung-Russell diagram. However, new methods should still be developed to probe the deep magnetic fields in these stars.\r\n\r\nAims. Our goal is to provide seismic diagnoses that allow us to probe the internal magnetism of stars.\r\n\r\nMethods. We focused on asymptotic low-frequency gravity modes and high-frequency acoustic modes. Using a first-order perturbative theory, we derived magnetic splittings of their frequencies as explicit functions of stellar parameters.\r\n\r\nResults. As in the case of rotation, we show that asymptotic gravity and acoustic modes can allow us to probe the different components of the magnetic field in the cavities in which they propagate. This again demonstrates the high potential of using mixed-modes when this is possible.","lang":"eng"}],"doi":"10.1051/0004-6361/202039180","status":"public","article_number":"A122","fulldoi":"https://doi.org/10.1051/0004-6361/202039180","intvolume":"       647","main_file_link":[{"url":"https://arxiv.org/abs/2012.11050","open_access":"1"}],"day":"18","oa_version":"Preprint","publisher":"EDP Sciences","year":"2021","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"S. Mathis, L.A. Bugnet, V. Prat, K. Augustson, S. Mathur, R.A. Garcia, Astronomy &#38; Astrophysics 647 (2021).","ieee":"S. Mathis, L. A. Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia, “Probing the internal magnetism of stars using asymptotic magneto-asteroseismology,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","ista":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. 2021. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. Astronomy &#38; Astrophysics. 647, A122.","chicago":"Mathis, S., Lisa Annabelle Bugnet, V. Prat, K. Augustson, S. Mathur, and R. A. Garcia. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>.","ama":"Mathis S, Bugnet LA, Prat V, Augustson K, Mathur S, Garcia RA. Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>","mla":"Mathis, S., et al. “Probing the Internal Magnetism of Stars Using Asymptotic Magneto-Asteroseismology.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A122, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039180\">10.1051/0004-6361/202039180</a>.","apa":"Mathis, S., Bugnet, L. A., Prat, V., Augustson, K., Mathur, S., &#38; Garcia, R. A. (2021). Probing the internal magnetism of stars using asymptotic magneto-asteroseismology. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039180\">https://doi.org/10.1051/0004-6361/202039180</a>"},"arxiv":1,"date_updated":"2024-10-14T11:39:21Z","author":[{"first_name":"S.","full_name":"Mathis, S.","last_name":"Mathis"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet"},{"full_name":"Prat, V.","first_name":"V.","last_name":"Prat"},{"full_name":"Augustson, K.","first_name":"K.","last_name":"Augustson"},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"first_name":"R. A.","full_name":"Garcia, R. A.","last_name":"Garcia"}],"month":"03","date_published":"2021-03-18T00:00:00Z","article_type":"original","external_id":{"arxiv":["2012.11050"]},"acknowledgement":"The authors thank the referee and Pr. J. Christensen-Dalsgaard for their very constructive comments and remarks that allowed us to improve the article. St. M., L. B., V. P., and K. A. acknowledge support from the European Research Council through ERC grant SPIRE 647383. All the members from CEA acknowledge support from GOLF and PLATO CNES grants of the Astrophysics Division at CEA. S. Mathur acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. We made great use of the megyr python package for interfacing MESA and GYRE codes.","scopus_import":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"title":"Probing the internal magnetism of stars using asymptotic magneto-asteroseismology","article_processing_charge":"No","language":[{"iso":"eng"}],"date_created":"2022-07-18T12:15:27Z","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / waves / stars","magnetic field / stars","oscillations / methods","analytical"]},{"quality_controlled":"1","oa":1,"volume":647,"abstract":[{"text":"In order to understand stellar evolution, it is crucial to efficiently determine stellar surface rotation periods. Indeed, while they are of great importance in stellar models, angular momentum transport processes inside stars are still poorly understood today. Surface rotation, which is linked to the age of the star, is one of the constraints needed to improve the way those processes are modelled. Statistics of the surface rotation periods for a large sample of stars of different spectral types are thus necessary. An efficient tool to automatically determine reliable rotation periods is needed when dealing with large samples of stellar photometric datasets. The objective of this work is to develop such a tool. For this purpose, machine learning classifiers constitute relevant bases to build our new methodology. Random forest learning abilities are exploited to automate the extraction of rotation periods in Kepler light curves. Rotation periods and complementary parameters are obtained via three different methods: a wavelet analysis, the autocorrelation