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description Publicationkeyboard_double_arrow_right Article 2020 Italy, Spain, Netherlands, Netherlands, Netherlands, Netherlands, United Kingdom, Netherlands, United States, Netherlands, Italy, Finland, Denmark, FrancePublisher:EDP Sciences Funded by:NSERC, NSF | Graduate Research Fellows..., NSF | PSCIC Full Proposal: The ... +15 projectsNSERC ,NSF| Graduate Research Fellowship Program (GRFP) ,NSF| PSCIC Full Proposal: The iPlant Collaborative: A Cyberinfrastructure-Centered Community for a New Plant Biology ,NWO| From micro- to mega-scales: understanding how black holes shape the local Universe ,AKA| Physics of Black Hole-Powered Jets ,AKA| Physics of Black Hole-Powered Jets ,EC| RadioNet ,AKA| Physics of Black Hole-Powered Jets ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| The iPlant Collaborative: Cyberinfrastructure for the Life Sciences ,NSF| CyVerse: Cyberinfrastructure for the Life Sciences ,NSF| Physics Frontier Center at the Kavli Institute for Cosmological Physics: Pushing Cosmology to the Edge ,NSF| The Arizona Radio Observatory: Surveying the ISM through Millimeter and Sub-millimeter Spectroscopy ,EC| AENEAS ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| Cosmological Research with the 10-meter South Pole Telescope ,EC| BLACKHOLECAM ,NSF| Probing Gravitational Physics with Event Horizon Telescope and Gravitational Wave Observations of Black HolesF. Roelofs; M. Janssen; I. Natarajan; R. Deane; J. Davelaar; H. Olivares; O. Porth; S. N. Paine; K. L. Bouman; R. P. J. Tilanus; I. M. van Bemmel; H. Falcke; K. Akiyama; A. Alberdi; W. Alef; K. Asada; R. Azulay; A. Baczko; D. Ball; M. Baloković; J. Barrett; D. Bintley; L. Blackburn; W. Boland; G. C. Bower; M. Bremer; C. D. Brinkerink; R. Brissenden; S. Britzen; A. E. Broderick; D. Broguiere; T. Bronzwaer; D. Byun; J. E. Carlstrom; A. Chael; C. Chan; S. Chatterjee; K. Chatterjee; M. Chen; Y. Chen; I. Cho; P. Christian; J. E. Conway; J. M. Cordes; G. B. Crew; Y. Cui; M. De Laurentis; J. Dempsey; G. Desvignes; J. Dexter; S. S. Doeleman; R. P. Eatough; V. L. Fish; E. Fomalont; R. Fraga-Encinas; P. Friberg; C. M. Fromm; J. L. Gómez; P. Galison; C. F. Gammie; R. García; O. Gentaz; B. Georgiev; C. Goddi; R. Gold; M. Gu; M. Gurwell; K. Hada; M. H. Hecht; R. Hesper; L. C. Ho; P. Ho; M. Honma; C. L. Huang; L. Huang; D. H. Hughes; S. Ikeda; M. Inoue; S. Issaoun; D. J. James; B. T. Jannuzi; B. Jeter; W. Jiang; M. D. Johnson; S. Jorstad; T. Jung; M. Karami; R. Karuppusamy; T. Kawashima; G. K. Keating; M. Kettenis; J. Kim; J. Kim; J. Kim; M. Kino; J. Y. Koay; P. M. Koch; S. Koyama; M. Kramer; C. Kramer; T. P. Krichbaum; C. Kuo; T. R. Lauer; S. Lee; Y. Li; Z. Li; M. Lindqvist; R. Lico; K. Liu; E. Liuzzo; W. Lo; A. P. Lobanov; L. Loinard; C. Lonsdale; R. Lu; N. R. MacDonald; J. Mao; S. Markoff; D. P. Marrone; A. P. Marscher; I. Martí-Vidal; S. Matsushita; L. D. Matthews; L. Medeiros; K. M. Menten; Y. Mizuno; I. Mizuno; J. M. Moran; K. Moriyama; M. Moscibrodzka; C. Müller; H. Nagai; N. M. Nagar; M. Nakamura; R. Narayan; G. Narayanan; R. Neri; C. Ni; A. Noutsos; H. Okino; H. Olivares; G. N. Ortiz-León; T. Oyama; F. Özel; D. C. M. Palumbo; N. Patel; U. Pen; D. W. Pesce; V. Piétu; R. Plambeck; A. PopStefanija; B. Prather; J. A. Preciado-López; D. Psaltis; H. Pu; V. Ramakrishnan; R. Rao; M. G. Rawlings; A. W. Raymond; L. Rezzolla; B. Ripperda; A. Rogers; E. Ros; M. Rose; A. Roshanineshat; H. Rottmann; A. L. Roy; C. Ruszczyk; B. R. Ryan; K. L. J. Rygl; S. Sánchez; D. Sánchez-Arguelles; M. Sasada; T. Savolainen; F. P. Schloerb; K. Schuster; L. Shao; Z. Shen; D. Small; B. Won Sohn; J. SooHoo; F. Tazaki; P. Tiede; M. Titus; K. Toma; P. Torne; E. Traianou; T. Trent; S. Trippe; S. Tsuda; H. J. van Langevelde; D. R. van Rossum; J. Wagner; J. Wardle; J. Weintroub; N. Wex; R. Wharton; M. Wielgus; G. N. Wong; Q. Wu; Z. Younsi; Y. Yuan; G. Zhao; S. Zhao;This work is supported by the ERC Synergy Grant "BlackHoleCam: Imaging the Event Horizon of Black Holes" (Grant 610058). I. Natarajan and R. Deane are grateful for the support from 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 Technology (DST) of South Africa. The authors of the present paper further thank the following organizations and programmes: the Academy of Finland (projects 274477, 284495, 312496); the Advanced European Network of E-infrastructures for Astronomy with the SKA (AENEAS) project, supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement 731016; the Alexander von Humboldt Stiftung; the Black Hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Comision Nacional de Investigacio Cientifica y Tecnologica (CONICYT, Chile, via PIA ACT172033, Fondecyt 1171506, BASAL AFB-170002, ALMAconicyt 31140007); Consejo Nacional de Ciencia y Tecnologia (CONACYT, Mexico, projects 104497, 275201, 279006, 281692); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Direccion General de Asuntos del Personal Academico-Universidad Nacional Autonoma de Mexico (DGAPA-UNAM, project IN112417); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177; 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 GenT