6-cm VLBI Observations of Compact Radio Sources PDF Download
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Author:
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ISBN:
Category :
Languages : en
Pages : 15
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Author:
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ISBN:
Category :
Languages : en
Pages : 15
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Author: Roberto Fanti
Publisher: Springer Science & Business Media
ISBN: 9789027717399
Category : Science
Languages : en
Pages : 522
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Book Description
I.A.U. symposium No. 110 on VLBI and Compact Radio Sources was held in Bologna, Italy from June 27 to July 1, 1983. 166 participants from 19 countries were registered and 106 invited and contributed papers were registered. The scientific presentations and discussion concentrated on VLBI observation and interpretation of galactic and extragalactic radio sour ces, including topics as diverse as quasars and galactic nuclei, inter stellar masers, pulsars, and astrometry. Geodetic applications and tech nical development were treated only briefly, as these topics have been the subject of other recent international symposia. Since the first VLBI observations in 1967, sensitivity, resolution, and image quality have improved dramatically. Radio maps shown at the symposium were of comparable quality to conventional synthesis maps be ing made at the time of the first VLBI experiments 15 years ago, but with a resolution more than a factor of 1000 better. We wanted to accommodate the large number of contributed papers in this rapidly developing field, but there was inadequate time for normal oral presentations and discussion. We therefore asked that all contrib uted papers be put on display for at least 24 hours prior to a brief oral summary. A question and discussion period followed groups of oral pres entations on the same or similar topic. In this way the opportunity for interactive discussion, not available in conventional poster displays, was preserved.
Author: Mark Warren Hodges
Publisher:
ISBN:
Category : Interferometry
Languages : en
Pages : 172
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Author: K. Y. Lo
Publisher:
ISBN:
Category :
Languages : en
Pages : 14
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The detection of a compact radio source in the direction of the Galactic Center during VLBI observations at 3.7 cm on 19 May, 1975 between the Owens Valley Radio Observatory 40-m telescope and the Goldstone 64-m telescope is reported. The recording of the signals and the subsequent cross-correlation were made with the standard MkII VLBI system with a bandwidth of 2 MHz.
Author: Roberto Fanti
Publisher: Springer
ISBN: 9789401099387
Category : Science
Languages : en
Pages : 0
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Book Description
I.A.U. symposium No. 110 on VLBI and Compact Radio Sources was held in Bologna, Italy from June 27 to July 1, 1983. 166 participants from 19 countries were registered and 106 invited and contributed papers were registered. The scientific presentations and discussion concentrated on VLBI observation and interpretation of galactic and extragalactic radio sour ces, including topics as diverse as quasars and galactic nuclei, inter stellar masers, pulsars, and astrometry. Geodetic applications and tech nical development were treated only briefly, as these topics have been the subject of other recent international symposia. Since the first VLBI observations in 1967, sensitivity, resolution, and image quality have improved dramatically. Radio maps shown at the symposium were of comparable quality to conventional synthesis maps be ing made at the time of the first VLBI experiments 15 years ago, but with a resolution more than a factor of 1000 better. We wanted to accommodate the large number of contributed papers in this rapidly developing field, but there was inadequate time for normal oral presentations and discussion. We therefore asked that all contrib uted papers be put on display for at least 24 hours prior to a brief oral summary. A question and discussion period followed groups of oral pres entations on the same or similar topic. In this way the opportunity for interactive discussion, not available in conventional poster displays, was preserved.
Author: Antonios G. Polatidis
Publisher:
ISBN:
Category :
Languages : en
Pages : 320
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Author: K. I. Kellermann
Publisher:
ISBN:
Category :
Languages : en
Pages : 55
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The small scale structure of extragalactic radio sources has been studied at 18 and 6 cm wavelengths using a tape recording interferometer. At the longest antenna spacing, 10,536 km, the baselines at 6 cm was 176 million wavelengths and the resolution was about 0.0004 arc seconds for the stronger sources. Many sources, including optically identified galaxies and quasars, are found to have several distinct components of widely differing size in the range from the few hundredths of a second of arc to the limit of our resolution. Many sources, including 0106+01, 3C 273, 3C279, 1555+00, 2145+06, 3C 446, 3C 454.3, and 2345-16 all contain components which are unresolved on the longest baseline are less than .0004 arc sec. in diameter. Observations at shorter wavelengths are required to resolve these sources. Because the maximum brightness temperature is limited to 10 to the 12th power K, by inverse Compton scattering, baselines no greater than the diameter of the earth are probably adequate to resolve all of the stronger extragalactic sources. (Author).
Author: John J. Broderick
Publisher:
ISBN:
Category : Astronomy
Languages : en
Pages : 7
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Author: Roberto Fanti
Publisher:
ISBN:
Category :
Languages : en
Pages : 489
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Book Description
Author: J. Anton Zensus
Publisher: Cambridge University Press
ISBN: 9780521392266
Category : Crafts & Hobbies
Languages : en
Pages : 430
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Book Description
Quasars and active galaxies are the most powerful emitters of radiation in the universe. Modern radio telescope arrays have shown that the ultimate energy source resides in the central few parsecs of the galactic nucleus, and powers the emitting regions by way of two oppositely-directed relativistic jets of energy. This volume presents the latest observations and theories of these remarkable objects. Topics discussed include superluminal motions, the physics of jets and shock fronts in jets, related optical observations, and cosmic evolution. Particular attention is given to the "unified theories," which attempt to show that many of the phenomena in powerful extragalactic objects are different aspects of a single, basic mechanism; the main difference in their appearance is a result of their different orientation with respect to the observer.
