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Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre 总被引:1,自引:0,他引:1
Doeleman SS Weintroub J Rogers AE Plambeck R Freund R Tilanus RP Friberg P Ziurys LM Moran JM Corey B Young KH Smythe DL Titus M Marrone DP Cappallo RJ Bock DC Bower GC Chamberlin R Davis GR Krichbaum TP Lamb J Maness H Niell AE Roy A Strittmatter P Werthimer D Whitney AR Woody D 《Nature》2008,455(7209):78-80
The cores of most galaxies are thought to harbour supermassive black holes, which power galactic nuclei by converting the gravitational energy of accreting matter into radiation. Sagittarius A* (Sgr A*), the compact source of radio, infrared and X-ray emission at the centre of the Milky Way, is the closest example of this phenomenon, with an estimated black hole mass that is 4,000,000 times that of the Sun. A long-standing astronomical goal is to resolve structures in the innermost accretion flow surrounding Sgr A*, where strong gravitational fields will distort the appearance of radiation emitted near the black hole. Radio observations at wavelengths of 3.5 mm and 7 mm have detected intrinsic structure in Sgr A*, but the spatial resolution of observations at these wavelengths is limited by interstellar scattering. Here we report observations at a wavelength of 1.3 mm that set a size of 37(+16)(-10) microarcseconds on the intrinsic diameter of Sgr A*. This is less than the expected apparent size of the event horizon of the presumed black hole, suggesting that the bulk of Sgr A* emission may not be centred on the black hole, but arises in the surrounding accretion flow. 相似文献
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