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dc.contributorInstitute of Astronomy, KU Leuven, Leuven, Belgium; Anton Pannekoek Institute for Astronomy, Amsterdam, The Netherlands
dc.contributorInstitute of Astronomy, KU Leuven, Leuven, Belgium
dc.contributorInstitute of Astronomy, KU Leuven, Leuven, Belgium; Royal Observatory of Belgium, Brussels, Belgium
dc.contributorCenter for Astrophysics, Harvard & Smithsonian, Cambridge, MA, USA; Harvard Society of Fellows, Cambridge, MA, USA; Max-Planck Institute for Astronomy, Heidelberg, Germany
dc.contributorArgelander-Institut für Astronomie, Universität Bonn, Bonn, Germany; Max-Planck-Institut für Radioastronomie, Bonn, Germany
dc.contributorEscola de Ciências e Tecnologia, Universidade Federal do Rio Grande do Norte, Natal, Brazil; Programa de Pós-graduação em Física, Universidade do Estado do Rio Grande do Norte, Mossoró, Brazil
dc.contributorEuropean Southern Observatory, Santiago de Chile, Chile
dc.contributorEuropean Organisation for Astronomical Research in the Southern Hemisphere (ESO), Garching, Germany
dc.contributorDepartment of Physics & Astronomy, University of Sheffield, Sheffield, UK
dc.contributorICREA, Barcelona, Spain; Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Barcelona, Spain
dc.contributorAstronomical Observatory, University of Warsaw, Warsaw, Poland
dc.contributorDepartment of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia, Canada
dc.contributorInstituto de Astrofísica de Canarias, La Laguna, Spain; Departamento Astrofísica, Universidad de La Laguna, La Laguna, Spain
dc.contributorCentro de Astrobiología, CSIC-INTA, Villanueva de la Cañada, Spain
dc.contributorDépartament de physique, Université de Montréal, Montreal, Quebec, Canada
dc.contributorAstronomical Observatory, University of Warsaw, Warsaw, Poland; Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
dc.contributorHeidelberger Institut für Theoretische Studien, Heidelberg, Germany; Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany
dc.contributorAnton Pannekoek Institute for Astronomy, Amsterdam, The Netherlands
dc.contributorDepartment of Physics, University of Warwick, Coventry, UK
dc.contributorArmagh Observatory and Planetarium, Armagh, UK
dc.contributor.authorShenar, Tomer
dc.contributor.authorSana, Hugues
dc.contributor.authorMahy, Laurent
dc.contributor.authorEl-Badry, Kareem
dc.contributor.authorMarchant, Pablo
dc.contributor.authorLanger, Norbert
dc.contributor.authorHawcroft, Calum
dc.contributor.authorFabry, Matthias
dc.contributor.authorSen, Koushik
dc.contributor.authorAlmeida, Leonardo A.
dc.contributor.authorAbdul-Masih, Michael
dc.contributor.authorBodensteiner, Julia
dc.contributor.authorCrowther, Paul A.
dc.contributor.authorGieles, Mark
dc.contributor.authorGromadzki, Mariusz
dc.contributor.authorHénault-Brunet, Vincent
dc.contributor.authorHerrero, Artemio
dc.contributor.authorde Koter, Alex
dc.contributor.authorIwanek, Patryk
dc.contributor.authorKozłowski, Szymon
dc.contributor.authorLennon, Daniel J.
dc.contributor.authorMaíz Apellániz, Jesús
dc.contributor.authorMróz, Przemysław
dc.contributor.authorMoffat, Anthony F. J.
dc.contributor.authorPicco, Annachiara
dc.contributor.authorPietrukowicz, Paweł
dc.contributor.authorPoleski, Radosław
dc.contributor.authorRybicki, Krzysztof
dc.contributor.authorSchneider, Fabian R. N.
dc.contributor.authorSkowron, Dorota M.
dc.contributor.authorSkowron, Jan
dc.contributor.authorSoszyński, Igor
dc.contributor.authorSzymański, Michał K.
dc.contributor.authorToonen, Silvia
dc.contributor.authorUdalski, Andrzej
dc.contributor.authorUlaczyk, Krzysztof
dc.contributor.authorVink, Jorick S.
dc.contributor.authorWrona, Marcin
dc.date.accessioned2024-02-02T13:30:29Z
dc.date.available2024-02-02T13:30:29Z
dc.date.issued2022-07-01T00:00:00Z
dc.identifier.doi10.1038/s41550-022-01730-y
dc.identifier.doi10.48550/arXiv.2207.07675
dc.identifier.other2022arXiv220707675S
dc.identifier.otherastro-ph.HE
dc.identifier.otherastro-ph.GA
dc.identifier.otherastro-ph.SR
dc.identifier.other2022arXiv220707675S
dc.identifier.otherarXiv:2207.07675
dc.identifier.other10.1038/s41550-022-01730-y
dc.identifier.other10.48550/arXiv.2207.07675
dc.identifier.other2022NatAs...6.1085S
dc.identifier.other0000-0003-0642-8107
dc.identifier.other0000-0001-6656-4130
dc.identifier.other0000-0003-0688-7987
dc.identifier.other-
dc.identifier.other0000-0002-0338-8181
dc.identifier.other0000-0003-0145-8964
dc.identifier.other0000-0003-4200-7852
dc.identifier.other0000-0002-8134-4854
dc.identifier.other0000-0002-9552-7010
dc.identifier.other0000-0002-9716-1868
dc.identifier.other0000-0002-1650-1518
dc.identifier.other0000-0003-2927-5465
dc.identifier.other0000-0002-1198-3167
dc.identifier.other0000-0003-3063-4867
dc.identifier.other0000-0003-0825-3443
dc.identifier.other0000-0001-7016-1692
dc.identifier.other0000-0003-3095-6049
dc.identifier.other0000-0002-2339-5899
dc.identifier.other0000-0002-9245-6368
dc.identifier.other0000-0002-9326-9329
dc.identifier.other0000-0002-5965-1022
dc.identifier.other0000-0001-9439-604X
dc.identifier.other0000-0002-2335-1730
dc.identifier.other0000-0002-7777-0842
dc.identifier.other0000-0001-5207-5619
dc.identifier.other0000-0002-8445-4397
dc.identifier.other0000-0002-3051-274X
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1522
dc.description.abstractStellar-mass black holes are the final remnants of stars born with more than 15 solar masses. Billions are expected to reside in the Local Group, yet only a few are known, mostly detected through X-rays emitted as they accrete material from a companion star. Here, we report on VFTS 243: a massive X-ray-faint binary in the Large Magellanic Cloud. With an orbital period of 10.4 d, it comprises an O-type star of 25 solar masses and an unseen companion of at least nine solar masses. Our spectral analysis excludes a non-degenerate companion at a 5σ confidence level. The minimum companion mass implies that it is a black hole. No other X-ray-quiet black hole is unambiguously known outside our Galaxy. The (near-)circular orbit and kinematics of VFTS 243 imply that the collapse of the progenitor into a black hole was associated with little or no ejected material or black-hole kick. Identifying such unique binaries substantially impacts the predicted rates of gravitational-wave detections and properties of core-collapse supernovae across the cosmos.
dc.publisherNature Astronomy
dc.titleAn X-ray-quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud
dc.typearticle
dc.source.journalNatAs
dc.source.journalNatAs...6
dc.source.volume6
refterms.dateFOA2024-02-02T13:30:29Z
dc.identifier.bibcode2022NatAs...6.1085S


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