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Cui Y, Hada K, Kawashima T, Kino M, Lin W, Mizuno Y, Ro H, Honma M, Yi K, Yu J, Park J, Jiang W, Shen Z, Kravchenko E, Algaba JC, Cheng X, Cho I, Giovannini G, Giroletti M, Jung T, Lu RS, Niinuma K, Oh J, Ohsuga K, Sawada-Satoh S, Sohn BW, Takahashi HR, Takamura M, Tazaki F, Trippe S, Wajima K, Akiyama K, An T, Asada K, Buttaccio S, Byun DY, Cui L, Hagiwara Y, Hirota T, Hodgson J, Kawaguchi N, Kim JY, Lee SS, Lee JW, Lee JA, Maccaferri G, Melis A, Melnikov A, Migoni C, Oh SJ, Sugiyama K, Wang X, Zhang Y, Chen Z, Hwang JY, Jung DK, Kim HR, Kim JS, Kobayashi H, Li B, Li G, Li X, Liu Z, Liu Q, Liu X, Oh CS, Oyama T, Roh DG, Wang J, Wang N, Wang S, Xia B, Yan H, Yeom JH, Yonekura Y, Yuan J, Zhang H, Zhao R, Zhong W. Precessing jet nozzle connecting to a spinning black hole in M87. Nature 2023; 621:711-715. [PMID: 37758892 DOI: 10.1038/s41586-023-06479-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/24/2023] [Accepted: 07/25/2023] [Indexed: 09/29/2023]
Abstract
The nearby radio galaxy M87 offers a unique opportunity to explore the connections between the central supermassive black hole and relativistic jets. Previous studies of the inner region of M87 revealed a wide opening angle for the jet originating near the black hole1-4. The Event Horizon Telescope resolved the central radio source and found an asymmetric ring structure consistent with expectations from general relativity5. With a baseline of 17 years of observations, there was a shift in the jet's transverse position, possibly arising from an 8- to 10-year quasi-periodicity3. However, the origin of this sideways shift remains unclear. Here we report an analysis of radio observations over 22 years that suggests a period of about 11 years for the variation in the position angle of the jet. We infer that we are seeing a spinning black hole that induces the Lense-Thirring precession of a misaligned accretion disk. Similar jet precession may commonly occur in other active galactic nuclei but has been challenging to detect owing to the small magnitude and long period of the variation.
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Affiliation(s)
- Yuzhu Cui
- Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China.
- Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai, China.
- Astronomical Science Program, The Graduate University for Advanced Studies, Mitaka, Japan.
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan.
| | - Kazuhiro Hada
- Astronomical Science Program, The Graduate University for Advanced Studies, Mitaka, Japan
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
| | - Tomohisa Kawashima
- Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa, Japan
| | - Motoki Kino
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
- Kogakuin University of Technology & Engineering, Academic Support Center, Hachioji, Japan
| | - Weikang Lin
- South-Western Institute For Astronomy Research, Yunnan University, Kunming, China
| | - Yosuke Mizuno
- Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai, China
- School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, China
- Institut für Theoretische Physik, Goethe-Universität Frankfurt, Frankfurt, Germany
| | - Hyunwook Ro
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- Department of Astronomy, Yonsei University, Seodaemun-gu, Republic of Korea
| | - Mareki Honma
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
- Department of Astronomy, Graduate School of Science, The University of Tokyo, Bunkyo, Japan
| | - Kunwoo Yi
- Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Republic of Korea
| | - Jintao Yu
- Department of Intelligence, Air Force Early Warning Academy, Wuhan, China
| | - Jongho Park
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- Institute of Astronomy and Astrophysics, Academia Sinica, Hilo, HI, USA
| | - Wu Jiang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Zhiqiang Shen
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | | | - Juan-Carlos Algaba
- Department of Physics, Faculty of Science, Universiti Malaya, Kuala Lumpur, Malaysia
| | - Xiaopeng Cheng
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Ilje Cho
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- Instituto de Astrofísica de Andalucía - CSIC, Glorieta de la Astronomía s/n, Granada, Spain
| | - Gabriele Giovannini
- DIFA Bologna University, Bologna, Italy
- INAF-Istituto di Radioastronomia, Bologna, Italy
| | | | - Taehyun Jung
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- University of Science and Technology, Yuseong-gu, Republic of Korea
| | - Ru-Sen Lu
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
- Max-Planck-Institut für Radioastronomie, Bonn, Germany
| | - Kotaro Niinuma
- Graduate School of Sciences and Technology for Innovation, Yamaguchi University, Yamaguchi, Japan
- The Research Institute for Time Studies, Yamaguchi University, Yamaguchi, Japan
| | - Junghwan Oh
- Joint Institute for VLBI ERIC, Dwingeloo, the Netherlands
| | - Ken Ohsuga
- Center for Computational Sciences, University of Tsukuba, Tsukuba, Japan
| | | | - Bong Won Sohn
