CaltechAUTHORS
  A Caltech Library Service

Event Horizon Telescope imaging of the archetypal blazar 3C 279 at an extreme 20 microarcsecond resolution

Kim, Jae-Young and Krichbaum, Thomas P. and Broderick, Avery E. and Wielgus, Maciek and Blackburn, Lindy and Gómez, José L. and Johnson, Michael D. and Bouman, Katherine L. and Chael, Andrew and Akiyama, Kazunori and Jorstad, Svetlana and Marscher, Alan P. and Issaoun, Sara and Janssen, Michael and Chan, Chi-kwan and Savolainen, Tuomas and Pesce, Dominic W. and Özel, Feryal and Alberdi, Antxon and Alef, Walter and Asada, Keiichi and Azulay, Rebecca and Baczko, Anne-Kathrin and Ball, David and Baloković, Mislav and Barrett, John and Bintley, Dan and Boland, Wilfred and Bower, Geoffrey C. and Bremer, Michael and Brinkerink, Christiaan D. and Brissenden, Roger and Britzen, Silke and Broguiere, Dominique and Bronzwaer, Thomas and Byun, Do-Young and Carlstrom, John E. and Chatterjee, Shami and Chatterjee, Koushik and Chen, Ming-Tang and Chen, Yongjun and Cho, Ilje and Christian, Pierre and Conway, John E. and Cordes, James M. and Crew, Geoffrey B. 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 Fish, Vincent L. and Fomalont, Ed and Fraga-Encinas, Raquel and Friberg, Per and Fromm, Christian M. and Galison, Peter and Gammie, Charles F. and García, Roberto and Gentaz, Olivier and Georgiev, Boris and Goddi, Ciriaco and Gold, Roman and Gómez-Ruiz, Arturo I. and Gu, Minfeng and Gurwell, Mark and Hada, Kazuhiro and Hecht, Michael H. and Hesper, Ronald 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 James, David J. and Jannuzi, Buell T. and Jeter, Britton and Jiang, Wu and Jimenez-Rosales, Alejandra and Jung, Taehyun and Karami, Mansour and Karuppusamy, Ramesh and Kawashima, Tomohisa and Keating, Garrett K. and Kettenis, Mark and Kim, Junhan and Kim, Jongsoo and Kino, Motoki and Koay, Jun Yi and Koch, Patrick M. and Koyama, Shoko and Kramer, Michael and Kramer, Carsten and Kuo, Cheng-Yu and Lauer, Tod R. and Lee, Sang-Sung and Li, Yan-Rong and Li, Zhiyuan and Lindqvist, Michael and Lico, Rocco 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 Markoff, Sera and Marrone, Daniel P. and Martí-Vidal, Iván and Matsushita, Satoki and Matthews, Lynn D. and Medeiros, Lia and Menten, Karl M. and Mizuno, Yosuke and Mizuno, Izumi and Moran, James M. and Moriyama, Kotaro and Moscibrodzka, Monika and Musoke, Gibwa and Müller, Cornelia and Nagai, Hiroshi and Nagar, Neil M. and Nakamura, Masanori and Narayan, Ramesh and Narayanan, Gopal and Natarajan, Iniyan and Neri, Roberto and Ni, Chunchong and Noutsos, Aristeidis and Okino, Hiroki and Olivares, Héctor and Ortiz-León, Gisela N. and Oyama, Tomoaki and Palumbo, Daniel C. M. and Park, Jongho and Patel, Nimesh and Pen, Ue-Li and Piétu, Vincent and Plambeck, Richard and PopStefanija, Aleksandar and Porth, Oliver 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 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 Ryan, Benjamin R. and Rygl, Kazi L. J. and Sánchez, Salvador and Sánchez-Arguelles, David and Sasada, Mahito 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 Tazaki, Fumie 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 Tsuda, Shuichiro and van Bemmel, Ilse and van Langevelde, Huib Jan and van Rossum, Daniel R. and Wagner, Jan and Wardle, John