An international team monitors the deeper structure of a quasar’s jet stream


An international team monitors the deeper structure of a quasar's jet stream

Radio astronomy images of 3C 273. The close-up view on the left is the deepest look yet at the plasma flow of quasar 3C 273. The image in the center shows the elongated fuselage of the aircraft. The image on the right is a visible light image of a quasar taken by the Hubble Space Telescope. Wireless observations were made by a Global Millimeter VLBI Array (GMVA) joined by the Atacama Large Millimeter/submillimeter Array (ALMA) and High Sensitivity Array (HSA). Credit: Hiroki Okino and Kazunori Akiyama; GMVA+ALMA and HSA images: Okino et al.; HST image: ESA/Hubble & NASA

An international team of scientists observed the narrowing of the quasar’s jet for the first time using a network of radio telescopes around the world. The results indicate that the narrowing of the jet is unrelated to the activity level of the galaxy that triggered it.

Almost every galaxy hosts a Giant black hole in the midst of it. In some cases, huge amounts of energy are released by gas falling toward the black hole, creating a phenomenon known as a quasar. Quasars emit narrow, even streams of material at nearly the speed of light. But how and where the quasar jets collide has been a long-standing mystery.

An international team led by Hiroki Okino, a graduate student at the University of Tokyo, and including members from the National Astronomical Observatory of Japan (NAOJ), MIT, Kogakuen University, Hachinohe National College of Technology, and Niigata University, captured an image with the highest angle resolution to date that shows the deepest Part of the outflow in a bright quasar known as 3C 273.

فريق دولي يراقب البنية الأعمق لنفث الكوازار النفاث 1 . Oceanic lows are 6.5 mJy beam -1 at 43GHz, 8.2mJ -1 at 22GHz, 7.1mJ -1 at 15 GHz and 11.6 mJ beam -1 At 1.7 GHz. The boundaries of all images are multiplied by a factor of 2. The lowest bounding level for each image is estimated from the rms mean of the remaining image of the reconstructions in the upper group. Credit: The Astrophysical Journal (2022). DOI: 10.3847/1538-4357/ac97e5″/>

Multi-frequency images of 3C 273 aircraft with HSA at 43, 22 and 15 GHz and VLBA at 1.7 GHz. Each panel shows the mean of the upper group image at each frequency recovered by the circular Gaussian beam angle solid beam for the uniform weighting beam size in Table 1. The lowest contour levels are 6.5 mJy beam-1 At 43 GHz, the beam is 8.2 mJ-1 At 22 GHz, the beam is 7.1 mJ-1 at 15 GHz and 11.6 mJ beam-1 At 1.7 GHz. The boundaries of all images are multiplied by a factor of 2. The lowest bounding level for each image is estimated from the rms mean of the remaining image of the reconstructions in the upper group. attributed to him: Astrophysical Journal (2022). DOI: 10.3847/1538-4357/ac97e5

The team found that the outflow from the quasar narrows to a very long distance. This narrow part of the plane continues incredibly far, far beyond the region dominated by the black hole’s gravity. The results show that the airframe is similar to planes launched from nearby galaxies With a low-luminosity active core. This may indicate that the jet collimators are independent of the level of activity in the host galaxy, providing an important clue to revealing the inner workings of the jets.

These results appeared in Astrophysical Journal On November 22, 2022.

more information:
Hiroki Okino et al, Relativistic jet collimator at Quasar 3C 273, Astrophysical Journal (2022). DOI: 10.3847/1538-4357/ac97e5

the quote: International Team Observes Quasar Jet’s Innermost Structure (2022, November 22) Retrieved November 23, 2022 from https://phys.org/news/2022-11-international-team-innermost-quasar-jet.html

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