Supermassive black holes (SMBHs) are millions to billions of times heavier than the Sun and lurk in the centres of almost all massive galaxies. In our cosmic neighbourhood, most of these galactic SMBHs are inactive. However, some are extremely active, releasing enormous amounts of energy across the electromagnetic spectrum as matter falls into them under gravity1–3. Some spectacular manifestations of active SMBHs are radio galaxies — galaxies that eject two powerful, highly collimated jets of matter that emit radio waves. These radio jets are thought to be launched, focused and shaped by magnetic fields4–6, but direct evidence of this process is limited (see go.nature.com/3xvingm). Now, in a paper in Nature, Chibueze et al.7 report the observation of an interaction between such radio jets and magnetic fields in a galaxy cluster.
In a radio galaxy, much of the observed radiation is produced by electrons that are ejected in the vicinity of the galaxy’s SMBH at speeds close to that of light. Magnetic fields in the surrounding gas cause these particles to follow circular paths and, in doing so, to emit radio waves. Such fields also hold the particles together and focus them into two narrow jets. If left undisturbed (for example, when located outside galaxy clusters), these radio jets typically extend up to hundreds of thousands of parsecs before dissipating (1 parsec is about 3 light years). In some rare cases, they can even stretch across millions of parsecs8 — roughly 100 times the size of the Milky Way. Consequently, these jets are extremely sensitive probes of the environment near their host galaxies.
Chibueze and colleagues obtained high-resolution images of the radio galaxy MRC 0600‑399 (and a nearby radio galaxy) in the galaxy cluster Abell 3376 using the MeerKAT radio telescope in South Africa. MeerKAT consists of 64 antennas working collectively, and is one of the most sensitive radio telescopes in the world. The images show that the radio jets of MRC 0600‑399 bend sharply by almost 90° (Fig. 1), as seen previously9. They also reveal diffuse regions of radio emission on both sides of the jet-deflection points, referred to as double-scythe structures. The authors used state-of-the-art computer simulations to demonstrate that the bent jets and double-scythe structures can be explained if the jets travel at supersonic speed and strike a curved layer of strong, ordered magnetic fields that they cannot penetrate.
The origin of this strong magnetic layer is connected to ongoing cluster-building processes. Radio and X-ray observations of the cluster Abell 3376 have revealed a pair of giant arcs that trace radio emission from charged particles energized in powerful shock waves at the cluster’s outskirts9 (see Fig. 1a of the paper7). These shock waves are caused by matter (comprising galaxies and cold gas) falling into the cluster under gravity and releasing energy through violent collisions and mergers.
X-ray images of Abell 3376 show an odd, comet-like structure consisting of a cold gas cloud, which encompasses both MRC 0600‑399 and its nearby radio galaxy, and a long gas tail9 (see Fig. 1a of the paper7). Chibueze et al. propose that the gas cloud was ejected from the centre of Abell 3376 at supersonic speed, and that the pressure of the hot gas in the cluster on this fast-moving cloud produces the gas tail. They also suggest that this pressure causes the previously mentioned strong magnetic layer to drape around the boundary of the gas cloud, known as the cold front10 (Fig. 1). Without this protective magnetic layer, the cloud would evaporate rapidly, and the cold front would not form11,12.
If the authors’ interpretation is correct, it is a remarkable finding, because it implies that relatively strong, ordered magnetic fields (of a few tens of microgauss in strength) exist in the highly disrupted environments of galaxy clusters such as Abell 3376. For comparison, relatively weak magnetic fields (of a few microgauss) have been detected13 in the gas at the centres of clusters less disrupted than Abell 3376. So far, it has proved extremely challenging to detect and measure magnetic fields in clusters and in the space between galaxies, and the origin of cosmic magnetic fields is still mysterious. Consequently, any observational evidence for such fields in cluster environments is valuable.
However, there is another plausible explanation for the bent jets, referred to as the slingshot model. In this scenario, MRC 0600‑399 and the nearby radio galaxy are falling back towards the centre of Abell 3376 after being ejected from the centre at supersonic speed. The radio jets of MRC 0600‑399 are bent simply by the pressure of gaseous wind acting in the opposite direction to the galaxy’s motion. Although this alternative model can explain the bent jets, it cannot account for the peculiar double-scythe structures, which suggest that the jets are interacting with a layer of strong, ordered magnetic fields. One limitation of the current work is that the magnetic-field strength in the jet-interaction region was not measured directly but was obtained from numerical simulations.
The most exciting aspect of Chibueze and colleagues’ finding is that the observations of radio jets from SMBHs in galactic centres might help to explain poorly understood processes involving gas dynamics in galaxy-cluster formation. Sensitive measurements of the polarization of radio waves could confirm the strength and ordering of the magnetic fields in the magnetic boundary layer. Moreover, the discovery of other examples of strongly distorted radio jets might enable scientists to, for example, measure the total energy injected into jets by SMBHs, understand the role of magnetic fields in jet stabilization and determine the magnetic-field strength of the gas inside clusters. In the upcoming years, the most sensitive radio telescopes ever built will reveal many spectacular processes in the Universe that cannot be seen using optical instruments.
Nature 593, 40-41 (2021)
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