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- Department of Astronomy, Yonsei University, Seodaemun-gu, Republic of Korea
- University of Science and Technology, Yuseong-gu, Republic of Korea
| | - Hiroyuki R Takahashi
- Department of Natural Sciences, Faculty of Arts and Sciences, Komazawa University, Setagaya, Japan
| | - Mieko Takamura
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
- Department of Astronomy, Graduate School of Science, The University of Tokyo, Bunkyo, Japan
| | - Fumie Tazaki
- Tokyo Electron Technology Solutions Limited, Oshu City, Japan
| | - Sascha Trippe
- Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Republic of Korea
- SNU Astronomy Research Center, Seoul National University, Gwanak-gu, Republic of Korea
| | - Kiyoaki Wajima
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- University of Science and Technology, Yuseong-gu, Republic of Korea
| | - Kazunori Akiyama
- National Radio Astronomy Observatory, Charlottesville, VA, USA
- Massachusetts Institute of Technology Haystack Observatory, Westford, MA, USA
- Black Hole Initiative at Harvard University, Cambridge, MA, USA
| | - Tao An
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - Keiichi Asada
- Institute of Astronomy and Astrophysics, Academia Sinica, Hilo, HI, USA
| | | | - Do-Young Byun
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- University of Science and Technology, Yuseong-gu, Republic of Korea
| | - Lang Cui
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | | | - Tomoya Hirota
- Astronomical Science Program, The Graduate University for Advanced Studies, Mitaka, Japan
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
| | - Jeffrey Hodgson
- Department of Physics and Astronomy, Sejong University, Gwangjin-gu, Republic of Korea
| | - Noriyuki Kawaguchi
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
| | - Jae-Young Kim
- Max-Planck-Institut für Radioastronomie, Bonn, Germany
- Department of Astronomy and Atmospheric Sciences, Kyungpook National University, Daegu, Republic of Korea
| | - Sang-Sung Lee
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- University of Science and Technology, Yuseong-gu, Republic of Korea
| | - Jee Won Lee
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Jeong Ae Lee
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | | | - Andrea Melis
- INAF - Osservatorio Astronomico di Cagliari, Selargius, CA, Italy
| | - Alexey Melnikov
- Institute of Applied Astronomy, Russian Academy of Sciences, St. Petersburg, Russia
| | - Carlo Migoni
- INAF - Osservatorio Astronomico di Cagliari, Selargius, CA, Italy
| | - Se-Jin Oh
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Koichiro Sugiyama
- National Astronomical Research Institute of Thailand (Public Organization), Chiangmai, Thailand
| | - Xuezheng Wang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - Yingkang Zhang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - Zhong Chen
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Ju-Yeon Hwang
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Dong-Kyu Jung
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Hyo-Ryoung Kim
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Jeong-Sook Kim
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Hideyuki Kobayashi
- Astronomical Science Program, The Graduate University for Advanced Studies, Mitaka, Japan
| | - Bin Li
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Guanghui Li
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Xiaofei Li
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Zhiyong Liu
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Qinghui Liu
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Xiang Liu
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Chung-Sik Oh
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Tomoaki Oyama
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu, Japan
| | - Duk-Gyoo Roh
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Jinqing Wang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Na Wang
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Shiqiang Wang
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Bo Xia
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - Hao Yan
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Jae-Hwan Yeom
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | | | - Jianping Yuan
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Hua Zhang
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Rongbing Zhao
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
| | - Weiye Zhong
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
- Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences, Beijing, China
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Abstract