function of the light curve, and the composite spectrum. We trained three different classifiers: one to detect if rotational modulations are present in the light curve, one to flag close binary or classical pulsators candidates that can bias our rotation period determination, and finally one classifier to provide the final rotation period. We tested our machine learning pipeline on 23 431 stars of the Kepler K and M dwarf reference rotation catalogue for which 60% of the stars have been visually inspected. For the sample of 21 707 stars where all the input parameters are provided to the algorithm, 94.2% of them are correctly classified (as rotating or not). Among the stars that have a rotation period in the reference catalogue, the machine learning provides a period that agrees within 10% of the reference value for 95.3% of the stars. Moreover, the yield of correct rotation periods is raised to 99.5% after visually inspecting 25.2% of the stars. Over the two main analysis steps, rotation classification and period selection, the pipeline yields a global agreement with the reference values of 92.1% and 96.9% before and after visual inspection. Random forest classifiers are efficient tools to determine reliable rotation periods in large samples of stars. The methodology presented here could be easily adapted to extract surface rotation periods for stars with different spectral types or observed by other instruments such as K2, TESS or by PLATO in the near future.","lang":"eng"}],"doi":"10.1051/0004-6361/202039947","_id":"11608","publication_status":"published","publication":"Astronomy & Astrophysics","year":"2021","type":"journal_article","oa_version":"Preprint","publisher":"EDP Sciences","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2101.10152"}],"day":"19","intvolume":"       647","article_number":"A125","fulldoi":"https://doi.org/10.1051/0004-6361/202039947","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"S. N.","full_name":"Breton, S. N.","last_name":"Breton"},{"first_name":"A. R. G.","full_name":"Santos, A. R. G.","last_name":"Santos"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet"},{"last_name":"Mathur","full_name":"Mathur, S.","first_name":"S."},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"last_name":"Pallé","first_name":"P. L.","full_name":"Pallé, P. L."}],"date_updated":"2022-08-22T08:47:47Z","arxiv":1,"citation":{"ieee":"S. N. Breton, A. R. G. Santos, L. A. Bugnet, S. Mathur, R. A. García, and P. L. Pallé, “ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","chicago":"Breton, S. N., A. R. G. Santos, Lisa Annabelle Bugnet, S. Mathur, R. A. García, and P. L. Pallé. “ROOSTER: A Machine-Learning Analysis Tool for Kepler Stellar Rotation Periods.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039947\">https://doi.org/10.1051/0004-6361/202039947</a>.","ista":"Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. 2021. ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. Astronomy &#38; Astrophysics. 647, A125.","short":"S.N. Breton, A.R.G. Santos, L.A. Bugnet, S. Mathur, R.A. García, P.L. Pallé, Astronomy &#38; Astrophysics 647 (2021).","apa":"Breton, S. N., Santos, A. R. G., Bugnet, L. A., Mathur, S., García, R. A., &#38; Pallé, P. L. (2021). ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039947\">https://doi.org/10.1051/0004-6361/202039947</a>","mla":"Breton, S. N., et al. “ROOSTER: A Machine-Learning Analysis Tool for Kepler Stellar Rotation Periods.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A125, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039947\">10.1051/0004-6361/202039947</a>.","ama":"Breton SN, Santos ARG, Bugnet LA, Mathur S, García RA, Pallé PL. ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039947\">10.1051/0004-6361/202039947</a>"},"date_published":"2021-03-19T00:00:00Z","month":"03","acknowledgement":"We thank Suzanne Aigrain and Joe Llama for providing us with the simulated data used in Aigrain et al. (2015). S. N. B., L. B. and R. A. G. acknowledge the support from PLATO and GOLF CNES grants. A. R. G. S. acknowledges the support from NASA under grant NNX17AF27G. S. M. acknowledges the support from the Spanish Ministry of Science and Innovation with the Ramon y Cajal fellowship number RYC-2015-17697. P. L. P. and S. M. acknowledge support from the Spanish Ministry of Science and Innovation with the grant number PID2019-107187GB-I00. