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First M87 Event Horizon Telescope Results. VIII. Magnetic Field Structure near The Event Horizon

Akiyama, Kazunori and Algaba, Juan Carlos and Alberdi, Antxon and Alef, Walter and Anantua, Richard and Asada, Keiichi and Azulay, Rebecca and Baczko, Anne-Kathrin and Ball, David and Baloković, Mislav and Barrett, John and Benson, Bradford A. and Bintley, Dan and Blackburn, Lindy and Blundell, Raymond and Boland, Wilfred and Bouman, Katherine L. and Bower, Geoffrey C. and Boyce, Hope and Bremer, Michael and Brinkerink, Christiaan D. and Brissenden, Roger and Britzen, Silke and Broderick, Avery E. and Broguiere, Dominique and Bronzwaer, Thomas and Byun, Do-Young and Carlstrom, John E. and Chael, Andrew and Chan, Chi-kwan and Chatterjee, Shami and Chatterjee, Koushik and Chen, Ming-Tang and Chen, Yongjun and Chesler, Paul M. and Cho, Ilje and Christian, Pierre and Conway, John E. and Cordes, James M. and Crawford, Thomas M. and Crew, Geoffrey B. and Cruz-Osorio, Alejandro and Cui, Yuzhu and Davelaar, Jordy and De Laurentis, Mariafelicia and Deane, Roger and Dempsey, Jessica and Desvignes, Gregory and Dexter, Jason and Doeleman, Sheperd S. and Eatough, Ralph P. and Falcke, Heino and Farah, Joseph and Fish, Vincent L. and Fomalont, Ed and Ford, H. Alyson and Fraga-Encinas, Raquel and Friberg, Per and Fromm, Christian M. and Fuentes, Antonio and Galison, Peter and Gammie, Charles F. and García, Roberto and Gelles, Zachary and Gentaz, Olivier and Georgiev, Boris and Goddi, Ciriaco and Gold, Roman and Gómez, José L. and Gómez-Ruiz, Arturo I. and Gu, Minfeng and Gurwell, Mark and Hada, Kazuhiro and Haggard, Daryl and Hecht, Michael H. and Hesper, Ronald and Himwich, Elizabeth and Ho, Luis C. and Ho, Paul and Honma, Mareki and Huang, Chih-Wei L. and Huang, Lei and Hughes, David H. and Ikeda, Shiro and Inoue, Makoto and Issaoun, Sara and James, David J. and Jannuzi, Buell T. and Janssen, Michael and Jeter, Britton and Jiang, Wu and Jimenez-Rosales, Alejandra and Johnson, Michael D. and Jorstad, Svetlana and Jung, Taehyun and Karami, Mansour and Karuppusamy, Ramesh and Kawashima, Tomohisa and Keating, Garrett K. and Kettenis, Mark and Kim, Dong-Jin and Kim, Jae-Young and Kim, Jongsoo and Kim, Junhan and Kino, Motoki and Koay, Jun Yi and Kofuji, Yutaro and Koch, Patrick M. and Koyama, Shoko and Kramer, Michael and Kramer, Carsten and Krichbaum, Thomas P. and Kuo, Cheng-Yu and Lauer, Tod R. and Lee, Sang-Sung and Levis, Aviad and Li, Yan-Rong and Li, Zhiyuan and Lindqvist, Michael and Lico, Rocco and Lindahl, Greg and Liu, Jun and Liu, Kuo and Liuzzo, Elisabetta and Lo, Wen-Ping and Lobanov, Andrei P. and Loinard, Laurent and Lonsdale, Colin and Lu, Ru-Sen and MacDonald, Nicholas R. and Mao, Jirong and Marchili, Nicola and Markoff, Sera and Marrone, Daniel P. and Marscher, Alan P. and Martí-Vidal, Iván and Matsushita, Satoki and Matthews, Lynn D. and Medeiros, Lia and Menten, Karl M. and Mizuno, Izumi and Mizuno, Yosuke and Moran, James M. and Moriyama, Kotaro and Moscibrodzka, Monika and Müller, Cornelia and Musoke, Gibwa and Mejías, Alejandro Mus and Michalik, Daniel and Nadolski, Andrew and Nagai, Hiroshi and Nagar, Neil M. and Nakamura, Masanori and Narayan, Ramesh and Narayanan, Gopal and Natarajan, Iniyan and Nathanail, Antonios and Neilsen, Joey and Neri, Roberto and Ni, Chunchong and Noutsos, Aristeidis and