Black Hole Shadow Image and Visibility Analysis of Sagittarius A*

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dc.creatorHuang, Lei
dc.creatorCai, Mike
dc.creatorShen, Zhi-Qiang
dc.creatorYuan, Feng
dc.date2007-03-12
dc.date2007-03-13
dc.date.accessioned2026-07-07T11:01:03Z
dc.date.available2026-07-07T11:01:03Z
dc.descriptionThe 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.
dc.description11 pages, 18 figures (.eps), MNRAS accepted
dc.identifierhttps://arxiv.org/abs/astro-ph/0703254
dc.identifierhttp://arxiv.org/abs/astro-ph/0703254
dc.identifierMon.Not.Roy.Astron.Soc.379:833-840,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11713.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187844
dc.subjectAstrophysics
dc.titleBlack Hole Shadow Image and Visibility Analysis of Sagittarius A*
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