Program (Generalitat Valenciana) under project CIDEGENT/2018/021; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; the Jansky Fellowship program of the National Radio Astronomy Observatory (NRAO); 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, QYZDJ-SSW-SYS008); 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, 25120007); 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-001027, 107-2119-M-001-017, 107-2119-M-001-020, and 107-2119-M-110-005); the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC17K0649); NASA through the NASA 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; 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-1312651, AST-1337663, AST-1440254, AST-1555365, AST-1715061, AST-1615796, AST-1716327, OISE-1743747, AST-1816420); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11933007); 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 Youth Thousand Talents Program of China; the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants NRF-2015H1A2A1033752, 2015-R1D1A1A01056807, the Korea Research Fellowship Program: NRF-2015H1D3A1066561); 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 Technology (DST) of South Africa; 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 Princeton/Flatiron Postdoctoral Prize Fellowship; the Russian Science Foundation (grant 17-12-01029); the Spanish Ministerio de Economia y Competitividad (grants AYA2015-63939-C21-P, AYA2016-80889-P); the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); the Toray Science Foundation; 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 Italian Ministero dell'Istruzione Universita e Ricerca through the grant Progetti Premiali 2012-iALMA (CUP C52I13000140001); the European Union's Horizon 2020 research and innovation programme under grant agreement No 730562 RadioNet; ALMA North America Development Fund; the Academia Sinica; Chandra TM6-17006X. 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 DBI1743442. XSEDE Stampede2 resource at TACC was allocated through TGAST170024 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 (http://computeontario.ca), Calcul Quebec (http://www. calculquebec.ca) and Compute Canada (http://www.computecanada.ca).We thank the sta ff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00841.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. APEX is a collaboration between the Max-Planck-Institut fur 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 Astrofisica, Optica, y Electronica (Mexico) and the University of Massachusetts at Amherst (USA). The IRAM 30m 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 Geografico 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. The software presented in this work makes use of the Numpy (van derWalt et al. 2011), Scipy (Jones et al. 2001), Astropy (Astropy Collaboration 2013, 2018) libraries and the KERN software bundle (Molenaar & Smirnov 2018). Context. Realistic synthetic observations of theoretical source models are essential for our understanding of real observational data. In using synthetic data, one can verify the extent to which source parameters can be recovered and evaluate how various data corruption effects can be calibrated. These studies are the most important when proposing observations of new sources, in the characterization of the capabilities of new or upgraded instruments, and when verifying model-based theoretical predictions in a direct comparison with observational data. Aims. We present the SYnthetic Measurement creator for long Baseline Arrays (SYMBA), a novel synthetic data generation pipeline for Very Long Baseline Interferometry (VLBI) observations. SYMBA takes into account several realistic atmospheric, instrumental, and calibration effects. Methods. We used SYMBA to create synthetic observations for the Event Horizon Telescope (EHT), a millimetre VLBI array, which has recently captured the first image of a black hole shadow. After testing SYMBA with simple source and corruption models, we study the importance of including all corruption and calibration effects, compared to the addition of thermal noise only. Using synthetic data based on two example general relativistic magnetohydrodynamics (GRMHD) model images of M 87, we performed case studies to assess the image quality that can be obtained with the current and future EHT array for different weather conditions. Results. Our synthetic observations show that the effects of atmospheric and instrumental corruptions on the measured visibilities are significant. Despite these effects, we demonstrate how the overall structure of our GRMHD source models can be recovered robustly with the EHT2017 array after performing calibration steps, which include fringe fitting, a priori amplitude and network calibration, and self-calibration. With the planned addition of new stations to the EHT array in the coming years, images could be reconstructed with higher angular resolution and dynamic range. In our case study, these improvements allowed for a distinction between a thermal and a non-thermal GRMHD model based on salient features in reconstructed images. © 2020 ESO.