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Software: Python (Van Rossum & Drake 2009), numpy (Oliphant 2006), pandas (The pandas development team 2020; McKinney 2010), matplotlib (Hunter 2007), scikit-learn (Pedregosa et al. 2011). The source code used to obtain the present results can be found at: https://gitlab.com/sybreton/pushkin ; https://gitlab.com/sybreton/ml_surface_rotation_paper .","external_id":{"arxiv":["2101.10152"]},"article_type":"original","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis / stars: solar-type / stars: activity / stars: rotation / starspots"],"extern":"1","date_created":"2022-07-18T12:21:32Z","language":[{"iso":"eng"}],"article_processing_charge":"No","title":"ROOSTER: A machine-learning analysis tool for Kepler stellar rotation periods","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1"},{"article_type":"original","external_id":{"arxiv":["2006.10660"]},"acknowledgement":"The authors acknowledge support from the European Research Council through ERC grant SPIRE 647383 and from GOLF and PLATO CNES grants at the Department of Astrophysics at CEA Paris-Saclay. We thank the referee, Prof. A. J. Barker, for his constructive comments that allow us to improve the article.","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","title":"Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration","article_processing_charge":"No","date_created":"2022-07-18T13:24:32Z","language":[{"iso":"eng"}],"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","hydrodynamics / turbulence / stars","rotation / stars","evolution"],"citation":{"short":"J. Park, V. Prat, S. Mathis, L.A. Bugnet, Astronomy &#38; Astrophysics 646 (2021).","ista":"Park J, Prat V, Mathis S, Bugnet LA. 2021. Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration. Astronomy &#38; Astrophysics. 646, A64.","chicago":"Park, J., V. Prat, S. Mathis, and Lisa Annabelle Bugnet. “Horizontal Shear Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis Acceleration.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202038654\">https://doi.org/10.1051/0004-6361/202038654</a>.","ieee":"J. Park, V. Prat, S. Mathis, and L. A. Bugnet, “Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration,” <i>Astronomy &#38; Astrophysics</i>, vol. 646. EDP Sciences, 2021.","ama":"Park J, Prat V, Mathis S, Bugnet LA. Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration. <i>Astronomy &#38; Astrophysics</i>. 2021;646. doi:<a href=\"https://doi.org/10.1051/0004-6361/202038654\">10.1051/0004-6361/202038654</a>","mla":"Park, J., et al. “Horizontal Shear Instabilities in Rotating Stellar Radiation Zones: II. Effects of the Full Coriolis Acceleration.” <i>Astronomy &#38; Astrophysics</i>, vol. 646, A64, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202038654\">10.1051/0004-6361/202038654</a>.","apa":"Park, J., Prat, V., Mathis, S., &#38; Bugnet, L. A. (2021). Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202038654\">https://doi.org/10.1051/0004-6361/202038654</a>"},"arxiv":1,"date_updated":"2022-08-19T10:18:03Z","author":[{"last_name":"Park","first_name":"J.","full_name":"Park, J."},{"first_name":"V.","full_name":"Prat, V.","last_name":"Prat"},{"last_name":"Mathis","full_name":"Mathis, S.","first_name":"S."},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","last_name":"Bugnet"}],"month":"02","date_published":"2021-02-08T00:00:00Z","fulldoi":"https://doi.org/10.1051/0004-6361/202038654","article_number":"A64","status":"public","intvolume":"       646","main_file_link":[{"url":"https://arxiv.org/abs/2006.10660","open_access":"1"}],"day":"08","year":"2021","type":"journal_article","oa_version":"Preprint","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":646,"quality_controlled":"1","oa":1,"publication":"Astronomy & Astrophysics","_id":"11609","publication_status":"published","abstract":[{"text":"Context. Stellar interiors are the seat of efficient transport of angular momentum all along their evolution. In this context, understanding the dependence of the turbulent transport triggered by the instabilities of the vertical and horizontal shears of the differential rotation in stellar radiation zones as a function of their rotation, stratification, and thermal diffusivity is mandatory. Indeed, it constitutes one of the cornerstones of the rotational transport and mixing theory, which is implemented in stellar evolution codes to predict the rotational and chemical evolutions of stars.\r\n\r\nAims. We investigate horizontal shear instabilities in rotating stellar radiation zones by considering the full Coriolis acceleration with both the dimensionless horizontal Coriolis component f̃ and the vertical component f.\r\n\r\nMethods. We performed a linear stability analysis using linearized equations derived from the Navier-Stokes and heat transport equations in the rotating nontraditional f-plane. We considered a horizontal shear flow with a hyperbolic tangent profile as the base flow. The linear stability was analyzed numerically in wide ranges of parameters, and we performed an asymptotic analysis for large vertical wavenumbers using the Wentzel-Kramers-Brillouin-Jeffreys (WKBJ) approximation for nondiffusive and highly-diffusive fluids.