Black Hole Shadow Image and Visibility Analysis of Sagittarius A
The compact dark objects with very large masses residing at the centres of galaxies are believed to be black holes. Due to the gravitational lensing effect, they would cast a shadow larger than their horizon size over the background, whose shape and size can be calculated. For the supermassive black hole candidate Sgr A*, this shadow-spans an angular size of about 50 micro arc second, which is under the resolution attainable with the current astronomical instruments. Such a shadow image of Sgr A* will be observable at about 1 mm wavelength, considering the scatter broadening by the interstellar medium. By simulating the black hole shadow image of Sgr A* with the radiatively inefficient accretion flow model, we demonstrate that analyzing the properties of the visibility function can help us determine some parameters of the black hole configuration, which is instructive to the sub-millimeter VLBI observations of Sgr A* in the near future.
black hole physics- relativity - methods numerical - scattering -Galaxyx entre - sub-millimeter - techniques rinterferometric
Lei Huang Mike Cai Zhi-Qiang Shen Feng Yuan
Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China;Graduate School Academia Sinica,Institute of Astronomy and Astrophysics,Taipei,China Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China;Joint Institute
国际会议
北京
英文
2007-04-21（万方平台首次上网日期，不代表论文的发表时间）