Nowak, Michael A. and Okino, Hiroki and Olivares, Héctor and Ortiz-León, Gisela N. and Oyama, Tomoaki and Özel, Feryal and Palumbo, Daniel C. M. and Park, Jongho and Patel, Nimesh and Pen, Ue-Li and Pesce, Dominic W. and Piétu, Vincent and Plambeck, Richard and PopStefanija, Aleksandar and Porth, Oliver and Pötzl, Felix M. and Prather, Ben and Preciado-López, Jorge A. and Psaltis, Dimitrios and Pu, Hung-Yi and Ramakrishnan, Venkatessh and Rao, Ramprasad and Rawlings, Mark G. and Raymond, Alexander W. and Rezzolla, Luciano and Ricarte, Angelo and Ripperda, Bart and Roelofs, Freek and Rogers, Alan and Ros, Eduardo and Rose, Mel and Roshanineshat, Arash and Rottmann, Helge and Roy, Alan L. and Ruszczyk, Chet and Rygl, Kazi L. J. and Sánchez, Salvador and Sánchez-Arguelles, David and Sasada, Mahito and Savolainen, Tuomas and Schloerb, F. Peter and Schuster, Karl-Friedrich and Shao, Lijing and Shen, Zhiqiang and Small, Des and Sohn, Bong Won and SooHoo, Jason and Sun, He and Tazaki, Fumie and Tetarenko, Alexandra J. and Tiede, Paul and Tilanus, Remo P. J. and Titus, Michael and Toma, Kenji and Torne, Pablo and Trent, Tyler and Traianou, Efthalia and Trippe, Sascha and Bemmel, Ilse van and van Langevelde, Huib Jan and van Rossum, Daniel R. and Wagner, Jan and Ward-Thompson, Derek and Wardle, John and Weintroub, Jonathan and Wex, Norbert and Wharton, Robert and Wielgus, Maciek and Wong, George N. and Wu, Qingwen and Yoon, Doosoo and Young, André and Young, Ken and Younsi, Ziri and Yuan, Feng and Yuan, Ye-Fei and Zensus, J. Anton and Zhao, Guang-Yao and Zhao, Shan-Shan (2021) First M87 Event Horizon Telescope Results. VIII. Magnetic Field Structure near The Event Horizon. Astrophysical Journal Letters, 910 (1). Art. No. L13. ISSN 2041-8205.

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Event Horizon Telescope (EHT) observations at 230 GHz have now imaged polarized emission around the supermassive black hole in M87 on event-horizon scales. This polarized synchrotron radiation probes the structure of magnetic fields and the plasma properties near the black hole. Here we compare the resolved polarization structure observed by the EHT, along with simultaneous unresolved observations with the Atacama Large Millimeter/submillimeter Array, to expectations from theoretical models. The low fractional linear polarization in the resolved image suggests that the polarization is scrambled on scales smaller than the EHT beam, which we attribute to Faraday rotation internal to the emission region. We estimate the average density ne ~ 10⁴⁻⁷ cm⁻³, magnetic field strength B ~ 1–30 G, and electron temperature T_e ~ (1–12) × 10¹⁰ K of the radiating plasma in a simple one-zone emission model. We show that the net azimuthal linear polarization pattern may result from organized, poloidal magnetic fields in the emission region. In a quantitative comparison with a large library of simulated polarimetric images from general relativistic magnetohydrodynamic (GRMHD) simulations, we identify a subset of physical models that can explain critical features of the polarimetric EHT observations while producing a relativistic jet of sufficient power. The consistent GRMHD models are all of magnetically arrested accretion disks, where near-horizon magnetic fields are dynamically important. We use the models to infer a mass accretion rate onto the black hole in M87 of (3–20) × 10⁻⁴ M⊙ yr⁻¹.

