Galactic Radio Astronomy by V. Radhakrishnan (auth.), F. J. Kerr, S. C. Simonson III

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By V. Radhakrishnan (auth.), F. J. Kerr, S. C. Simonson III (eds.)

'Galactic Radio Astronomy' used to be selected because the topic of this Symposium, which used to be held along with the IAU basic meeting that happened in Sydney in August 1973, mostly since it is a really appropriate Southern Hemisphere subject. This leads to half from the benefits of a southern situation in learning the Galaxy and partially from the lengthy organization of Australia with radio astronomy. Following the overall meeting, the Symposium was once held on the Surf air Inter­ nationwide inn in Maroochydore, Queensland, from three to 7 September, 1973. The convention individuals have been successfully remoted from the remainder of the realm throughout the Symposium, and the superb spring climate and geographical state of affairs resulted in the improvement of an surprisingly solid rapport. The Symposium used to be subsidized by way of Commissions forty, 33, and 34. The Organizing Committee used to be composed of A. H. Barrett (chairman), J. E. Baldwin, D. S. Heeschen, F. J. Kerr, J. Lequeux, S. W. McCuskey, P. G. Mezger, B. Y. generators, Yu. N. Parijskij, B. J. Robinson, H. van der Laan, and H. F. Weaver. The neighborhood Committee, consisting ofB. J. Robinson, N. G. Seddon, and P. J. Kelly, taken care of the preparations in very advantageous kind. The Symposium was once supported financially via the IAU, the Australian Academy o~ technological know-how, the CSIRO department of Radiophysics, Union Carbide Australia restricted, and the technology beginning for Physics in the collage of Sydney.

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This implies angular structure on the scale of 1°, or about 2 pc for this cloud. H I data shows that this cloud extends about 12° in longitude at b=23°, and about 20° in latitude. 5 to 1 (km S-1) per degree. However, there are a number of sub-condensations within the cloud. The Pleiades cluster lies near an internal boundary where the H I changes particularly rapidly with position. Thus the optical data show the structure within the cloud rather than the angular extent of the cloud as a whole, and an interpretation based on the latter assumption is misleading.

4 km s - 1 for two sheets. The velocity of a sheet varies slowly, if at all, with position. Another sheet has been found in the Taurus region by Baker (1973b), who suspects the sheets may form a ring-like structure around the solar neighborhood. Herbig (1968), using optical techniques, finds a large sheet in front of ( Oph from interstellar absorption lines. Sancisi and van Woerden (1970) saw a filamentary-shaped feature near 1=350°, b=20°. This object is barely visible on Figure 2. It is 4° wide and 14° long, perhaps longer because it may extend beyond their southern declination limit of - 30°.

Van Woerden (1967) mapped 140 deg 2 of the Orion region, distinguishing 31 clouds by careful Gaussian analysis of all the profiles. He mapped the clouds by mapping the Gaussian parameters and found that the clouds are not dissimilar from the 'standard' interstellar cloud (Spitzer, 1968b). Both the velocities and shapes appear randomly distributed, in accord with the standard cloud model. Assuming a distance of 280 pc as used in Table I rather than the 480 pc used by van Woerden, cloud diameters are typically 25 pc, densities a few atoms cm- 3, and masses about l000M 0 .

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