Accreting supermassive black holes in active galactic nuclei (AGN) produce powerful relativistic jets that shine from radio to GeV/TeV γ-rays. Over the past decade, AGN jets have extensively been studied in various energy bands and our knowledge about the broadband emission and rapid flares are now significantly updated. Meanwhile, the progress of magnetohydrodynamic simulations with a rotating black hole have greatly improved our theoretical understanding of powerful jet production. Nevertheless, it is still challenging to observationally resolve such flaring sites or jet formation regions since the relevant spatial scales are tiny. Observations with very long baseline interferometry (VLBI) are currently the only way to directly access such compact scales. Here we overview some recent progress of VLBI studies of AGN jets. As represented by the successful black hole shadow imaging with the Event Horizon Telescope, the recent rapid expansion of VLBI capability is remarkable. The last decade has also seen a variety of advances thanks to the advent of RadioAstron, GMVA, new VLBI facilities in East Asia as well as to the continued upgrade of VLBA. These instruments have resolved the innermost regions of relativistic jets for a number of objects covering a variety of jetted AGN classes (radio galaxies, blazars, and narrow-line Seyfert 1 galaxies), and the accumulated results start to establish some concrete (and likely universal) picture on the collimation, acceleration, recollimation shocks, magnetic field topology, and the connection to high-energy flares in the innermost part of AGN jets.
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Abstract
M87 is one of the best available source for studying the AGN jet-launching region. To enrich our knowledge of this region, with quasi-simultaneous observations using VLBA at 22, 43 and 86 GHz, we capture the images of the radio jet in M87 on a scale within several thousand R s . Based on the images, we analyze the transverse jet structure and obtain the most accurate spectral-index maps of the jet in M87 so far, then for the first time, we compare the results of the two analyses and find a spatial association between the jet collimations and the local enhancement of the density of external medium in the jet-launching region. We also find the external medium is not uniform, and greatly contributes to the free-free absorption in this region. In addition, we find for the jet in M87, its temporal morphology in the launching region may be largely affected by the local, short-lived kink instability growing in itself.
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First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab0ec7] [Citation(s) in RCA: 1437] [Impact Index Per Article: 287.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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5
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6
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First M87 Event Horizon Telescope Results. IV. Imaging the Central Supermassive Black Hole. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab0e85] [Citation(s) in RCA: 517] [Impact Index Per Article: 103.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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7
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First M87 Event Horizon Telescope Results. VI. The Shadow and Mass of the Central Black Hole. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab1141] [Citation(s) in RCA: 588] [Impact Index Per Article: 117.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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8
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Abstract
Over the past decade, our knowledge of the γ -ray sky has been revolutionized by ground- and space-based observatories by detecting photons up to several hundreds of tera-electron volt (TeV) energies. A major population of the γ -ray bright objects are active galactic nuclei (AGN) with their relativistic jets pointed along our line-of-sight. Gamma-ray emission is also detected from nearby misaligned AGN such as radio galaxies. While the TeV-detected radio galaxies ( T e V R a d ) only form a small fraction of the γ -ray detected AGN, their multi-wavelength study offers a unique opportunity to probe and pinpoint the high-energy emission processes and sites. Even in the absence of substantial Doppler beaming T e V R a d are extremely bright objects in the TeV sky (luminosities detected up to 10 45 erg s − 1 ), and exhibit flux variations on timescales shorter than the event-horizon scales (flux doubling timescale less than 5 min). Thanks to the recent advancement in the imaging capabilities of high-resolution radio interferometry (millimeter very long baseline interferometry, mm-VLBI), one can probe the scales down to less than 10 gravitational radii in T e V R a d , making it possible not only to test jet launching models but also to pinpoint the high-energy emission sites and to unravel the emission mechanisms. This review provides an overview of the high-energy observations of T e V R a d with a focus on the emitting sites and radiation processes. Some recent approaches in simulations are also sketched. Observations by the near-future facilities like Cherenkov Telescope Array, short millimeter-VLBI, and high-energy polarimetry instruments will be crucial for discriminating the competing high-energy emission models.