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URLURL TypeDescription
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Additional Information:© 2021. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2020 December 2; revised 2021 February 3; accepted 2021 February 8; published 2021 March 24. The authors of the present Letter thank the following organizations and programs: the Academy of Finland (projects 274477, 284495, 312496, 315721); Agencia Nacional de Investigación y Desarrollo (ANID), Chile via NCN19_058 (TITANs), and Fondecyt 3190878; the Alexander von Humboldt Stiftung; an Alfred P. Sloan Research Fellowship; Allegro, the European ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA and the astronomy institutes of the University of Amsterdam, Leiden University and Radboud University; the black hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Consejo Nacional de Ciencia y Tecnología (CONACYT, Mexico, projects U0004-246083, U0004-259839, F0003-272050, M0037-279006, F0003-281692, 104497, 275201, 263356, 57265507); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Dirección General de Asuntos del Personal Académico-Universidad Nacional Autónoma de México (DGAPA-UNAM, projects IN112417 and IN112820); the EACOA Fellowship of the East Asia Core Observatories Association; the European Research Council Synergy Grant "BlackHoleCam: Imaging the Event Horizon of Black Holes" (grant 610058); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177 and GenT Program (project CIDEGENT/2018/021); MICINN Research Project PID2019-108995GB-C22; the Gordon and Betty Moore Foundation (grants GBMF- 3561, GBMF-5278); the Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche TEONGRAV; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; Joint Princeton/Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships, research at the Flatiron Institute is supported by the Simons Foundation; the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJSSW- SYS008, ZDBS-LY-SLH011). We further thank the Leverhulme Trust Early Career Research Fellowship; the Max-Planck-Gesellschaft (MPG); the Max Planck Partner Group of the MPG and the CAS; the MEXT/JSPS KAKENHI (grants 18KK0090, JP18K13594, JP18K03656, JP18H03721, 18K03709, 18H01245, JP19H01943, 25120007); the Malaysian Fundamental Research Grant Scheme (FRGS) FRGS/1/2019/STG02/UM/02/6; the MIT International Science and Technology Initiatives (MISTI) Funds; the Ministry of Science and Technology (MOST) of Taiwan (105-2112-M-001-025-MY3, 106-2112-M-001-011, 106-2119- M-001-027, 107-2119-M-001-017, 107-2119-M-001-020, 107-2119-M-110-005, 108-2112-M-001-048, and 109-2124-M-001-005); the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC20K1567, NASA Astrophysics Theory Program grant 80NSSC20K0527, NASA grant NNX17AL82G, Hubble Fellowship grant HST-HF2-51431.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555, and NASA NuSTAR award 80NSSC20K0645); the National Institute of Natural Sciences (NINS) of Japan; the National Key Research and Development Program of China (grant 2016YFA0400704, 2016YFA0400702); the National Science Foundation (NSF, grants AST-0096454, AST-0352953, AST-0521233, AST-0705062, AST-0905844, AST-0922984, AST-1126433, AST-1140030, DGE-1144085, AST-1207704, AST-1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-1310896, AST-1337663, AST-1440254, AST-1555365, AST-1615796, AST-1715061, AST-1716327, AST-1716536, OISE-1743747, AST-1816420, AST-1903847, AST-1935980, AST-2034306); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11933007, 11991052, 11991053); a fellowship of China Postdoctoral Science Foundation (2020M671266); the Natural Sciences and Engineering Research Council of Canada (NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral Program); the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants 2014H1A2A1018695, NRF-2015H1A2A1033752, 2015-R1D1A1A01056807, the Korea Research Fellowship Program: NRF-2015H1D3A1066561, Basic Research Support Grant 2019R1F1A1059721); the Netherlands Organization for Scientific Research (NWO) VICI award (grant 639.043.513) and Spinoza Prize SPI 78-409; the New Scientific Frontiers with Precision Radio Interferometry Fellowship awarded by the South African Radio Astronomy Observatory (SARAO), which is a facility of the National Research Foundation (NRF), an agency of the Department of Science and Innovation (DSI) of South Africa; the South African Research Chairs Initiative of the Department of Science and Innovation and National Research Foundation; the Onsala Space Observatory (OSO) national infrastructure, for the provisioning of its facilities/observational support (OSO receives funding through the Swedish Research Council under grant 2017-00648) the Perimeter Institute for Theoretical