and Ward-Thompson, Derek and Weintroub, Jonathan and Wex, Norbert and Wharton, Robert 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, Guangyao and Zhao, Shan-Shan and Zhu, Ziyan and Algaba, Juan-Carlos and Allardi, Alexander and Amestica, Rodrigo and Anczarski, Jadyn and Bach, Uwe and Baganoff, Frederick K. and Beaudoin, Christopher and Benson, Bradford A. and Berthold, Ryan and Blanchard, Jay M. and Blundell, Ray and Bustamente, Sandra and Cappallo, Roger and Castillo-Domínguez, Edgar and Chang, Chih-Cheng and Chang, Shu-Hao and Chang, Song-Chu and Chen, Chung-Chen and Chilson, Ryan and Chuter, Tim C. and Rosado, Rodrigo Córdova and Coulson, Iain M. and Crowley, Joseph and Derome, Mark and Dexter, Matthew and Dornbusch, Sven and Dudevoir, Kevin A. and Dzib, Sergio A. and Eckart, Andreas and Eckert, Chris and Erickson, Neal R. and Everett, Wendeline B. and Faber, Aaron and Farah, Joseph R. and Fath, Vernon and Folkers, Thomas W. and Forbes, David C. and Freund, Robert and Gale, David M. and Gao, Feng and Geertsema, Gertie and Graham, David A. and Greer, Christopher H. and Grosslein, Ronald and Gueth, Frédéric and Haggard, Daryl and Halverson, Nils W. and Han, Chih-Chiang and Han, Kuo-Chang and Hao, Jinchi and Hasegawa, Yutaka and Henning, Jason W. and Hernández-Gómez, Antonio and Herrero-Illana, Rubén and Heyminck, Stefan and Hirota, Akihiko and Hoge, James and Huang, Yau-De and Impellizzeri, C. M. Violette and Jiang, Homin and John, David and Kamble, Atish and Keisler, Ryan and Kimura, Kimihiro and Kono, Yusuke and Kubo, Derek and Kuroda, John and Lacasse, Richard and Laing, Robert A. and Leitch, Erik M. and Li, Chao-Te and Lin, Lupin C.-C. and Liu, Ching-Tang and Liu, Kuan-Yu and Lu, Li-Ming and Marson, Ralph G. and Martin-Cocher, Pierre L. and Massingill, Kyle D. and Matulonis, Callie and McColl, Martin P. and McWhirter, Stephen R. and Messias, Hugo and Meyer-Zhao, Zheng and Michalik, Daniel and Montaña, Alfredo and Montgomerie, William and Mora-Klein, Matias and Muders, Dirk and Nadolski, Andrew and Navarro, Santiago and Neilsen, Joseph and Nguyen, Chi H. and Nishioka, Hiroaki and Norton, Timothy and Nowak, Michael A. and Nystrom, George and Ogawa, Hideo and Oshiro, Peter and Oyama, Tomoaki and Parsons, Harriet and Peñalver, Juan and Phillips, Neil M. and Poirier, Michael and Pradel, Nicolas and Primiani, Rurik A. and Raffin, Philippe A. and Rahlin, Alexandra S. and Reiland, George and Risacher, Christopher and Ruiz, Ignacio and Sáez-Madaín, Alejandro F. and Sassella, Remi and Schellart, Pim and Shaw, Paul and Silva, Kevin M. and Shiokawa, Hotaka and Smith, David R. and Snow, William and Souccar, Kamal and Sousa, Don and Sridharan, Tirupati K. and Srinivasan, Ranjani and Stahm, William and Stark, Antony A. and Story, Kyle and Timmer, Sjoerd T. and Vertatschitsch, Laura and Walther, Craig and Wei, Ta-Shun and Whitehorn, Nathan and Whitney, Alan R. and Woody, David P. and Wouterloot, Jan G. A. and Wright, Melvin and Yamaguchi, Paul and Yu, Chen-Yu and Zeballos, Milagros and Zhang, Shuo and Ziurys, Lucy (2020) Event Horizon Telescope imaging of the archetypal blazar 3C 279 at an extreme 20 microarcsecond resolution. Astronomy and Astrophysics, 640 . Art. No. A69. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20200813-174837430