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9
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Pausch R, Bussmann M, Huebl A, Schramm U, Steiniger K, Widera R, Debus A. Identifying the linear phase of the relativistic Kelvin-Helmholtz instability and measuring its growth rate via radiation. Phys Rev E 2018; 96:013316. [PMID: 29347084 DOI: 10.1103/physreve.96.013316] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/08/2016] [Indexed: 11/07/2022]
Abstract
For the relativistic Kelvin-Helmholtz instability (KHI), which occurs at shear interfaces between two plasma streams, we report results on the polarized radiation over all observation directions and frequencies emitted by the plasma electrons from ab initio kinetic simulations. We find the polarization of the radiation to provide a clear signature for distinguishing the linear phase of the KHI from its other phases. During the linear phase, we predict the growth rate of the KHI radiation power to match the growth rate of the KHI to a high degree. Our predictions are based on a model of the vortex dynamics, which describes the electron motion in the vicinity of the shear interface between the two streams. Albeit the complex and turbulent dynamics happening in the shear region, we find excellent agreement between our model and large-scale particle-in-cell simulations. Our findings pave the way for identifying the KHI linear regime and for measuring its growth rate in astrophysical jets observable on earth as well as in laboratory plasmas.
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Affiliation(s)
- R Pausch
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany.,Technische Universität Dresden, 01062 Dresden, Germany
| | - M Bussmann
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany
| | - A Huebl
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany.,Technische Universität Dresden, 01062 Dresden, Germany
| | - U Schramm
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany.,Technische Universität Dresden, 01062 Dresden, Germany
| | - K Steiniger
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany.,Technische Universität Dresden, 01062 Dresden, Germany
| | - R Widera
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany
| | - A Debus
- Helmholtz-Zentrum Dresden - Rossendorf, Bautzner Landstraße 400, 01328 Dresden, Germany
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10
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The Power of (Near) Simultaneous Multi-Frequency Observations for mm-VLBI and Astrometry. GALAXIES 2017. [DOI: 10.3390/galaxies5010009] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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11
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12
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13
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Resolving the Base of the Relativistic Jet in M87 at 6Rsch Resolution with Global mm-VLBI. GALAXIES 2016. [DOI: 10.3390/galaxies4040039] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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14
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15
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HIGH-SENSITIVITY 86 GHz (3.5 mm) VLBI OBSERVATIONS OF M87: DEEP IMAGING OF THE JET BASE AT A RESOLUTION OF 10 SCHWARZSCHILD RADII. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/817/2/131] [Citation(s) in RCA: 110] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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16
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Kino M, Takahara F, Hada K, Akiyama K, Nagai H, Sohn BW. MAGNETIZATION DEGREE AT THE JET BASE OF M87 DERIVED FROM THE EVENT HORIZON TELESCOPE DATA: TESTING THE MAGNETICALLY DRIVEN JET PARADIGM. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/803/1/30] [Citation(s) in RCA: 49] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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17
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Zamaninasab M, Clausen-Brown E, Savolainen T, Tchekhovskoy A. Dynamically important magnetic fields near accreting supermassive black holes. Nature 2014; 510:126-8. [PMID: 24899311 DOI: 10.1038/nature13399] [Citation(s) in RCA: 172] [Impact Index Per Article: 17.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/13/2014] [Accepted: 04/14/2014] [Indexed: 11/09/2022]
Abstract
Accreting supermassive black holes at the centres of active galaxies often produce 'jets'--collimated bipolar outflows of relativistic particles. Magnetic fields probably play a critical role in jet formation and in accretion disk physics. A dynamically important magnetic field was recently found near the Galactic Centre black hole. If this is common and if the field continues to near the black hole event horizon, disk structures will be affected, invalidating assumptions made in standard models. Here we report that jet magnetic field and accretion disk luminosity are tightly correlated over seven orders of magnitude for a sample of 76 radio-loud active galaxies. We conclude that the jet-launching regions of these radio-loud galaxies are threaded by dynamically important fields, which will affect the disk properties. These fields obstruct gas infall, compress the accretion disk vertically, slow down the disk rotation by carrying away its angular momentum in an outflow and determine the directionality of jets.