Physics (research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Research, Innovation and Science); the Spanish Ministerio de Economía y Competitividad (grants PGC2018-098915-B-C21, AYA2016-80889-P, PID2019-108995GB-C21); the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709); the Toray Science Foundation; the Consejería de Economía, Conocimiento, Empresas y Universidad of the Junta de Andalucía (grant P18-FR-1769), the Consejo Superior de Investigaciones Científicas (grant 2019AEP112); the US Department of Energy (USDOE) through the Los Alamos National Laboratory (operated by Triad National Security, LLC, for the National Nuclear Security Administration of the USDOE (Contract 89233218CNA000001); the European Union's Horizon 2020 research and innovation program under grant agreement No 730562 RadioNet; ALMA North America Development Fund; the Academia Sinica; Chandra TM6-17006X and DD7-18089X; the GenT Program (Generalitat Valenciana) Project CIDEGENT/2018/021. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), supported by NSF grant ACI-1548562, and CyVerse, supported by NSF grants DBI-0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2 resource at TACC was allocated through TG-AST170024 and TG-AST080026N. XSEDE JetStream resource at PTI and TACC was allocated through AST170028. The simulations were performed in part on the SuperMUC cluster at the LRZ in Garching, on the LOEWE cluster in CSC in Frankfurt, and on the HazelHen cluster at the HLRS in Stuttgart. This research was enabled in part by support provided by Compute Ontario (, Calcul Quebec ( and Compute Canada ( We thank the staff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.01154.V. ALMA is a partnership of the European Southern Observatory (ESO; Europe, representing its member states), NSF, and National Institutes of Natural Sciences of Japan, together with National Research Council (Canada), Ministry of Science and Technology (MOST; Taiwan), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA; Taiwan), and Korea Astronomy and Space Science Institute (KASI; Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc. (AUI)/NRAO, and the National Astronomical Observatory of Japan (NAOJ). The NRAO is a facility of the NSF operated under cooperative agreement by AUI. This paper has made use of the following APEX data: Project ID T-091.F-0006-2013. APEX is a collaboration between the Max-Planck-Institut für Radioastronomie (Germany), ESO, and the Onsala Space Observatory (Sweden). The SMA is a joint project between the SAO and ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. The JCMT is operated by the East Asian Observatory on behalf of the NAOJ, ASIAA, and KASI, as well as the Ministry of Finance of China, Chinese Academy of Sciences, and the National Key R&D Program (No. 2017YFA0402700) of China. Additional funding support for the JCMT is provided by the Science and Technologies Facility Council (UK) and participating universities in the UK and Canada. The LMT is a project operated by the Instituto Nacional de Astrófisica, Óptica, y Electrónica (Mexico) and the University of Massachusetts at Amherst (USA), with financial support from the Consejo Nacional de Ciencia y Tecnología and the National Science Foundation. The IRAM 30-m telescope on Pico Veleta, Spain is operated by IRAM and supported by CNRS (Centre National de la Recherche Scientifique, France), MPG (Max-Planck- Gesellschaft, Germany) and IGN (Instituto Geográfico Nacional, Spain). The SMT is operated by the Arizona Radio Observatory, a part of the Steward Observatory of the University of Arizona, with financial support of operations from the State of Arizona and financial support for instrumentation development from the NSF. The SPT is supported by the National Science Foundation through grant PLR- 1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. The SPT hydrogen maser was provided on loan from the GLT, courtesy of ASIAA. The EHTC has received generous donations of FPGA chips from Xilinx Inc., under the Xilinx University Program. The EHTC has benefited from technology shared under open-source license by the Collaboration for Astronomy Signal Processing and Electronics Research (CASPER). The EHT project is grateful to T4Science and Microsemi for their assistance with Hydrogen Masers. This research has made use of NASA's Astrophysics Data System. We gratefully acknowledge the support provided by the extended staff of the ALMA, both from the inception of the ALMA Phasing Project through the observational campaigns of 2017 and 2018. We would like to thank A. Deller and W. Brisken for EHT-specific support with the use of DiFX. We acknowledge the significance that Maunakea, where the SMA and JCMT EHT stations are located, has for the indigenous Hawaiian people.