\r\n\r\nResults. As in the traditional f-plane approximation, we identify two types of instabilities: the inflectional and inertial instabilities. The inflectional instability is destabilized as f̃ increases and its maximum growth rate increases significantly, while the thermal diffusivity stabilizes the inflectional instability similarly to the traditional case. The inertial instability is also strongly affected; for instance, the inertially unstable regime is also extended in the nondiffusive limit as 0 < f < 1 + f̃ 2/N2, where N is the dimensionless Brunt-Väisälä frequency. More strikingly, in the high thermal diffusivity limit, it is always inertially unstable at any colatitude θ except at the poles (i.e., 0° < θ <  180°). We also derived the critical Reynolds numbers for the inertial instability using the asymptotic dispersion relations obtained from the WKBJ analysis. Using the asymptotic and numerical results, we propose a prescription for the effective turbulent viscosities induced by the inertial and inflectional instabilities that can be possibly used in stellar evolution models. The characteristic time of this turbulence is short enough so that it is efficient to redistribute angular momentum and to mix chemicals in stellar radiation zones.","lang":"eng"}],"doi":"10.1051/0004-6361/202038654"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","year":"2020","oa_version":"Published Version","publisher":"EDP Sciences","day":"03","main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"intvolume":"       638","fulldoi":"https://doi.org/10.1051/0004-6361/201937340","article_number":"A12","status":"public","doi":"10.1051/0004-6361/201937340","abstract":[{"lang":"eng","text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time."}],"_id":"11503","publication_status":"published","publication":"Astronomy & Astrophysics","quality_controlled":"1","oa":1,"volume":638,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"extern":"1","date_created":"2022-07-06T09:50:48Z","language":[{"iso":"eng"}],"article_processing_charge":"No","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","external_id":{"arxiv":["2003.12083"]},"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima, Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy (http://www.astropy.org), which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE. This work was supported by the project FOGHAR (Agence Nationale de la Recherche, ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid for Scientic Research 19J01620.","article_type":"original","date_published":"2020-06-03T00:00:00Z","month":"06","author":[{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"first_name":"Jérémy","full_name":"Blaizot, Jérémy","last_name":"Blaizot"},{"last_name":"Garel","full_name":"Garel, Thibault","first_name":"Thibault"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"last_name":"Hashimoto","first_name":"Takuya","full_name":"Hashimoto, Takuya"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"last_name":"Conseil","first_name":"Simon","full_name":"Conseil, Simon"},{"last_name":"Guiderdoni","full_name":"Guiderdoni, Bruno","first_name":"Bruno"},{"last_name":"Drake","first_name":"Alyssa B.","full_name":"Drake, Alyssa B."},{"first_name":"Edmund","full_name":"Christian Herenz, Edmund","last_name":"Christian Herenz"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Anna Marino","first_name":"Raffaella","full_name":"Anna Marino, Raffaella"},{"first_name":"Kasper","full_name":"Borello Schmidt, Kasper","last_name":"Borello Schmidt"},{"last_name":"Pelló","full_name":"Pelló, Roser","first_name":"Roser"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"last_name":"Kerutt","first_name":"Josephine","full_name":"Kerutt, Josephine"},{"first_name":"Guillaume","full_name":"Mahler, Guillaume","last_name":"Mahler"}],"date_updated":"2022-07-19T09:35:20Z","arxiv":1,"citation":{"short":"H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T. Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz, J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló, M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy &#38; Astrophysics 638 (2020).","ieee":"H. Kusakabe <i>et al.</i>, “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” <i>Astronomy &#38; Astrophysics</i>, vol. 638. EDP Sciences, 2020.","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy &#38; Astrophysics. 638, A12.","chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>.","mla":"Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” <i>Astronomy &#38; Astrophysics</i>, vol. 638, A12, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>.","ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. <i>Astronomy &#38; Astrophysics</i>. 2020;638. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937340\">10.1051/0004-6361/201937340</a>","apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937340\">https://doi.org/10.1051/0004-6361/201937340</a>"}},{"date_updated":"2024-10-14T11:33:21Z","author":[{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"},{"last_name":"Lilly","full_name":"Lilly, Simon","first_name":"Simon"},{"last_name":"Boogaard","first_name":"Leindert","full_name":"Boogaard, Leindert"},{"first_name":"Raffaella","full_name":"Marino, Raffaella","last_name":"Marino"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"}],"citation":{"short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","ieee":"J. J. Matthee <i>et al.