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Affiliation(s)
- M Zamaninasab
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
| | - E Clausen-Brown
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
| | - T Savolainen
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
| | - A Tchekhovskoy
- 1] Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, California 94720, USA [2] Department of Astronomy and Theoretical Astrophysics Center, University of California, Berkeley, California 94720-3411, USA
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18
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Deane RP, Paragi Z, Jarvis MJ, Coriat M, Bernardi G, Fender RP, Frey S, Heywood I, Klöckner HR, Grainge K, Rumsey C. A close-pair binary in a distant triple supermassive black hole system. Nature 2014; 511:57-60. [PMID: 24990745 DOI: 10.1038/nature13454] [Citation(s) in RCA: 80] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/25/2014] [Accepted: 05/01/2014] [Indexed: 11/09/2022]
Abstract
Galaxies are believed to evolve through merging, which should lead to some hosting multiple supermassive black holes. There are four known triple black hole systems, with the closest black hole pair being 2.4 kiloparsecs apart (the third component in this system is at 3 kiloparsecs), which is far from the gravitational sphere of influence (about 100 parsecs for a black hole with mass one billion times that of the Sun). Previous searches for compact black hole systems concluded that they were rare, with the tightest binary system having a separation of 7 parsecs (ref. 10). Here we report observations of a triple black hole system at redshift z = 0.39, with the closest pair separated by about 140 parsecs and significantly more distant from Earth than any other known binary of comparable orbital separation. The effect of the tight pair is to introduce a rotationally symmetric helical modulation on the structure of the large-scale radio jets, which provides a useful way to search for other tight pairs without needing extremely high resolution observations. As we found this tight pair after searching only six galaxies, we conclude that tight pairs are more common than hitherto believed, which is an important observational constraint for low-frequency gravitational wave experiments.
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Affiliation(s)
- R P Deane
- 1] Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Rondebosch, 7701, Cape Town, South Africa [2] Square Kilometre Array South Africa, Pinelands, 7405, Cape Town, South Africa
| | - Z Paragi
- Joint Institute for VLBI in Europe, 7990 AA, Dwingeloo, The Netherlands
| | - M J Jarvis
- 1] Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UK [2] Physics Department, University of the Western Cape, Belville, 7535, South Africa
| | - M Coriat
- 1] Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Rondebosch, 7701, Cape Town, South Africa [2] Square Kilometre Array South Africa, Pinelands, 7405, Cape Town, South Africa
| | - G Bernardi
- 1] Square Kilometre Array South Africa, Pinelands, 7405, Cape Town, South Africa [2] Centre for Radio Astronomy Techniques and Technologies, Department of Physics and Electronics, Rhodes University, Grahamstown, 6140, South Africa [3] Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA
| | - R P Fender
- Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UK
| | - S Frey
- Satellite Geodetic Observatory, Institute of Geodesy, Cartography and Remote Sensing, H-1592, Budapest, Hungary
| | - I Heywood
- 1] Centre for Radio Astronomy Techniques and Technologies, Department of Physics and Electronics, Rhodes University, Grahamstown, 6140, South Africa [2] Australia Telescope National Facility, CSIRO Astronomy and Space Science, Epping, New South Wales 1710, Australia
| | - H-R Klöckner
- Max-Planck-Institut für Radioastronomie, D-53121 Bonn, Germany
| | - K Grainge
- Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, UK
| | - C Rumsey
- Astrophysics Group, Cavendish Laboratory, University of Cambridge, Cambridge, UK
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19
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Doi A, Hada K, Nagai H, Kino M, Honma M, Akiyama K, Oyama T, Kono Y. ALMA Continuum Spectrum of the M87 Nucleus. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136108008] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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20
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Haga T, Doi A, Murata Y, Sudou H, Kameno S, Hada K, Nagai H. The core shift measurements for two-sided jets affected by Free-Free absorption using VLBA. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136108004] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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21
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McKinney JC, Tchekhovskoy A, Blandford RD. Alignment of magnetized accretion disks and relativistic jets with spinning black holes. Science 2013; 339:49-52. [PMID: 23160958 DOI: 10.1126/science.1230811] [Citation(s) in RCA: 129] [Impact Index Per Article: 11.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Accreting black holes (BHs) produce intense radiation and powerful relativistic jets, which are affected by the BH's spin magnitude and direction. Although thin disks might align with the BH spin axis via the Bardeen-Petterson effect, this does not apply to jet systems with thick disks. We used fully three-dimensional general relativistic magnetohydrodynamical simulations to study accreting BHs with various spin vectors and disk thicknesses and with magnetic flux reaching saturation. Our simulations reveal a "magneto-spin alignment" mechanism that causes magnetized disks and jets to align with the BH spin near BHs and to reorient with the outer disk farther away. This mechanism has implications for the evolution of BH mass and spin, BH feedback on host galaxies, and resolved BH images for the accreting BHs in SgrA* and M87.