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For further information contact us at helpdesk@openaire.eudescription Publicationkeyboard_double_arrow_right Article 2019 France, Netherlands, Netherlands, Netherlands, United Kingdom, Netherlands, Italy, Italy, United States, Netherlands, Finland, Japan, Spain, NetherlandsPublisher:American Astronomical Society Funded by:NSF | Center for Cosmological P..., NSERC, NSF | Graduate Research Fellows... +15 projectsNSF| Center for Cosmological Physics ,NSERC ,NSF| Graduate Research Fellowship Program (GRFP) ,EC| BLACKHOLECAM ,NSF| Physics Frontier Center at the Kavli Institute for Cosmological Physics: Pushing Cosmology to the Edge ,NSF| The Arizona Radio Observatory: Surveying the ISM through Millimeter and Sub-millimeter Spectroscopy ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| Cosmological Research with the 10-meter South Pole Telescope ,NSF| PSCIC Full Proposal: The iPlant Collaborative: A Cyberinfrastructure-Centered Community for a New Plant Biology ,NWO| From micro- to mega-scales: understanding how black holes shape the local Universe ,AKA| Physics of Black Hole-Powered Jets ,NSF| The iPlant Collaborative: Cyberinfrastructure for the Life Sciences ,EC| AENEAS ,NSF| CyVerse: Cyberinfrastructure for the Life Sciences ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| MRI: Development of an ALMA Beamformer for Ultra High Resolution VLBI and High Frequency Phased Array Science ,EC| RadioNet ,AKA| Physics of Black Hole-Powered JetsKazunori Akiyama; Antxon Alberdi; Walter Alef; Keiichi Asada; Rebecca Azulay; Anne Kathrin Baczko; David Ball; Mislav Baloković; John E. Barrett; Dan Bintley; Lindy Blackburn; W. Boland; Katherine L. Bouman; Geoffrey C. Bower; Michael Bremer; Christiaan D. Brinkerink; Roger Brissenden; Silke Britzen; Avery E. Broderick; Thomas Bronzwaer; Do-Young Byun; Andrew Chael; Chi-kwan Chan; Shami Chatterjee; Koushik Chatterjee; Ming-Tang Chen; Yi Chen; Ilje Cho; Pierre Christian; John Conway; James M. Cordes; Geoffrey B. Crew; Yuzhu Cui; Jordy Davelaar; Mariafelicia De Laurentis; Roger Deane; Jessica Dempsey; Gregory Desvignes; Jason Dexter; Sheperd S. Doeleman; R. P. Eatough; Heino Falcke; Vincent L. Fish; Ed Fomalont; Raquel Fraga-Encinas; Per Friberg; José L. Gómez; Peter Galison; Charles F. Gammie; Roberto Garcia; Olivier Gentaz; Boris Georgiev; Ciriaco Goddi; Roman Gold; Minfeng Gu; Mark Gurwell; Kazuhiro Hada; Michael H. Hecht; Ronald Hesper; Luis C. Ho; Paul T. P. Ho; Mareki Honma; Chih-Wei Locutus Huang; Lei Huang; David H. Hughes; Shiro Ikeda; Makoto Inoue; Sara Issaoun; David J. James; Buell T. Jannuzi; Michael Janssen; Britton Jeter; Wu Jiang; Michael D. Johnson; Svetlana G. Jorstad; Taehyun Jung; Mansour Karami; Ramesh Karuppusamy; Tomohisa Kawashima; Garrett K. Keating; Mark Kettenis; Jae-Young Kim; Junhan Kim; Motoki Kino; Jun Yi Koay; Patrick M. Koch; Shoko Koyama; Michael Kramer; Carsten Kramer; Thomas P. Krichbaum; C. Y. Kuo; Tod R. Lauer; Sang-Sung Lee; Yan-Rong Li; Zhiyuan Li; Michael Lindqvist; Kuo Liu; Elisabetta Liuzzo; Andrei P. Lobanov; Laurent Loinard; Colin J. Lonsdale; Ru-Sen Lu; Nicholas R. MacDonald; Jirong Mao; Sera Markoff; Daniel P. Marrone; Alan P. Marscher; Satoki Matsushita; Lynn D. Matthews; Lia Medeiros; Karl M. Menten; Yosuke Mizuno; Izumi Mizuno; James M. Moran; Kotaro Moriyama; Monika Moscibrodzka; Cornelia Müller; Hiroshi Nagai; Neil M. Nagar; Masanori Nakamura; Ramesh Narayan; Gopal Narayanan; Iniyan Natarajan; Roberto Neri; Chunchong Ni; Aristeidis Noutsos; Hector Olivares; Gisela N. Ortiz-León; Feryal Özel; Daniel C. M. Palumbo; Nimesh A. Patel; Ue-Li Pen; Dominic W. Pesce; Richard L. Plambeck; Aleksandar Popstefanija; Oliver Porth; Ben Prather; Jorge A. Preciado-López; Dimitrios Psaltis; Hung Yi Pu; Venkatessh Ramakrishnan; Ramprasad Rao; Mark G. Rawlings; Alexander W. Raymond; Luciano Rezzolla; Bart Ripperda; Freek Roelofs; Alan E. E. Rogers; Eduardo Ros; Mel Rose; Arash Roshanineshat; Helge Rottmann; Alan L. Roy; Chet Ruszczyk; Benjamin R. Ryan; Kazi L.J. Rygl; David Sánchez-Arguelles; Mahito Sasada; Tuomas Savolainen; F. Peter Schloerb; Karl Friedrich Schuster; Lijing Shao; Zhiqiang Shen; Des Small; Bong Won Sohn; Jason SooHoo; Fumie Tazaki; Paul Tiede; Remo P. J. Tilanus; Michael Titus; Kenji Toma; Pablo Torne; Tyler Trent; Sascha Trippe; Ilse van Bemmel; Huib Jan van Langevelde; Daniel R. van Rossum; Jan Wagner; John Wardle; Jonathan Weintroub; Norbert Wex; Robert Wharton; Maciek Wielgus; George N. Wong; Qingwen Wu; André Young; Ken H. Young; Ziri Younsi; Feng Yuan; Ye-Fei Yuan; J. Anton Zensus; Guang-Yao Zhao; Shan Shan Zhao; Ziyan Zhu; Roger J. Cappallo; Joseph R. Farah; Thomas W. Folkers; Zheng Meyer-Zhao; Daniel Michalik; A. Nadolski; Hiroaki Nishioka; Nicolas Pradel; Rurik A. Primiani; Kamal Souccar; Paul Yamaguchi;Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJ-SSW-SYS008); 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, 25120007); 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-M001-011, 106-2119-M-001-027, 107-2119-M-001-017, 107- 2119-M-001-020, and 107-2119-M-110-005); the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC17K0649); 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, AST0705062, AST-0905844, AST-0922984, AST-1126433, AST1140030, DGE-1144085, AST-1207704, AST-1207730, AST1207752, MRI-1228509, OPP-1248097, AST-1310896, AST1312651, AST-1337663, AST-1440254, AST-1555365, AST1715061, AST-1615796, AST-1614868, AST-1716327, OISE1743747, AST-1816420); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11873028, 11873073, U1531245, 11473010); 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 Youth Thousand Talents Program of China; the National Research Foundation of Korea (grant 2015-R1D1A1A01056807, the Global PhD Fellowship Grant: NRF-2015H1A2A1033752, and the Korea Research Fellowship Program: NRF-2015H1D3A1066561); 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 The authors of this Letter thank the following organizations and programs: the Academy of Finland (projects 274477, 284495, 312496); the Advanced European Network of E-infrastructures for Astronomy with the SKA (AENEAS) project, supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement 731016; the Alexander von Humboldt Stiftung; the Black Hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Comisión Nacional de Investigación Científica y Tecnológica (CONICYT, Chile, via PIA ACT172033, Fondecyt 1171506, BASAL AFB170002, ALMA-conicyt 31140007); Consejo Nacional de Ciencia y Tecnología (CONACYT, Mexico, projects 104497, 275201, 279006, 281692); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Dirección General