</i>, “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020.","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059.","chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa2550\">https://doi.org/10.1093/mnras/staa2550</a>.","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:<a href=\"https://doi.org/10.1093/mnras/staa2550\">10.1093/mnras/staa2550</a>.","ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;498(2):3043-3059. doi:<a href=\"https://doi.org/10.1093/mnras/staa2550\">10.1093/mnras/staa2550</a>","apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa2550\">https://doi.org/10.1093/mnras/staa2550</a>"},"issue":"2","arxiv":1,"date_published":"2020-10-01T00:00:00Z","month":"10","page":"3043-3059","external_id":{"arxiv":["2008.01731"]},"article_type":"original","date_created":"2022-07-07T10:36:01Z","language":[{"iso":"eng"}],"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","article_processing_charge":"No","volume":498,"quality_controlled":"1","oa":1,"publication":"Monthly Notices of the Royal Astronomical Society","_id":"11529","publication_status":"published","doi":"10.1093/mnras/staa2550","abstract":[{"lang":"eng","text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst."}],"day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}],"type":"journal_article","year":"2020","oa_version":"Preprint","publisher":"Oxford University Press","fulldoi":"https://doi.org/10.1093/mnras/staa2550","status":"public","intvolume":"       498","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"Behnam","full_name":"Darvish, Behnam","last_name":"Darvish"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"}],"date_updated":"2024-10-14T11:33:34Z","arxiv":1,"issue":"2","citation":{"apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;492(2):1778-1790. doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>","mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","ieee":"J. J. Matthee <i>et al.</i>, “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790."},"date_published":"2020-02-01T00:00:00Z","page":"1778-1790","month":"02","external_id":{"arxiv":["1909.06376"]},"acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","article_type":"original","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"extern":"1","language":[{"iso":"eng"}],"date_created":"2022-07-07T12:21:36Z","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","article_processing_charge":"No","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"quality_controlled":"1","volume":492,"doi":"10.1093/mnras/stz3554","abstract":[{"lang":"eng","text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies."}],"publication":"Monthly Notices of the Royal Astronomical Society","_id":"11534","publication_status":"published","publisher":"Oxford University Press","oa_version":"Preprint","type":"journal_article","year":"2020","main_file_link":[{"url":"https://arxiv.org/abs/1909.06376","open_access":"1"}],"day":"01","intvolume":"       492","status":"public","fulldoi":"https://doi.org/10.1093/mnras/stz3554","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"month":"02","date_published":"2020-02-05T00:00:00Z","citation":{"short":"J. Bodensteiner, H. Sana, L. Mahy, L.R. Patrick, A. de Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, N. Langer, D.J. Lennon, F.R.N. Schneider, F. Tramper, Astronomy &#38; Astrophysics 634 (2020).","ista":"Bodensteiner J, Sana H, Mahy L, Patrick LR, de Koter A, de Mink SE, Evans CJ, Götberg YLL, Langer N, Lennon DJ, Schneider FRN, Tramper F. 2020. The young massive SMC cluster NGC 330 seen by MUSE. Astronomy &#38; Astrophysics. 634, A51.","chicago":"Bodensteiner, J., H. Sana, L. Mahy, L. R. Patrick, A. de Koter, S. E. de Mink, C. J. Evans, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201936743\">https://doi.org/10.1051/0004-6361/201936743</a>.","ieee":"J. Bodensteiner <i>et al.</i>, “The young massive SMC cluster NGC 330 seen by MUSE,” <i>Astronomy &#38; Astrophysics</i>, vol. 634. EDP Sciences, 2020.","ama":"Bodensteiner J, Sana H, Mahy L, et al. The young massive SMC cluster NGC 330 seen by MUSE. <i>Astronomy &#38; Astrophysics</i>. 2020;634. doi:<a href=\"https://doi.org/10.1051/0004-6361/201936743\">10.1051/0004-6361/201936743</a>","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE.” <i>Astronomy &#38; Astrophysics</i>, vol. 634, A51, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201936743\">10.1051/0004-6361/201936743</a>.","apa":"Bodensteiner, J., Sana, H., Mahy, L., Patrick, L. R., de Koter, A., de Mink, S. E., … Tramper, F. (2020). The young massive SMC cluster NGC 330 seen by MUSE. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201936743\">https://doi.org/10.1051/0004-6361/201936743</a>"},"arxiv":1,"date_updated":"2023-08-09T12:50:01Z","author":[{"full_name":"Bodensteiner, J.","first_name":"J.","last_name":"Bodensteiner"},{"last_name":"Sana","first_name":"H.","full_name":"Sana, H."},{"last_name":"Mahy","first_name":"L.","full_name":"Mahy, L."},{"full_name":"Patrick, L. R.","first_name":"L. R.","last_name":"Patrick"},{"first_name":"A.","full_name":"de Koter, A.","last_name":"de Koter"},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"first_name":"C. J.","full_name":"Evans, C. J.","last_name":"Evans"},{"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":"N.","full_name":"Langer, N.","last_name":"Langer"},{"last_name":"Lennon","first_name":"D. J.","full_name":"Lennon, D. J."