Fan-beam Observations of Radio Sources at 21 cm Wavelength

Labrum, N. R.; Krishnan, T.; Payten, W. J.; Harting, E.

doi:10.1071/ph640323

Cited by 6 publications

(3 citation statements)

References 3 publications

(3 reference statements)

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“…Investigations of the important question of the relative position of fundamental and harmonic is as yet unanswered ; the first observations are being analysed. 10 -u Observations of type V bursts (e.g., Figure 3) and U bursts (e.g., Figure 4) by Labrum 10 and others support existing theories convincingly. When a type III burst is followed by a type V 7 > 10 ' 12 it is common to find a shift in position and an increase in angular size.…”

Section: Type III V and U Bursts: Impulsive Streams Of Fast Electronsmentioning

confidence: 54%

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Some Investigations of the Solar Corona: The First Two Years of Observation With the Culgoora Radioheliograph

Wild

1970

Publ. Astron. Soc. Aust.

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The first meaningful observation with the 80 MHz Cul-goora radioheliograph was made on 2 September 1967, a few weeks before the instrument was officially commissioned. Systematic observations, normally for 4 to 6 hours per day, began late in February 1968 and the Sun has since been observed on 438 days. The remaining days and many nights have been used for investigations of radio sources and the interplanetary medium and for maintenance and instrumental extension. The standard of reliability thus achieved has been due to the sustained efforts of K. V. Sheridan, W. J. Payten, K. R. McAlister, M. Beard and their colleagues. These first two years have been a period mainly of exploration—a phase of great interest to those engaged in observing, though possibly bewildering to those not. The present review is a first attempt to collate and summarize what has so far been found and where possible to draw preliminary conclusions. The observations to be described and their discussion have been due to a joint effort on the part of a number of workers, particularly G. A. Dulk (on leave from the University of Colorado), K. Kai (on leave from the University of Tokyo), N. R. Labrum, D. J. McLean, A. C. Riddle, K. V. Sheridan, S. F. Smerd, R. T. Stewart, and the present writer. The period has also seen considerable development in the evolution of intricate computer programmes for analysing the data, particularly on the part of L. H. Heisler and D. J. McLean.

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Section: Type III V and U Bursts: Impulsive Streams Of Fast Electronsmentioning

confidence: 54%

“…(After Labrum. 10 ) which the type V is not distinguished from the III except for a higher temperature in its region of origin. Most of the U bursts so far observed show marked changes in position between upward and downward branches.…”

Section: Type III V and U Bursts: Impulsive Streams Of Fast Electronsmentioning

confidence: 91%

Some Investigations of the Solar Corona: The First Two Years of Observation With the Culgoora Radioheliograph

Wild

1970

Publ. Astron. Soc. Aust.

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“…Measurements with comparable resolving power at the intermediate wavelength of 21·1 cm by Labrum et al (1964), however, do not indicate a simple variation with wavelength. All we can say is that the spectra of the two parts, or of the finer structures yet to be resolved, are sharply different.…”

Section: 'mentioning

confidence: 99%

The Central Component Of Centaurus A

1966

Aust. J. Phys.

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SummaryTransit observations of Centaurus A with a fan beam 1'·5 wide at 73 cm show that the north-eastern component of the central source has an east-west width of 1'·7 and that the south-western source has a width of 2'·3. Since the situation at 9·1 cm is roughly the reverse of this, the two components must have sharply different spectra. The right ascensions observed are 13 h 22 m 48s . 0 and 13h 22m 20s·2±os·2 (1950). The right ascension of the centre of NGC5128 has been separately determined as 13h 22m 31s·6±os·3, showing that the two components are at significantly unequal distances from the optical object.

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Expanding Horizons – The Milky Way and Beyond

Orchiston

Robertson

Sullivan

2021

Golden Years of Australian Radio Astronomy

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Non-solar research at the Radiophysics Laboratory (RP) was launched in September 1946 when Joe Pawsey (1908–1962) tried unsuccessfully to observe the enigmatic ‘radio star’ in Cygnus that the British team of Stanley Hey (1909–2000, Fig. 4.1), John Parsons and James Phillips (1946) had announced in the 17 August issue of Nature. Two months later, John Bolton (1922–1993; Fig. 4.2) and research assistant Bruce Slee (1924–2016) were at Dover Heights trying to observe the Sun at 60 MHz. When it insisted on remaining inactive they decided to use their 2-Yagi antenna in sea interferometer mode to search for radio emission from other types of objects. Neither had a background in astronomy, and their astronomical knowledge and resources were virtually non-existent. Bolton (1982: 349) later described how they used the Russell, Duggan and Stewart book Astronomy to “… hazard guesses as to which types of objects might emit copious amounts of radio emission …” and Norton’s Star Atlas “… to find the position of the brightest candidate in each class.”

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Fan-beam Observations of Radio Sources at 21 cm Wavelength

Cited by 6 publications

References 3 publications

Some Investigations of the Solar Corona: The First Two Years of Observation With the Culgoora Radioheliograph

Some Investigations of the Solar Corona: The First Two Years of Observation With the Culgoora Radioheliograph

The Central Component Of Centaurus A

Expanding Horizons – The Milky Way and Beyond

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