de Asuntos del Personal Académico-Universidad Nacional 9 The Astrophysical Journal Letters, 875:L1 (17pp), 2019 April 10 The EHT Collaboration et al. Autónoma de México (DGAPA-UNAM, project IN112417); the European Research Council (ERC) Synergy Grant “BlackHoleCam: Imaging the Event Horizon of Black Holes” (grant 610058); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177; 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; the Jansky Fellowship program of the National Radio Astronomy Observatory (NRAO); the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); JSPS Overseas Research Fellowships; the Key Research Program of Frontier Sciences, Chinese 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 Technology (DST) of South Africa; 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 Canada and by the Province of Ontario through the Ministry of Economic Development, Job Creation and Trade); the Russian Science Foundation (grant 17-12-01029); the Spanish Ministerio de Economía y Competitividad (grants AYA2015-63939-C2-1-P, AYA2016-80889-P); 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 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 Italian Ministero dell’Istruzione Università e Ricerca through the grant Progetti Premiali 2012-iALMA (CUP C52I13000140001); the European Unionʼs Horizon 2020 research and innovation programme under grant agreement No 730562 RadioNet; ALMA North America Development Fund; Chandra TM6-17006X We present the calibration and reduction of Event Horizon Telescope (EHT) 1.3 mm radio wavelength observations of the supermassive black hole candidate at the center of the radio galaxy M87 and the quasar 3C 279, taken during the 2017 April 5–11 observing campaign. These global very long baseline interferometric observations include for the first time the highly sensitive Atacama Large Millimeter/submillimeter Array (ALMA); reaching an angular resolution of 25 μas, with characteristic sensitivity limits of ~1 mJy on baselines to ALMA and ~10 mJy on other baselines. The observations present challenges for existing data processing tools, arising from the rapid atmospheric phase fluctuations, wide recording bandwidth, and highly heterogeneous array. In response, we developed three independent pipelines for phase calibration and fringe detection, each tailored to the specific needs of the EHT. The final data products include calibrated total intensity amplitude and phase information. They are validated through a series of quality assurance tests that show consistency across pipelines and set limits on baseline systematic errors of 2% in amplitude and 1° in phase. The M87 data reveal the presence of two nulls in correlated flux density at ~3.4 and ~8.3 Gλ and temporal evolution in closure quantities, indicating intrinsic variability of compact structure on a timescale of days, or several light-crossing times for a few billion solar-mass black hole. These measurements provide the first opportunity to image horizon-scale structure in M87.© 2019. The American Astronomical Society Peer reviewed
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description Publicationkeyboard_double_arrow_right Article 2020 Italy, Spain, Netherlands, Netherlands, Netherlands, Netherlands, United Kingdom, Netherlands, United States, Netherlands, Italy, Finland, Denmark, FrancePublisher:EDP Sciences Funded by:NSERC, NSF | Graduate Research Fellows..., NSF | PSCIC Full Proposal: The ... +15 projectsNSERC ,NSF| Graduate Research Fellowship Program (GRFP) ,NSF| PSCIC Full Proposal: The iPlant Collaborative: A Cyberinfrastructure-Centered Community for a New Plant Biology ,NWO| From micro- to mega-scales: understanding how black holes shape the local Universe ,AKA| Physics of Black Hole-Powered Jets ,AKA| Physics of Black Hole-Powered Jets ,EC| RadioNet ,AKA| Physics of Black Hole-Powered Jets ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| The iPlant Collaborative: Cyberinfrastructure for the Life Sciences ,NSF| CyVerse: Cyberinfrastructure for the Life Sciences ,NSF| Physics Frontier Center at the Kavli Institute for Cosmological Physics: Pushing Cosmology to the Edge ,NSF| The Arizona Radio Observatory: Surveying the ISM through Millimeter and Sub-millimeter Spectroscopy ,EC| AENEAS ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| Cosmological Research with the 10-meter South Pole Telescope ,EC| BLACKHOLECAM ,NSF| Probing Gravitational Physics with Event Horizon Telescope and Gravitational Wave Observations of Black HolesF. Roelofs; M. Janssen; I. Natarajan; R. Deane; J. Davelaar; H. Olivares; O. Porth; S. N. Paine; K. L. Bouman; R. P. J. Tilanus; I. M. van Bemmel; H. Falcke; K. Akiyama; A. Alberdi; W. Alef; K. Asada; R. Azulay; A. Baczko; D. Ball; M. Baloković; J. Barrett; D. Bintley; L. Blackburn; W. Boland; G. C. Bower; M. Bremer; C. D. Brinkerink; R. Brissenden; S. Britzen; A. E. Broderick; D. Broguiere; T. Bronzwaer; D. Byun; J. E. Carlstrom; A. Chael; C. Chan; S. Chatterjee; K. Chatterjee; M. Chen; Y. Chen; I. Cho; P. Christian; J. E. Conway; J. M. Cordes; G. B. Crew; Y. Cui; M. De Laurentis; J. Dempsey; G. Desvignes; J. Dexter; S. S. Doeleman; R. P. Eatough; V. L. Fish; E. Fomalont; R. Fraga-Encinas; P. Friberg; C. M. Fromm; J. L. Gómez; P. Galison; C. F. Gammie; R. García; O. Gentaz; B. Georgiev; C. Goddi; R. Gold; M. Gu; M. Gurwell; K. Hada; M. H. Hecht; R. Hesper; L. C. Ho; P. Ho; M. Honma; C. L. Huang; L. Huang; D. H. Hughes; S. Ikeda; M. Inoue; S. Issaoun; D. J. James; B. T. Jannuzi; B. Jeter; W. Jiang; M. D. Johnson; S. Jorstad; T. Jung; M. Karami; R. Karuppusamy; T. Kawashima; G. K. Keating; M. Kettenis; J. Kim; J. Kim; J. Kim; M. Kino; J. Y. Koay; P. M. Koch; S. Koyama; M. Kramer; C. Kramer; T. P. Krichbaum; C. Kuo; T. R. Lauer; S. Lee; Y. Li; Z. Li; M. Lindqvist; R. Lico; K. Liu; E. Liuzzo; W. Lo; A. P. Lobanov; L. Loinard; C. Lonsdale; R. Lu; N. R. MacDonald; J. Mao; S. Markoff; D. P. Marrone; A. P. Marscher; I. Martí-Vidal; S. Matsushita; L. D. Matthews; L. Medeiros; K. M. Menten; Y. Mizuno; I. Mizuno; J. M. Moran; K. Moriyama; M. Moscibrodzka; C. Müller; H. Nagai; N. M. Nagar; M. Nakamura; R. Narayan; G. Narayanan; R. Neri; C. Ni; A. Noutsos; H. Okino; H. Olivares; G. N. Ortiz-León; T. Oyama; F. Özel; D. C. M. Palumbo; N. Patel; U. Pen; D. W. Pesce; V. Piétu; R. Plambeck; A. PopStefanija; B. Prather; J. A. Preciado-López; D. Psaltis; H. Pu; V. Ramakrishnan; R. Rao; M. G. Rawlings; A. W. Raymond; L. Rezzolla; B. Ripperda; A. Rogers; E. Ros; M. Rose; A. Roshanineshat; H. Rottmann; A. L. Roy; C. Ruszczyk; B. R. Ryan; K. L. J. Rygl; S. Sánchez; D. Sánchez-Arguelles; M. Sasada; T. Savolainen; F. P. Schloerb; K. Schuster; L. Shao; Z. Shen; D. Small; B. Won