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Affiliation(s)
- Jonathan C McKinney
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94309, USA.
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Kino M, Takahara F, Hada K, Doi A. Energy densities of magnetic field and relativistic electrons at the innermost region of the M87 jet. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136101009] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
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Doeleman SS, Fish VL, Schenck DE, Beaudoin C, Blundell R, Bower GC, Broderick AE, Chamberlin R, Freund R, Friberg P, Gurwell MA, Ho PTP, Honma M, Inoue M, Krichbaum TP, Lamb J, Loeb A, Lonsdale C, Marrone DP, Moran JM, Oyama T, Plambeck R, Primiani RA, Rogers AEE, Smythe DL, SooHoo J, Strittmatter P, Tilanus RPJ, Titus M, Weintroub J, Wright M, Young KH, Ziurys LM. Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87. Science 2012; 338:355-8. [DOI: 10.1126/science.1224768] [Citation(s) in RCA: 314] [Impact Index Per Article: 26.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Sheperd S. Doeleman
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Vincent L. Fish
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - David E. Schenck
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | | | - Ray Blundell
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Geoffrey C. Bower
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Avery E. Broderick
- Perimeter Institute, 31 Caroline Street, North Waterloo, Ontario N2L 2Y5, Canada
- Department of Physics and Astronomy, University of Waterloo, 200 University Avenue West, Waterloo, Ontario N2l 3G1, Canada
| | - Richard Chamberlin
- Caltech Submillimeter Observatory, 111 Nowelo Street, Hilo, HI 96720, USA
| | - Robert Freund
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - Per Friberg
- James Clerk Maxwell Telescope, Joint Astronomy Centre, 660 North A'ohoku Place University Park, Hilo, HI 96720, USA
| | - Mark A. Gurwell
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Paul T. P. Ho
- Academia Sinica Institute for Astronomy and Astrophysics, 11F Astronomy-Mathematics Building, National Taiwan University, No. 1, Roosevelt Road, Section 4 Taipei 10617, Taiwan, R.O.C
| | - Mareki Honma
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
- The Graduate University for Advanced Studies, Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Makoto Inoue
- Academia Sinica Institute for Astronomy and Astrophysics, 11F Astronomy-Mathematics Building, National Taiwan University, No. 1, Roosevelt Road, Section 4 Taipei 10617, Taiwan, R.O.C
| | - Thomas P. Krichbaum
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
| | - James Lamb
- Owens Valley Radio Observatory, California Institute of Technology, 100 Leighton Lane, Big Pine, CA 93513–0968, USA
| | - Abraham Loeb
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Colin Lonsdale
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Daniel P. Marrone
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - James M. Moran
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Tomoaki Oyama
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Richard Plambeck
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Rurik A. Primiani
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | | | | | - Jason SooHoo
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Peter Strittmatter
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - Remo P. J. Tilanus
- James Clerk Maxwell Telescope, Joint Astronomy Centre, 660 North A'ohoku Place University Park, Hilo, HI 96720, USA
- Netherlands Organisation for Scientific Research, Laan van Nieuw Oost-Indie 300, NL2509 AC The Hague, Netherlands
| | - Michael Titus
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Jonathan Weintroub
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Melvyn Wright
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Ken H. Young
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Lucy M. Ziurys
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
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Erratum: An origin of the radio jet in M87 at the location of the central black hole. Nature 2012. [DOI: 10.1038/nature11425] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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