Journal
ASTROPHYSICAL JOURNAL
Volume 788, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/788/2/120
Keywords
black hole physics; galaxies: active; galaxies: jets; submillimeter: galaxies; techniques: high angular resolution; techniques: interferometric
Categories
Funding
- National Science Foundation
- NSF [AST-1310896, AST-1211539]
- Gordon & Betty Moore Foundation [GMBF-3561]
- Perimeter Institute for Theoretical Physics
- Natural Sciences and Engineering Research Council of Canada through a Discovery Grant
- Government of Canada through Industry Canada
- Province of Ontario through the Ministry of Research and Innovation
- Direct For Mathematical & Physical Scien [1210972] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1445935, 1126433, 1310896] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [1210972] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1337663, 1211539] Funding Source: National Science Foundation
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The Event Horizon Telescope (EHT) is a project to assemble a Very Long Baseline Interferometry (VLBI) network of millimeter wavelength dishes that can resolve strong field general relativistic signatures near a supermassive black hole. As planned, the EHT will include enough dishes to enable imaging of the predicted black hole shadow, a feature caused by severe light bending at the black hole boundary. The center of M87, a giant elliptical galaxy, presents one of the most interesting EHT targets as it exhibits a relativistic jet, offering the additional possibility of studying jet genesis on Schwarzschild radius scales. Fully relativistic models of the M87 jet that fit all existing observational constraints now allow horizon-scale images to be generated. We perform realistic VLBI simulations of M87 model images to examine the detectability of the black shadow with the EHT, focusing on a sequence of model images with a changing jet mass load radius. When the jet is launched close to the black hole, the shadow is clearly visible both at 230 and 345 GHz. The EHT array with a resolution of 20-30 mu as resolution (similar to 2-4 Schwarzschild radii) is able to image this feature independent of any theoretical models and we show that imaging methods used to process data from optical interferometers are applicable and effective for EHT data sets. We demonstrate that the EHT is also capable of tracing real-time structural changes on a few Schwarzschild radii scales, such as those implicated by very high-energy flaring activity of M87. While inclusion of ALMA in the EHT is critical for shadow imaging, the array is generally robust against loss of a station.
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