Sohn; J. SooHoo; F. Tazaki; P. Tiede; M. Titus; K. Toma; P. Torne; E. Traianou; T. Trent; S. Trippe; S. Tsuda; H. J. van Langevelde; D. R. van Rossum; J. Wagner; J. Wardle; J. Weintroub; N. Wex; R. Wharton; M. Wielgus; G. N. Wong; Q. Wu; Z. Younsi; Y. Yuan; G. Zhao; S. Zhao;This work is supported by the ERC Synergy Grant "BlackHoleCam: Imaging the Event Horizon of Black Holes" (Grant 610058). I. Natarajan and R. Deane are grateful for the support from 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 Technology (DST) of South Africa. The authors of the present paper further thank the following organizations and programmes: the Academy of Finland (projects 274477, 284495, 312496); the Advanced European Network of E-infrastructures for Astronomy with the SKA (AENEAS) project, supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement 731016; the Alexander von Humboldt Stiftung; the Black Hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Comision Nacional de Investigacio Cientifica y Tecnologica (CONICYT, Chile, via PIA ACT172033, Fondecyt 1171506, BASAL AFB-170002, ALMAconicyt 31140007); Consejo Nacional de Ciencia y Tecnologia (CONACYT, Mexico, projects 104497, 275201, 279006, 281692); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Direccion General de Asuntos del Personal Academico-Universidad Nacional Autonoma de Mexico (DGAPA-UNAM, project IN112417); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177; 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 GenT Program (Generalitat Valenciana) under project CIDEGENT/2018/021; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; the Jansky Fellowship program of the National Radio Astronomy Observatory (NRAO); 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, QYZDJ-SSW-SYS008); 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, 25120007); 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-001027, 107-2119-M-001-017, 107-2119-M-001-020, and 107-2119-M-110-005); the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC17K0649); NASA through the NASA 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; 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-1312651, AST-1337663, AST-1440254, AST-1555365, AST-1715061, AST-1615796, AST-1716327, OISE-1743747, AST-1816420); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11933007); 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 Youth Thousand Talents Program of China; the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants NRF-2015H1A2A1033752, 2015-R1D1A1A01056807, the Korea Research Fellowship Program: NRF-2015H1D3A1066561); 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 Technology (DST) of South Africa; 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 Princeton/Flatiron Postdoctoral Prize Fellowship; the Russian Science Foundation (grant 17-12-01029); the Spanish Ministerio de Economia y Competitividad (grants AYA2015-63939-C21-P, AYA2016-80889-P); the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); the Toray Science Foundation; 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 Italian Ministero dell'Istruzione Universita e Ricerca through the grant Progetti Premiali 2012-iALMA (CUP C52I13000140001); the European Union's Horizon 2020 research and innovation programme under grant agreement No 730562 RadioNet; ALMA North America Development Fund; the Academia Sinica; Chandra TM6-17006X. 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 DBI1743442. XSEDE Stampede2 resource at TACC was allocated through TGAST170024 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 (http://computeontario.ca), Calcul Quebec (http://www. calculquebec.ca) and Compute Canada (http://www.computecanada.ca).We thank the sta ff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00841.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. APEX is a collaboration between the Max-Planck-Institut fur 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 Astrofisica, Optica, y Electronica (Mexico) and the University of Massachusetts at Amherst (USA). The IRAM 30m 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 Geografico 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. The software presented in this work makes use of the Numpy (van derWalt et al. 2011), Scipy (Jones et al. 2001), Astropy (Astropy Collaboration 2013, 2018) libraries and the KERN software bundle (Molenaar & Smirnov 2018). Context. Realistic synthetic observations of theoretical source models are essential for our understanding of real observational data. In using synthetic data, one can verify the extent to which source parameters can be recovered and evaluate how various data corruption effects can be calibrated. These studies are the most important when proposing observations of new sources, in the characterization of the capabilities of new or upgraded instruments, and when verifying model-based theoretical predictions in a direct comparison with observational data. Aims. We present the SYnthetic Measurement creator for long Baseline Arrays (SYMBA), a novel synthetic data generation pipeline for Very Long Baseline Interferometry (VLBI) observations. SYMBA takes into account several realistic atmospheric, instrumental, and calibration effects. Methods. We used SYMBA to create synthetic observations for the Event Horizon Telescope (EHT), a millimetre VLBI array, which has recently captured the first image of a black hole shadow. After testing SYMBA with simple source and corruption models, we study the importance of including all corruption and calibration effects, compared to the addition of thermal noise only. Using synthetic data based on two example general relativistic magnetohydrodynamics (GRMHD) model images of M 87, we performed case studies to assess the image quality that can be obtained with the current and future EHT array for different weather conditions. Results. Our synthetic observations show that the effects of atmospheric and instrumental corruptions on the measured visibilities are significant. Despite these effects, we demonstrate how the overall structure of our GRMHD source models can be recovered robustly with the EHT2017 array after performing calibration steps, which include fringe fitting, a priori amplitude and network calibration, and self-calibration. With the planned addition of new stations to the EHT array in the coming years, images could be reconstructed with higher angular resolution and dynamic range. In our case study, these improvements allowed for a distinction between a thermal and a non-thermal GRMHD model based on salient features in reconstructed images. © 2020 ESO.