[img] PDF - Published Version
Creative Commons Attribution.

3661Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20200813-174837430

Abstract

3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique – global Very Long Baseline Interferometry (VLBI) at 1.3 mm (230 GHz) – to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variable γ-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array (ALMA), at an angular resolution of ∼20 μas (at a redshift of z = 0.536 this corresponds to ∼0.13 pc  ∼ 1700 Schwarzschild radii with a black hole mass MBH = 8 × 108 M⊙). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation. We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across different imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI “core”. This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet. We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 c and ∼20 c (∼1.3 and ∼1.7 μas day⁻¹, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3 mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≲10¹⁰ K, a magnitude or more lower than typical values seen at ≥7 mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/202037493DOIArticle
ORCID:
AuthorORCID
Kim, Jae-Young0000-0001-8229-7183
Bouman, Katherine L.0000-0003-0077-4367
Issaoun, Sara0000-0002-5297-921X
Janssen, Michael0000-0001-8685-6544
Azulay, Rebecca0000-0002-2200-5393
Byun, Do-Young0000-0003-1157-4109
Chatterjee, Shami0000-0002-2878-1502
Chatterjee, Koushik0000-0002-2825-3590
Cui, Yuzhu0000-0001-6311-4345
Deane, Roger0000-0003-1027-5043
Fraga-Encinas, Raquel0000-0002-5222-1361
Friberg, Per0000-0002-8010-8454
Jannuzi, Buell T.0000-0002-1578-6582
Kim, Junhan0000-0002-4274-9373
Kramer, Michael0000-0002-4175-2271
Lauer, Tod R.0000-0003-3234-7247
Lonsdale, Colin0000-0003-4062-4654
Matthews, Lynn D.0000-0002-3728-8082
Mizuno, Yosuke0000-0002-8131-6730
Müller, Cornelia0000-0002-2739-2994
Plambeck, Richard0000-0001-6765-9609
Pu, Hung-Yi0000-0001-9270-8812
Ramakrishnan, Venkatessh0000-0002-9248-086X
Rawlings, Mark G.0000-0002-6529-202X
Ruszczyk, Chet0000-0003-1191-9816
Tiede, Paul0000-0003-3826-5648
Trippe, Sascha0000-0003-0465-1559
Yoon, Doosoo0000-0001-8694-8166
Younsi, Ziri0000-0001-9283-1191
Castillo-Domínguez, Edgar0000-0002-8299-4023
Coulson, Iain M.0000-0002-7316-4626
Dornbusch, Sven0000-0003-3211-3352
Dzib, Sergio A.0000-0001-6010-6200
Eckert, Chris0000-0003-2496-0383
Farah, Joseph R.0000-0003-4914-5625
Han, Kuo-Chang0000-0002-0822-0273
Impellizzeri, C. M. Violette0000-0002-3443-2472
Leitch, Erik M.0000-0001-8553-9336
Massingill, Kyle D.0000-0002-0830-2033
Messias, Hugo0000-0002-2985-7994
Nadolski, Andrew0000-0001-9479-9957
Nguyen, Chi H.0000-0001-9368-3186
Parsons, Harriet0000-0002-6327-3423
Risacher, Christopher0000-0001-7162-4185
Smith, David R.0000-0003-0692-8582
Sousa, Don0000-0002-2625-2607
Wouterloot, Jan G. A.0000-0002-4694-6905
Zeballos, Milagros0000-0001-7737-2687
Additional Information:© 2020 J.-Y. Kim et al. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society. Received 13 January 2020; Accepted 3 March 2020; Published online 12 August 2020. The authors of the present paper 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 projects 1171506 and 3190878, BASAL AFB-170002, 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 Autónoma de México (DGAPA – UNAM, project IN112417); 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); 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); the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJ-SSW-SYS008, ZDBS-LY-SLH011); the Leverhulme Trust Early Career Research Fellowship; the Malaysian Fundamental Research Grant Scheme (FRGS, grant FRGS/1/2019/STG02/UM/02/6); 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-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 and 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 Russian Science Foundation (grant 17-12-01029); the Spanish Ministerio de Economía y Competitividad (grants PGC2018-098915-B-C21, 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 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; 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 (http://computeontario.ca), Calcul Quebec (http://www.calculquebec.ca) and Compute Canada (http://www.computecanada.ca). We thank the staff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.01154.V, ADS/JAO.ALMA#2016.1.01176.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 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). 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. This research has made use of data obtained with the Global Millimeter VLBI Array (GMVA), which consists of telescopes operated by the MPIfR, IRAM, Onsala, Metsahovi, Yebes, the Korean VLBI Network, the Green Bank Observatory and the Very Long Baseline Array (VLBA). The VLBA is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. The data were correlated at the correlator of the MPIfR in Bonn, Germany. This study makes use of 43 GHz VLBA data from the VLBA-BU Blazar Monitoring Program (VLBA-BU-BLAZAR; http://www.bu.edu/blazars/VLBAproject.html), funded by NASA through the Fermi Guest Investigator Program.
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