Group:Astronomy Department
Funding AgencyGrant Number
Academy of Finland274477
Academy of Finland284495
Academy of Finland312496
Academy of Finland315721
Agencia Nacional de Investigación y Desarrollo (ANID)NCN19_058
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3190878
Alexander von Humboldt StiftungUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Nederlandse Onderzoekschool Voor Astronomie (NOVA)UNSPECIFIED
University of AmsterdamUNSPECIFIED
Leiden UniversityUNSPECIFIED
Radboud UniversityUNSPECIFIED
Harvard UniversityUNSPECIFIED
John Templeton Foundation60477
China Scholarship CouncilUNSPECIFIED
Consejo Nacional de Ciencia y Tecnología (CONACYT)U0004-246083
Consejo Nacional de Ciencia y Tecnología (CONACYT)U0004-259839
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Consejo Nacional de Ciencia y Tecnología (CONACYT)104497
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Consejo Nacional de Ciencia y Tecnología (CONACYT)263356
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Dirección General de Asuntos del Personal Académico-Universidad Nacional Autónoma de MéxicoIN112417
Dirección General de Asuntos del Personal Académico-Universidad Nacional Autónoma de MéxicoIN112820
East Asia Core Observatories AssociationUNSPECIFIED
European Research Council (ERC)610058
Generalitat ValencianaAPOSTD/2018/177
Generalitat ValencianaCIDEGENT/2018/021
Ministerio de Ciencia e Innovación (MCINN)PID2019-108995GB-C22
Gordon and Betty Moore FoundationGBMF-3561
Gordon and Betty Moore FoundationGBMF-5278
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
International Max Planck Research School (IMPRS) for Astronomy and AstrophysicsUNSPECIFIED
Princeton UniversityUNSPECIFIED
Flatiron InstituteUNSPECIFIED
Columbia UniversityUNSPECIFIED
Simons FoundationUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17J08829
Key Research Program of Frontier SciencesUNSPECIFIED
Chinese Academy of SciencesQYZDJ-SSW-SLH057
Chinese Academy of SciencesQYZDJSSW-SYS008
Chinese Academy of SciencesZDBS-LY-SLH011
Leverhulme TrustUNSPECIFIED
Max-Planck-Gesellschaft (MPG)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)18KK0090
Japan Society for the Promotion of Science (JSPS)JP18K13594
Japan Society for the Promotion of Science (JSPS)JP18K03656
Japan Society for the Promotion of Science (JSPS)JP18H03721
Japan Society for the Promotion of Science (JSPS)18K03709
Japan Society for the Promotion of Science (JSPS)18H01245
Japan Society for the Promotion of Science (JSPS)JP19H01943
Japan Society for the Promotion of Science (JSPS)25120007
Malaysian Fundamental Research GrantFRGS/1/2019/STG02/UM/02/6
Massachusetts Institute of Technology (MIT)UNSPECIFIED
Ministry of Science and Technology (Taipei)105-2112-M-001-025-MY3
Ministry of Science and Technology (Taipei)106-2112-M-001-011
Ministry of Science and Technology (Taipei)106-2119-M-001-027
Ministry of Science and Technology (Taipei)107-2119-M-001-017
Ministry of Science and Technology (Taipei)107-2119-M-001-020
Ministry of Science and Technology (Taipei)107-2119-M-110-005
Ministry of Science and Technology (Taipei)108-2112-M-001-048
Ministry of Science and Technology (Taipei)109-2124-M-001-005
NASA Hubble FellowshipHST-HF2-51431.001-A
National Institute of Natural Sciences (NINS)UNSPECIFIED
National Key Research and Development Program of China2016YFA0400704