NARCIS arrow_drop_down Astronomy and AstrophysicsArticle . 2020OA@INAF - Istituto Nazionale di AstrofisicaArticle . 2020Data sources: OA@INAF - Istituto Nazionale di AstrofisicaRecolector de Ciencia Abierta, RECOLECTA; DIGITAL.CSICArticle . 2020Astronomy and Astrophysics; METIS Research Information System; NARCIS; Archivio della ricerca - Università degli studi di Napoli Federico IIArticle . 2020 . Peer-reviewedLicense: EDP Sciences Copyright and Publication Licensing PolicyUniversity of Southern Denmark Research OutputArticle . 2020Data sources: University of Southern Denmark Research OutputAaltodoc Publication ArchiveArticle . 2020 . Peer-reviewedData sources: Aaltodoc Publication Archiveadd ClaimPlease grant OpenAIRE to access and update your ORCID works.This Research product is the result of merged Research products in OpenAIRE.
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For further information contact us at helpdesk@openaire.euAccess RoutesGreen bronze 18 citations 18 popularity Top 10% influence Average impulse Top 10% Powered by BIP!visibility 97visibility views 97 download downloads 77 Powered bymore_vert NARCIS arrow_drop_down Astronomy and AstrophysicsArticle . 2020OA@INAF - Istituto Nazionale di AstrofisicaArticle . 2020Data sources: OA@INAF - Istituto Nazionale di AstrofisicaRecolector de Ciencia Abierta, RECOLECTA; DIGITAL.CSICArticle . 2020Astronomy and Astrophysics; METIS Research Information System; NARCIS; Archivio della ricerca - Università degli studi di Napoli Federico IIArticle . 2020 . Peer-reviewedLicense: EDP Sciences Copyright and Publication Licensing PolicyUniversity of Southern Denmark Research OutputArticle . 2020Data sources: University of Southern Denmark Research OutputAaltodoc Publication ArchiveArticle . 2020 . Peer-reviewedData sources: Aaltodoc Publication Archiveadd ClaimPlease grant OpenAIRE to access and update your ORCID works.This Research product is the result of merged Research products in OpenAIRE.
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For further information contact us at helpdesk@openaire.eudescription Publicationkeyboard_double_arrow_right Article 2019 France, Netherlands, Netherlands, Netherlands, United Kingdom, Netherlands, Italy, Italy, United States, Netherlands, Finland, Japan, Spain, NetherlandsPublisher:American Astronomical Society Funded by:NSF | Center for Cosmological P..., NSERC, NSF | Graduate Research Fellows... +15 projectsNSF| Center for Cosmological Physics ,NSERC ,NSF| Graduate Research Fellowship Program (GRFP) ,EC| BLACKHOLECAM ,NSF| Physics Frontier Center at the Kavli Institute for Cosmological Physics: Pushing Cosmology to the Edge ,NSF| The Arizona Radio Observatory: Surveying the ISM through Millimeter and Sub-millimeter Spectroscopy ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| Cosmological Research with the 10-meter South Pole Telescope ,NSF| PSCIC Full Proposal: The iPlant Collaborative: A Cyberinfrastructure-Centered Community for a New Plant Biology ,NWO| From micro- to mega-scales: understanding how black holes shape the local Universe ,AKA| Physics of Black Hole-Powered Jets ,NSF| The iPlant Collaborative: Cyberinfrastructure for the Life Sciences ,EC| AENEAS ,NSF| CyVerse: Cyberinfrastructure for the Life Sciences ,NSF| Collaborative Research: Building an Event Horizon Telescope: (Sub)millimeter VLBI from the South Pole Telescope ,NSF| MRI: Development of an ALMA Beamformer for Ultra High Resolution VLBI and High Frequency Phased Array Science ,EC| RadioNet ,AKA| Physics of Black Hole-Powered JetsKazunori Akiyama; Antxon Alberdi; Walter Alef; Keiichi Asada; Rebecca Azulay; Anne Kathrin Baczko; David Ball; Mislav Baloković; John E. Barrett; Dan Bintley; Lindy Blackburn; W. Boland; Katherine L. Bouman; Geoffrey C. Bower; Michael Bremer; Christiaan D. Brinkerink; Roger Brissenden; Silke Britzen; Avery E. Broderick; Thomas Bronzwaer; Do-Young Byun; Andrew Chael; Chi-kwan Chan; Shami Chatterjee; Koushik Chatterjee; Ming-Tang Chen; Yi Chen; Ilje Cho; Pierre Christian; John Conway; James M. Cordes; Geoffrey B. Crew; Yuzhu Cui; Jordy Davelaar; Mariafelicia De Laurentis; Roger Deane; Jessica Dempsey; Gregory Desvignes; Jason Dexter; Sheperd S. Doeleman; R. P. Eatough; Heino Falcke; Vincent L. Fish; Ed Fomalont; Raquel Fraga-Encinas; Per Friberg; José L. Gómez; Peter Galison; Charles F. Gammie; Roberto Garcia; Olivier Gentaz; Boris Georgiev; Ciriaco Goddi; Roman Gold; Minfeng Gu; Mark Gurwell; Kazuhiro Hada; Michael H. Hecht; Ronald Hesper; Luis C. Ho; Paul T. P. Ho; Mareki Honma; Chih-Wei Locutus Huang; Lei Huang; David H. Hughes; Shiro Ikeda; Makoto Inoue; Sara Issaoun; David J. James; Buell T. Jannuzi; Michael Janssen; Britton Jeter; Wu Jiang; Michael D. Johnson; Svetlana G. Jorstad; Taehyun Jung; Mansour Karami; Ramesh Karuppusamy; Tomohisa Kawashima; Garrett K. Keating; Mark Kettenis; Jae-Young Kim; Junhan Kim; Motoki Kino; Jun Yi Koay; Patrick M. Koch; Shoko