},{"last_name":"Schneider","full_name":"Schneider, F. R. N.","first_name":"F. R. N."},{"last_name":"Tramper","full_name":"Tramper, F.","first_name":"F."}],"scopus_import":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"title":"The young massive SMC cluster NGC 330 seen by MUSE","article_processing_charge":"No","language":[{"iso":"eng"}],"date_created":"2023-08-03T10:13:29Z","keyword":["stars: massive / stars: emission-line / Be / binaries: spectroscopic / blue stragglers / Magellanic Clouds"],"extern":"1","article_type":"original","external_id":{"arxiv":["1911.03477"]},"publication":"Astronomy & Astrophysics","_id":"13466","publication_status":"published","abstract":[{"lang":"eng","text":"Context. A majority of massive stars are part of binary systems, a large fraction of which will inevitably interact during their lives. Binary-interaction products (BiPs), that is, stars affected by such interaction, are expected to be commonly present in stellar populations. BiPs are thus a crucial ingredient in the understanding of stellar evolution.\r\nAims. We aim to identify and characterize a statistically significant sample of BiPs by studying clusters of 10 − 40 Myr, an age at which binary population models predict the abundance of BiPs to be highest. One example of such a cluster is NGC 330 in the Small Magellanic Cloud.\r\nMethods. Using MUSE WFM-AO observations of NGC 330, we resolved the dense cluster core for the first time and were able to extract spectra of its entire massive star population. We developed an automated spectral classification scheme based on the equivalent widths of spectral lines in the red part of the spectrum.\r\nResults. We characterize the massive star content of the core of NGC 330, which contains more than 200 B stars, 2 O stars, 6 A-type supergiants, and 11 red supergiants. We find a lower limit on the Be star fraction of 32 ± 3% in the whole sample. It increases to at least 46 ± 10% when we only consider stars brighter than V = 17 mag. We estimate an age of the cluster core between 35 and 40 Myr and a total cluster mass of 88−18+17 × 103 M⊙.\r\nConclusions. We find that the population in the cluster core is different than the population in the outskirts: while the stellar content in the core appears to be older than the stars in the outskirts, the Be star fraction and the observed binary fraction are significantly higher. Furthermore, we detect several BiP candidates that will be subject of future studies."}],"doi":"10.1051/0004-6361/201936743","volume":634,"oa":1,"quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","fulldoi":"https://doi.org/10.1051/0004-6361/201936743","article_number":"A51","intvolume":"       634","day":"05","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201936743","open_access":"1"}],"oa_version":"Published Version","publisher":"EDP Sciences","year":"2020","type":"journal_article"},{"article_type":"original","external_id":{"arxiv":["1905.13696"]},"acknowledgement":"We thank the anonymous referee for their critical review and useful suggestions. This work has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the “Investissements d’Avenir” French government programme managed by the ANR. Partially funded by the ERC starting grant CALENDS (JR, VP, BC, JM), the Agence Nationale de la recherche bearing the reference ANR-13-BS05-0010-02 (FOGHAR), and the “Programme National de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. GdV, RP, JR, GM, JM, BC, and VP also acknowledge support by the Programa de Cooperacion Cientifica – ECOS SUD Program C16U02. NL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 669253), ABD acknowledges support from the ERC advanced grant “Cosmic Gas”. LW acknowledges support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2, and TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE).. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345, 094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also based on observations obtained with the NASA/ESA Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013). All plots in this paper were created using Matplotlib (Hunter 2007).","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","article_processing_charge":"No","title":"Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE","date_created":"2022-07-06T10:09:36Z","language":[{"iso":"eng"}],"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","gravitational lensing: strong / galaxies: high-redshift / dark ages","reionization","first stars / galaxies: clusters: general / galaxies: luminosity function","mass function"],"citation":{"apa":"de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., … Soucail, G. (2019). Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>","mla":"de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>, vol. 628, A3, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>.","ama":"de La Vieuville G, Bina D, Pello R, et al. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. <i>Astronomy &#38; Astrophysics</i>. 2019;628. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>","ieee":"G. de La Vieuville <i>et al.