Journal
ASTRONOMY AT HIGH ANGULAR RESOLUTION 2011: THE CENTRAL KILOPARSEC IN GALACTIC NUCLEI
Volume 372, Issue -, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/1742-6596/372/1/012023
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Funding
- NASA Earth & Space Science Fellowship [NNX08AX59H]
- STScI [HST-GO-11732.02-A]
- NSF [AST 0807385]
- NASA [05-ATP05-96]
- NASA Chandra Fellowship [PF7-80048]
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Ongoing millimeter VLBI observations with the Event Horizon Telescope allow unprecedented study of the innermost portion of black hole accretion flows. Interpreting the observations requires relativistic, time-dependent physical modeling. We discuss the comparison of radiative transfer calculations from general relativistic MHD simulations of Sagittarius A* and M87 with current and future mm-VLBI observations. This comparison allows estimates of the viewing geometry and physical conditions of the Sgr A* accretion flow. The viewing geometry for M87 is already constrained from observations of its large-scale jet, but, unlike Sgr A*, there is no consensus for its millimeter emission geometry or electron population. Despite this uncertainty, as long as the emission region is compact, robust predictions for the size of its jet launching region can be made. For both sources, the black hole shadow may be detected with future observations including ALMA and/or the LMT, which would constitute the first direct evidence for a black hole event horizon.
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