Koyama; Michael Kramer; Carsten Kramer; Thomas P. Krichbaum; C. Y. Kuo; Tod R. Lauer; Sang-Sung Lee; Yan-Rong Li; Zhiyuan Li; Michael Lindqvist; Kuo Liu; Elisabetta Liuzzo; Andrei P. Lobanov; Laurent Loinard; Colin J. Lonsdale; Ru-Sen Lu; Nicholas R. MacDonald; Jirong Mao; Sera Markoff; Daniel P. Marrone; Alan P. Marscher; Satoki Matsushita; Lynn D. Matthews; Lia Medeiros; Karl M. Menten; Yosuke Mizuno; Izumi Mizuno; James M. Moran; Kotaro Moriyama; Monika Moscibrodzka; Cornelia Müller; Hiroshi Nagai; Neil M. Nagar; Masanori Nakamura; Ramesh Narayan; Gopal Narayanan; Iniyan Natarajan; Roberto Neri; Chunchong Ni; Aristeidis Noutsos; Hector Olivares; Gisela N. Ortiz-León; Feryal Özel; Daniel C. M. Palumbo; Nimesh A. Patel; Ue-Li Pen; Dominic W. Pesce; Richard L. Plambeck; Aleksandar Popstefanija; Oliver Porth; Ben Prather; Jorge A. Preciado-López; Dimitrios Psaltis; Hung Yi Pu; Venkatessh Ramakrishnan; Ramprasad Rao; Mark G. Rawlings; Alexander W. Raymond; Luciano Rezzolla; Bart Ripperda; Freek Roelofs; Alan E. E. Rogers; Eduardo Ros; Mel Rose; Arash Roshanineshat; Helge Rottmann; Alan L. Roy; Chet Ruszczyk; Benjamin R. Ryan; Kazi L.J. Rygl; David Sánchez-Arguelles; Mahito Sasada; Tuomas Savolainen; F. Peter Schloerb; Karl Friedrich Schuster; Lijing Shao; Zhiqiang Shen; Des Small; Bong Won Sohn; Jason SooHoo; Fumie Tazaki; Paul Tiede; Remo P. J. Tilanus; Michael Titus; Kenji Toma; Pablo Torne; Tyler Trent; Sascha Trippe; Ilse van Bemmel; Huib Jan van Langevelde; Daniel R. van Rossum; Jan Wagner; John Wardle; Jonathan Weintroub; Norbert Wex; Robert Wharton; Maciek Wielgus; George N. Wong; Qingwen Wu; André Young; Ken H. Young; Ziri Younsi; Feng Yuan; Ye-Fei Yuan; J. Anton Zensus; Guang-Yao Zhao; Shan Shan Zhao; Ziyan Zhu; Roger J. Cappallo; Joseph R. Farah; Thomas W. Folkers; Zheng Meyer-Zhao; Daniel Michalik; A. Nadolski; Hiroaki Nishioka; Nicolas Pradel; Rurik A. Primiani; Kamal Souccar; Paul Yamaguchi;Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJ-SSW-SYS008); 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, 25120007); 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-M001-011, 106-2119-M-001-027, 107-2119-M-001-017, 107- 2119-M-001-020, and 107-2119-M-110-005); the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC17K0649); 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, AST0705062, AST-0905844, AST-0922984, AST-1126433, AST1140030, DGE-1144085, AST-1207704, AST-1207730, AST1207752, MRI-1228509, OPP-1248097, AST-1310896, AST1312651, AST-1337663, AST-1440254, AST-1555365, AST1715061, AST-1615796, AST-1614868, AST-1716327, OISE1743747, AST-1816420); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11873028, 11873073, U1531245, 11473010); 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 Youth Thousand Talents Program of China; the National Research Foundation of Korea (grant 2015-R1D1A1A01056807, the Global PhD Fellowship Grant: NRF-2015H1A2A1033752, and the Korea Research Fellowship Program: NRF-2015H1D3A1066561); 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 The authors of this Letter thank the following organizations and programs: the Academy of Finland (projects 274477, 284495, 312496); the Advanced European Network of E-infrastructures for Astronomy with the SKA (AENEAS) project, supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement 731016; the Alexander von Humboldt Stiftung; the Black Hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Comisión Nacional de Investigación Científica y Tecnológica (CONICYT, Chile, via PIA ACT172033, Fondecyt 1171506, BASAL AFB170002, ALMA-conicyt 31140007); Consejo Nacional de Ciencia y Tecnología (CONACYT, Mexico, projects 104497, 275201, 279006, 281692); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Dirección General de Asuntos del Personal Académico-Universidad Nacional 9 The Astrophysical Journal Letters, 875:L1 (17pp), 2019 April 10 The EHT Collaboration et al. Autónoma de México (DGAPA-UNAM, project IN112417); the European Research Council (ERC) Synergy Grant “BlackHoleCam: Imaging the Event Horizon of Black Holes” (grant 610058); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177; 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; the Jansky Fellowship program of the National Radio Astronomy Observatory (NRAO); the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); JSPS Overseas Research Fellowships; the Key Research Program of Frontier Sciences, Chinese 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 Technology (DST) of South Africa; 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 Canada and by the Province of Ontario through the Ministry of Economic Development, Job Creation and Trade); the Russian Science Foundation (grant 17-12-01029); the Spanish Ministerio de Economía y Competitividad (grants AYA2015-63939-C2-1-P, AYA2016-80889-P); 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 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 