</i>, “Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE,” <i>Astronomy &#38; Astrophysics</i>, vol. 628. EDP Sciences, 2019.","ista":"de La Vieuville G, Bina D, Pello R, Mahler G, Richard J, Drake AB, Herenz EC, Bauer FE, Clément B, Lagattuta D, Laporte N, Martinez J, Patrício V, Wisotzki L, Zabl J, Bouwens RJ, Contini T, Garel T, Guiderdoni B, Marino RA, Maseda MV, Matthee JJ, Schaye J, Soucail G. 2019. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy &#38; Astrophysics. 628, A3.","chicago":"La Vieuville, G. de, D. Bina, R. Pello, G. Mahler, J. Richard, A. B. Drake, E. C. Herenz, et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>.","short":"G. de La Vieuville, D. Bina, R. Pello, G. Mahler, J. Richard, A.B. Drake, E.C. Herenz, F.E. Bauer, B. Clément, D. Lagattuta, N. Laporte, J. Martinez, V. Patrício, L. Wisotzki, J. Zabl, R.J. Bouwens, T. Contini, T. Garel, B. Guiderdoni, R.A. Marino, M.V. Maseda, J.J. Matthee, J. Schaye, G. Soucail, Astronomy &#38; Astrophysics 628 (2019)."},"arxiv":1,"date_updated":"2022-07-19T09:36:31Z","author":[{"last_name":"de La Vieuville","full_name":"de La Vieuville, G.","first_name":"G."},{"last_name":"Bina","first_name":"D.","full_name":"Bina, D."},{"first_name":"R.","full_name":"Pello, R.","last_name":"Pello"},{"first_name":"G.","full_name":"Mahler, G.","last_name":"Mahler"},{"last_name":"Richard","first_name":"J.","full_name":"Richard, J."},{"full_name":"Drake, A. B.","first_name":"A. B.","last_name":"Drake"},{"last_name":"Herenz","first_name":"E. C.","full_name":"Herenz, E. C."},{"last_name":"Bauer","first_name":"F. E.","full_name":"Bauer, F. E."},{"last_name":"Clément","full_name":"Clément, B.","first_name":"B."},{"last_name":"Lagattuta","full_name":"Lagattuta, D.","first_name":"D."},{"full_name":"Laporte, N.","first_name":"N.","last_name":"Laporte"},{"full_name":"Martinez, J.","first_name":"J.","last_name":"Martinez"},{"first_name":"V.","full_name":"Patrício, V.","last_name":"Patrício"},{"first_name":"L.","full_name":"Wisotzki, L.","last_name":"Wisotzki"},{"first_name":"J.","full_name":"Zabl, J.","last_name":"Zabl"},{"first_name":"R. J.","full_name":"Bouwens, R. J.","last_name":"Bouwens"},{"last_name":"Contini","first_name":"T.","full_name":"Contini, T."},{"first_name":"T.","full_name":"Garel, T.","last_name":"Garel"},{"full_name":"Guiderdoni, B.","first_name":"B.","last_name":"Guiderdoni"},{"first_name":"R. A.","full_name":"Marino, R. A.","last_name":"Marino"},{"full_name":"Maseda, M. V.","first_name":"M. V.","last_name":"Maseda"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Schaye","full_name":"Schaye, J.","first_name":"J."},{"last_name":"Soucail","full_name":"Soucail, G.","first_name":"G."}],"month":"07","date_published":"2019-07-25T00:00:00Z","fulldoi":"https://doi.org/10.1051/0004-6361/201834471","article_number":"A3","status":"public","intvolume":"       628","main_file_link":[{"url":"https://arxiv.org/abs/1905.13696","open_access":"1"}],"day":"25","year":"2019","type":"journal_article","publisher":"EDP Sciences","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":628,"quality_controlled":"1","oa":1,"publication":"Astronomy & Astrophysics","_id":"11505","publication_status":"published","abstract":[{"text":"Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 <  z <  6, 7, 2.9 <  z <  4.0, 4.0 <  z <  5.0, and 5.0 <  z <  6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6.","lang":"eng"}],"doi":"10.1051/0004-6361/201834471"},{"intvolume":"       482","status":"public","fulldoi":"https://doi.org/10.1093/mnras/sty2779","oa_version":"Preprint","publisher":"Oxford University Press","type":"journal_article","year":"2019","day":"01","main_file_link":[{"url":"https://arxiv.org/abs/1710.08422","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"quality_controlled":"1","volume":482,"doi":"10.1093/mnras/sty2779","abstract":[{"text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies.","lang":"eng"}],"publication_status":"published","_id":"11541","publication":"Monthly Notices of the Royal Astronomical Society","article_type":"original","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","external_id":{"arxiv":["1710.08422"]},"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","article_processing_charge":"No","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"language":[{"iso":"eng"}],"date_created":"2022-07-08T10:40:05Z","arxiv":1,"issue":"2","citation":{"apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;482(2):2422-2441. doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>.","ieee":"D. Sobral <i>et al.</i>, “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019.","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441."