Academy of Finland274477
Academy of Finland284495
Academy of Finland312496
European Research Council (ERC)731016
Alexander von Humboldt StiftungUNSPECIFIED
Harvard UniversityUNSPECIFIED
John Templeton Foundation60477
China Scholarship CouncilUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)PIA ACT172033
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1171506
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3190878
BASAL-CATAAFB-170002
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)31140007
Consejo Nacional de Ciencia y Tecnología (CONACYT)104497
Consejo Nacional de Ciencia y Tecnología (CONACYT)275201
Consejo Nacional de Ciencia y Tecnología (CONACYT)279006
Consejo Nacional de Ciencia y Tecnología (CONACYT)281692
Delaney Family John A. Wheeler ChairUNSPECIFIED
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Dirección General de Asuntos del Personal Académico-Universidad Nacional Autónoma de MéxicoIN112417
European Research Council (ERC)610058
Generalitat ValencianaAPOSTD/2018/177
Generalitat ValencianaCIDEGENT/2018/021
Gordon and Betty Moore FoundationGBMF-3561
Gordon and Betty Moore FoundationGBMF-5278
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
International Max Planck Research School for Astronomy and AstrophysicsUNSPECIFIED
Jansky FellowshipUNSPECIFIED
National Radio Astronomy ObservatoryUNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17J08829
Chinese Academy of SciencesQYZDJ-SSW-SLH057
Chinese Academy of SciencesQYZDJ-SSW-SYS008
Chinese Academy of SciencesZDBS-LY-SLH011
Leverhulme TrustUNSPECIFIED
Malaysian Fundamental Research GrantFRGS/1/2019/STG02/UM/02/6
Max-Planck-Gesellschaft (MPG)UNSPECIFIED
Max Planck Partner GroupUNSPECIFIED
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)25120007
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
NASA80NSSC17K0649
NASA Hubble FellowshipHST-HF2-51431.001-A
NASANAS5-26555
National Institute of Natural Sciences (NINS)UNSPECIFIED
National Key Research and Development Program of China2016YFA0400704
National Key Research and Development Program of China2016YFA0400702
NSFAST-0096454
NSFAST-0352953
NSFAST-0521233
NSFAST-0705062
NSFAST-0905844
NSFAST-0922984
NSFAST-1126433
NSFAST-1140030
NSF Graduate Research FellowshipDGE-1144085
NSFAST-1207704
NSFAST-1207730
NSFAST-1207752
NSFMRI-1228509
NSFOPP-1248097
NSFAST-1310896
NSFAST-1312651
NSFAST-1337663
NSFAST-1440254
NSFAST-1555365
NSFAST-1715061
NSFAST-1615796
NSFAST-1716327
NSFOISE-1743747
NSFAST-1816420
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
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
National Youth Thousand Talents Program of ChinaUNSPECIFIED
National Research Foundation of KoreaNRF-2015H1A2A1033752
National Research Foundation of Korea2015-R1D1A1A01056807
National Research Foundation of KoreaNRF-2015H1D3A1066561
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.043.513
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)SPI 78-409
South African Radio Astronomy Observatory (SARAO)UNSPECIFIED
National Research Foundation (South Africa)UNSPECIFIED
Department of Science and Technology (South Africa)UNSPECIFIED
Onsala Space Observatory (OSO)UNSPECIFIED
Swedish Research Council2017-00648
Department of Innovation, Science and Economic Development (Canada)UNSPECIFIED
Ontario Ministry of Research, Innovation and ScienceUNSPECIFIED
Russian Science Foundation17-12-01029
Ministerio de Economía y Competitividad (MINECO)PGC2018-098915-B-C21
Ministerio de Economía y Competitividad (MINECO)AYA2016-80889-P
Severo OchoaSEV-2017-0709
Toray Science FoundationUNSPECIFIED
Department of Energy (DOE)89233218CNA000001
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)2012-iALMA
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)CUP C52I13000140001
European Research Council (ERC)730562 RadioNet
ALMA North America Development FundUNSPECIFIED
Academia SinicaUNSPECIFIED
NASATM6-17006X
Generalitat ValencianaCIDEGENT/2018/021
NSFACI-1548562
NSFDBI-0735191
NSFDBI-1265383
NSFDBI-1743442
NSFTG-AST170024
NSFTG-AST080026N
NSFAST-170028
Compute OntarioUNSPECIFIED
Calcul QuebecUNSPECIFIED
Compute CanadaUNSPECIFIED
Smithsonian InstitutionUNSPECIFIED
Ministry of Finance (China)UNSPECIFIED
National Key Research and Development Program of China2017YFA0402700
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Instituto Geográfico Nacional (IGN)UNSPECIFIED
State of ArizonaUNSPECIFIED
NSFPLR-1248097
NSFPHY-1125897
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF 947
Subject Keywords:galaxies: active – galaxies: jets – galaxies: individual: 3C 279 – techniques: interferometric
Record Number:CaltechAUTHORS:20200813-174837430
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200813-174837430
Official Citation:Event Horizon Telescope imaging of the archetypal blazar 3C 279 at an extreme 20 microarcsecond resolution. Jae-Young Kim, et. al., and The Event Horizon Telescope Collaboration. A&A, 640 (2020) A69. DOI: https://doi.org/10.1051/0004-6361/202037493
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104960
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:14 Aug 2020 16:33
Last Modified:30 Sep 2020 17:42

Repository Staff Only: item control page