Time-Variable Compact Emission Around the Galactic Center Black Hole

Details Time-Variable Compact Emission Around the Galactic Center Black Hole Time-Variable Compact Emission Around the Galactic Center Black Hole

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21714301f&link_type=abstract

American Astronomical Society, AAS Meeting #217, #143.01; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

The Galactic Center radio source Sagittarius A* is believed to host a massive black hole. The event horizon of Sgr A* subtends a larger angle than any other known black hole candidate. The resolution of millimeter-wavelength very long baseline interferometry (VLBI) is perfectly suited to studying Sagittarius A*. In prior observations, our collaboration detected Sagittarius A* at 1.3 mm wavelength on a baseline between the James Clerk Maxwell Telescope (JCMT) in Hawaii and the Submillimeter Telescope (SMT) in Arizona, demonstrating the existence of structure on the scale of a few Schwarzschild radii. We report on new 1.3 mm VLBI observations of Sagittarius A* using an array consisting of the JCMT, the SMT, and two telescopes of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) in California. For the first time, we detect Sgr A* on JCMT-CARMA baselines. The data indicate that Sagittarius A* is composed of both a 43 microarcsecond (4.3 Schwarzschild radii) compact component as well as a large-scale component (> 300 microarcseconds) that is resolved out on VLBI baselines. The flux density of the compact component is seen to increase on one day, but the implied size of the emission region remains constant. These result place strong constraints on the quiescent and flaring emission mechanisms of Sgr A*.
High-frequency VLBI work is supported by grants from the National Science Foundation.

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