},"author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"last_name":"Ferrara","first_name":"Andrea","full_name":"Ferrara, Andrea"},{"last_name":"Alegre","full_name":"Alegre, Lara","first_name":"Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"full_name":"Darvish, Behnam","first_name":"Behnam","last_name":"Darvish"}],"date_updated":"2022-08-19T06:49:36Z","page":"2422-2441","month":"01","date_published":"2019-01-01T00:00:00Z"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"       485","fulldoi":"https://doi.org/10.1093/mnras/stz622","status":"public","type":"journal_article","year":"2019","publisher":"Oxford University Press","oa_version":"Preprint","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.00115"}],"doi":"10.1093/mnras/stz622","abstract":[{"text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars.","lang":"eng"}],"_id":"11615","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","oa":1,"volume":485,"title":"A search for red giant solar-like oscillations in all Kepler data","article_processing_charge":"No","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"date_created":"2022-07-18T14:26:03Z","language":[{"iso":"eng"}],"article_type":"original","acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","external_id":{"arxiv":["1903.00115"]},"month":"06","page":"5616-5630","date_published":"2019-06-01T00:00:00Z","issue":"4","arxiv":1,"citation":{"short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","ieee":"M. Hon <i>et al.</i>, “A search for red giant solar-like oscillations in all Kepler data,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>.","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>.","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;485(4):5616-5630. doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., &#38; Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>"},"author":[{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"full_name":"García, Rafael A","first_name":"Rafael A","last_name":"García"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"last_name":"Sharma","full_name":"Sharma, Sanjib","first_name":"Sanjib"},{"full_name":"Colman, Isabel L","first_name":"Isabel L","last_name":"Colman"},{"last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000"}],"date_updated":"2022-08-22T07:35:19Z"},{"_id":"11623","publication":"The Astrophysical Journal Supplement Series","publication_status":"published","abstract":[{"text":"Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy Sph using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with Sph being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods.","lang":"eng"}],"doi":"10.3847/1538-4365/ab3b56","volume":244,"oa":1,"quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","fulldoi":"https://doi.org/10.3847/1538-4365/ab3b56","article_number":"21","intvolume":"       244","day":"19","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1908.05222"}],"oa_version":"Preprint","publisher":"IOP Publishing","type":"journal_article","year":"2019","month":"09","date_published":"2019-09-19T00:00:00Z","citation":{"mla":"Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>.","ama":"Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. 2019;244(1). doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>","apa":"Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J. L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>","short":"A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S. Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement Series 244 (2019).","ieee":"A. R. G. Santos <i>et al.</i>, “Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars,” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1. IOP Publishing, 2019.","ista":"Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 244(1), 21.","chicago":"Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L. van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>."},"arxiv":1,"issue":"1","date_updated":"2022-08-22T08:10:38Z","author":[{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"first_name":"S.","full_name":"Mathur, S.","last_name":"Mathur"},{"last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000"},{"first_name":"J. L.","full_name":"van Saders, J. L.","last_name":"van Saders"},{"full_name":"Metcalfe, T. S.","first_name":"T. S.","last_name":"Metcalfe"},{"last_name":"Simonian","first_name":"G. V. A.","full_name":"Simonian, G. V. A."},{"last_name":"Pinsonneault","first_name":"M. H.","full_name":"Pinsonneault, M. H."}],"scopus_import":"1","publication_identifier":{"issn":["0067-0049"]},"article_processing_charge":"No","title":"Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars","language":[{"iso":"eng"}],"date_created":"2022-07-19T09:21:58Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis","stars: activity","stars: low-mass","stars: rotation","starspots","techniques: photometric"],"extern":"1","article_type":"original","acknowledgement":"The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg, and Isabel L. Colman for helping on the classification of stars. 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 is provided by the National Aeronautics and Space Administration (NASA) Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at the Max Planck Institute for Solar System Research. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy (van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities: MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -","external_id":{"arxiv":["1908.05222"]}}]