National Key Research and Development Program of China2016YFA0400702
NSF Graduate Research FellowshipDGE-1144085
National Natural Science Foundation of China11573051
National Natural Science Foundation of China11633006
National Natural Science Foundation of China11650110427
National Natural Science Foundation of China10625314
National Natural Science Foundation of China11721303
National Natural Science Foundation of China11725312
National Natural Science Foundation of China11933007
National Natural Science Foundation of China11991052
National Natural Science Foundation of China11991053
China Postdoctoral Science Foundation2020M671266
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
National Research Foundation of Korea2014H1A2A1018695
National Research Foundation of KoreaNRF-2015H1A2A1033752
National Research Foundation of Korea2015-R1D1A1A01056807
National Research Foundation of KoreaNRF-2015H1D3A1066561
National Research Foundation of Korea2019R1F1A1059721
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.043.513
Spinoza PrizeSPI 78-409
South African Radio Astronomy Observatory (SARAO)UNSPECIFIED
National Research Foundation (South Africa)UNSPECIFIED
Department of Science and Innovation (South Africa)UNSPECIFIED
Department of Science and Innovation (South Africa)UNSPECIFIED
Onsala Space Observatory (OSO)UNSPECIFIED
Swedish Research Council2017-00648
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Department of Innovation, Science and Economic Development (Canada)UNSPECIFIED
Province of Ontario Ministry of Research, Innovation and ScienceUNSPECIFIED
Severo OchoaPGC2018-098915-B-C21
Ministerio de Economía y Competitividad (MINECO)AYA2016-80889-P
Ministerio de Economía y Competitividad (MINECO)PID2019-108995GB-C21
Severo OchoaSEV-2017-0709
Toray Science FoundationUNSPECIFIED
Junta de AndalucíaP18-FR-1769
Consejo Superior de Investigaciones Científicas2019AEP112
Department of Energy (DOE)89233218CNA000001
European Research Council (ERC)730562 RadioNet
ALMA North America Development FundUNSPECIFIED
Academia SinicaUNSPECIFIED
NASA ChandraTM6-17006X
NASA ChandraDD7-18089X
Generalitat ValencianaCIDEGENT/2018/021
Compute OntarioUNSPECIFIED
National Key Research and Development Program of China2017YFA0402700
Science and Technology Facilities Council (STFC)UNSPECIFIED
State of ArizonaUNSPECIFIED
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF 947
Subject Keywords:Accretion; Black holes; Event horizons; Jets; Kerr black holes; Magnetic fields; Magnetohydrodynamics; Plasma astrophysics; Polarimetry; Radiative transfer; Radio jets; Relativistic jets
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Accretion (14); Black holes (162); Event horizons (479); Jets (870); Kerr black holes (886); Magnetic fields (994); Magnetohydrodynamics (1964); Plasma astrophysics (1261); Polarimetry (1278); Radiative transfer
Record Number:CaltechAUTHORS:20210324-142607806
Persistent URL:
Official Citation:First M87 Event Horizon Telescope Results. VIII. Magnetic Field Structure near The Event Horizon. The Event Horizon Telescope Collaboration et al 2021 ApJL 910 L13
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108546
Deposited By: Tony Diaz
Deposited On:24 Mar 2021 22:29
Last Modified:24 Mar 2021 22:29

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