Italian Ministero dell’Istruzione Università e Ricerca through the grant Progetti Premiali 2012-iALMA (CUP C52I13000140001); the European Unionʼs Horizon 2020 research and innovation programme under grant agreement No 730562 RadioNet; ALMA North America Development Fund; Chandra TM6-17006X We present the calibration and reduction of Event Horizon Telescope (EHT) 1.3 mm radio wavelength observations of the supermassive black hole candidate at the center of the radio galaxy M87 and the quasar 3C 279, taken during the 2017 April 5–11 observing campaign. These global very long baseline interferometric observations include for the first time the highly sensitive Atacama Large Millimeter/submillimeter Array (ALMA); reaching an angular resolution of 25 μas, with characteristic sensitivity limits of ~1 mJy on baselines to ALMA and ~10 mJy on other baselines. The observations present challenges for existing data processing tools, arising from the rapid atmospheric phase fluctuations, wide recording bandwidth, and highly heterogeneous array. In response, we developed three independent pipelines for phase calibration and fringe detection, each tailored to the specific needs of the EHT. The final data products include calibrated total intensity amplitude and phase information. They are validated through a series of quality assurance tests that show consistency across pipelines and set limits on baseline systematic errors of 2% in amplitude and 1° in phase. The M87 data reveal the presence of two nulls in correlated flux density at ~3.4 and ~8.3 Gλ and temporal evolution in closure quantities, indicating intrinsic variability of compact structure on a timescale of days, or several light-crossing times for a few billion solar-mass black hole. These measurements provide the first opportunity to image horizon-scale structure in M87.© 2019. The American Astronomical Society Peer reviewed
NARCIS arrow_drop_down NARCIS; Radboud RepositoryArticle . 2019The Astrophysical Journal LettersArticle . 2019Radboud Repository; The Astrophysical Journal LettersArticle . 2019Aaltodoc Publication ArchiveArticle . 2019 . Peer-reviewedData sources: Aaltodoc Publication ArchiveOA@INAF - Istituto Nazionale di AstrofisicaArticle . 2019Data sources: OA@INAF - Istituto Nazionale di AstrofisicaRecolector de Ciencia Abierta, RECOLECTA; DIGITAL.CSICArticle . 2019 . Peer-reviewedThe Astrophysical Journal; The Astrophysical Journal LettersArticle . 2019 . Peer-reviewedLicense: CC BYarXiv.org e-Print ArchiveOther literature type . Preprint . 2019Data sources: arXiv.org e-Print ArchiveHAL - UPEC / UPEM; HAL-Pasteur; HAL-Inserm; Hal-DiderotArticle . 2019https://doi.org/10.48550/arxiv...Article . 2019License: arXiv Non-Exclusive DistributionData sources: Dataciteadd ClaimPlease grant OpenAIRE to access and update your ORCID works.This Research product is the result of merged Research products in OpenAIRE.
You have already added works in your ORCID record related to the merged Research product.This Research product is the result of merged Research products in OpenAIRE.
You have already added works in your ORCID record related to the merged Research product.All Research productsarrow_drop_down <script type="text/javascript"> <!-- document.write('<div id="oa_widget"></div>'); document.write('<script type="text/javascript" src="https://www.openaire.eu/index.php?option=com_openaire&view=widget&format=raw&projectId=10.3847/2041-8213/ab0c57&type=result"></script>'); --> </script>
For further information contact us at helpdesk@openaire.euAccess RoutesGreen gold 504 citations 504 popularity Top 0.1% influence Top 1% impulse Top 0.01% Powered by BIP!visibility 30visibility views 30 download downloads 32 Powered bymore_vert NARCIS arrow_drop_down NARCIS; Radboud RepositoryArticle . 2019The Astrophysical Journal LettersArticle . 2019Radboud Repository; The Astrophysical Journal LettersArticle . 2019Aaltodoc Publication ArchiveArticle . 2019 . Peer-reviewedData sources: Aaltodoc Publication ArchiveOA@INAF - Istituto Nazionale di AstrofisicaArticle . 2019Data sources: OA@INAF - Istituto Nazionale di AstrofisicaRecolector de Ciencia Abierta, RECOLECTA; DIGITAL.CSICArticle . 2019 . Peer-reviewedThe Astrophysical Journal; The Astrophysical Journal LettersArticle . 2019 . Peer-reviewedLicense: CC BYarXiv.org e-Print ArchiveOther literature type . Preprint . 2019Data sources: arXiv.org e-Print ArchiveHAL - UPEC / UPEM; HAL-Pasteur; HAL-Inserm; Hal-DiderotArticle . 2019https://doi.org/10.48550/arxiv...Article . 2019License: arXiv Non-Exclusive DistributionData sources: Dataciteadd ClaimPlease grant OpenAIRE to access and update your ORCID works.This Research product is the result of merged Research products in OpenAIRE.
You have already added works in your ORCID record related to the merged Research product.This Research product is the result of merged Research products in OpenAIRE.
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