Imaging compact supermassive binary black holes with Very Long Baseline Interferometry
نویسندگان
چکیده
منابع مشابه
Masses of Nearby Supermassive Black Holes with Very Long Baseline Interferometry
Dynamical mass measurements to date have allowed determinations of the mass M and the distance D of a number of nearby supermassive black holes. In the case of Sgr A*, these measurements are limited by a strong correlation between the mass and distance scaling roughly as M ∼ D2. Future very long baseline interferometric (VLBI) observations will image a bright and narrow ring surrounding the sha...
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We report on the discovery of a supermassive binary black hole system in the radio galaxy 0402+379, with a projected separation between the two black holes of just 7.3 pc. This is the closest black hole pair yet found by more than two orders of magnitude. These results are based upon recent multi-frequency observations using the Very Long Baseline Array (VLBA) which reveal two compact, variable...
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Phase-referencing allows phase calibration of VLBI data. Using regular observations of a nearby calibrator source, delay, delay-rate, and phase corrections can be derived and their eeects removed from the target source visibility data. This technique allows imaging much weaker objects than is possible via fringe-tting methods. We examine the main types of phase error in VLBI observations (geome...
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A brief Note compiled by: Prof. Madhav N. Kulkarni, IIT Bombay Since the inception of the Very Long Baseline Interferometry (VLBI) system in 1967, this radio interferometry technique has revolutionised the fields of geodesy, geodynamics and astrometry. With the unprecedented precision and resolution made possible by VLBI various tasks such as geodetic positioning, reference frames interconnect...
متن کاملVery Long Baseline Interferometry and the VLBAASP
The special problems encountered when performing spectral-line VLBI observations are discussed in this Chapter. In particular, the usefulness of Fourier transforming measured visibility data with respect to time, delay or frequency for purposes of fringe detection and calibration is clariied.
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2006
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s174392130700511x