Magnetic launching of black hole jets in Perseus A

Radio image of the galaxy 3C 84 showing the black hole jet in the centre at different spatial scales (denoted by the horizontal bar below each image), with the EHT image on the right exhibiting the most details.
(c) Georgios Filippos Paraschos (MPIfR)

The Event Horizon Telescope collaboration, including scientists from the Max Planck Institute for Radio Astronomy in Bonn, Germany, has recently resolved the jet base of an evolving jet of plasma at ultra-high angular resolution. The international team of scientists used the Earth-size telescope to probe the magnetic structure in the nucleus of the radio galaxy 3C 84 (Perseus A), one of the closest active supermassive black holes in our cosmic neighbourhood. These novel results provide new insight into how jets are launched, revealing that in this cosmic tug of war, the magnetic fields overpower gravity.

The strong radio source 3C 84 or Perseus A corresponds to NGC 1275, the central galaxy in the Perseus cluster at a distance of 230 million light years. It hosts a relatively nearby active galactic nucleus, allowing for a detailed investigation of the central source at high resolution with the Event Horizon Telescope (EHT).

“Besides providing first images of black holes, the EHT is supremely suitable to observe astrophysical jets of plasma and their interplay with strong magnetic fields,” says Georgios Filippos Paraschos, researcher at the Max Planck Institute for Radio Astronomy (MPIfR), who led the project. “Our new findings provide new evidence that an ordered magnetic field extends throughout the heated gas enveloping the black hole.” The groundbreaking observations made by the EHT enable the scientists to address enduring questions regarding the process by which black holes accrete matter and eject powerful jets, reaching distances beyond their host galaxies.

In recent years, the Event horizon Telescope has unveiled images showing the direction of the light oscillation around the M 87* black hole. This property of the emitted light, called linear polarisation, provides clues about the underlying magnetic field. In particular, strong linear polarisation, as found in the present study, hints at a strong, well-ordered magnetic field in the 3C 84 black hole vicinity. Notably, such powerful magnetic fields are thought to be the driving force behind the launching of such plasma jets, consisting of matter that was not consumed by the black hole.

“The radio galaxy 3C 84 is particularly interesting for the challenges it presents in detecting and accurately measuring the polarisation of light near its black hole,” notes Jae-Young Kim, associate professor for astrophysics at Kyungpook National University (Daegu, South Korea), also affiliated with the MPIfR. “The Event Horizon Telescope’s exceptional capability to penetrate the dense, interstellar gas marks a groundbreaking advancement for precisely observing the vicinity of black holes.” Such high-precision observations pave the way for discovering and studying other supermassive black holes that have remained hidden and elusive to previous observational technologies.

Their findings also shed light on the way mass is accreted onto the supermassive black hole, which is via advection. The infalling matter is thought to form a strongly magnetised, so-called magnetically arrested disc. In this scenario, the magnetic field lines within the accretion disc become tightly wound and twisted, preventing the efficient release of magnetic energy. Furthermore, our study implies that the 3C 84 black hole is rapidly rotating, thus favouring an association between jet launching and large black hole spins.

“Why are black holes so good at producing powerful jets? This is one of the most fascinating questions in astrophysics,” says Maciek Wielgus, a researcher at the MPIfR. “We expect that general relativistic effects occurring just above the black hole’s event horizon may be the key to answer this question. Such high resolution observations are finally paving the way towards an observational verification.”

These exciting new results have been made possible by utilising the technique of very-long-baseline interferometry or VLBI, in which a number of telescopes observe the same object in the sky and then combine the collected signals to produce an image. This way they act as a virtual telescope of the size as large as the diameter of the Earth.

“We are extremely excited because these results are a significant step towards understanding galaxies such as 3C 84. Together with our international partners, we are striving to improve the capabilities of the Event Horizon Telescope, to enable even more detailed insight on jet formation around black holes,” concludes Anton Zensus, Director at the MPIfR and head of it’s Radio Astronomy / VLBI research department.

Additional Information

The EHT collaboration involves more than 300 researchers from Africa, Asia, Europe, and North and South America. The international collaboration is working to capture the most detailed black hole images ever obtained by creating a virtual Earth-sized telescope. Supported by considerable international investment, the EHT links existing telescopes using novel systems, creating a fundamentally new instrument with the highest angular resolving power that has yet been achieved.

Antennas of the Event Horizon Telescope used in April 2017 (clockwise from upper left): APEX, Pico Veleta, LMT, JCMT, ALMA, SMT (Heinrich Hertz Telescope), SMA, SPT.
Antennas of the Event Horizon Telescope used in April 2017 (clockwise from upper left): APEX, Pico Veleta, LMT, JCMT, ALMA, SMT (Heinrich Hertz Telescope), SMA, SPT. (c) APEX, IRAM, G. Narayanan, J. McMahon, JCMT/JAC, S. Hostler, D. Harvey, ESO/C. Malin

The individual telescopes involved are: ALMA, APEX, the IRAM 30-meter Telescope, the IRAM NOEMA Observatory, the James Clerk Maxwell Telescope (JCMT), the Large Millimeter Telescope (LMT), the Submillimeter Array (SMA), the Submillimeter Telescope (SMT), the South Pole Telescope (SPT), and the Kitt Peak Telescope.

The EHT consortium consists of 13 stakeholder institutes: the Academia Sinica Institute of Astronomy and Astrophysics, the University of Arizona, the University of Chicago, the East Asian Observatory, Goethe-Universität Frankfurt, Institut de Radioastronomie Millimétrique, Large Millimeter Telescope, Max Planck Institute for Radio Astronomy, MIT Haystack Observatory, National Astronomical Observatory of Japan, Perimeter Institute for Theoretical Physics, Radboud University, and the Smithsonian Astrophysical Observatory.

The following scientists affiliated to the MPIfR are co-authors of the publication: Georgios Filippos Paraschos, Jae-Young Kim, Maciek Wielgus, Jan Röder, Thomas P. Krichbaum, Eduardo Ros, Ioannis Myserlis, Efthalia Traianou, J. Anton Zensus, Michael Janssen, Walter Alef, Rebecca Azulay, Uwe Bach, Anne-Kathrin Baczko, Silke Britzen, Gregory Desvignes, Sergio A. Dzib, Ralph P. Eatough, Christian M. Fromm, Ramesh Karuppusamy, Dong-Jin Kim, Joana A. Kramer, Michael Kramer, Mikhail Lisakov, Jun Liu, Kuo Liu, RuSen Lu, Andrei P. Lobanov, Nicholas R. MacDonald, Nichola Marchilli, Karl M. Menten, Cornelia Müller, Hendrik Müller, Aristeidis Noutsos, Gisela N. Ortiz-León, Felix M. Pötzl, Helge Rottmann, Alan L. Roy, Tuomas Savolainen, Lijing Shao, Pablo Torne, Jan Wagner, Robert Wharton, and Gunther Witzel.

Wissenschaftliche Ansprechpartner:

Dr. Georgios Filippos Paraschos
Max Planck Institute for Radio Astronomy, Bonn
Fon: +49 228 525-365
E-mail: gfparaschos@mpifr-bonn.mpg.de

Dr. Maciek Wielgus
Max Planck Institute for Radio Astronomy, Bonn
Fon: +49 228 525-424
E-mail: mwielgus@mpifr-bonn.mpg.de

Prof. Dr. Eduardo Ros
European GMVA Scheduler
Max Planck Institute for Radio Astronomy, Bonn
Tel. +49 228 525-125
ros@mpifr-bonn.mpg.de

Originalpublikation:

G.F. Paraschos et al.: Ordered magnetic fields around the 3C 84 central black hole, Astronomy & Astrophysics, February 01, 2024, DOI: 10.1051/0004-6361/202348308

https://www.aanda.org/10.1051/0004-6361/202348308

Weitere Informationen:

https://www.mpifr-bonn.mpg.de/pressreleases/2024/4

Media Contact

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Max-Planck-Institut für Radioastronomie

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