By V. Radhakrishnan (auth.), F. J. Kerr, S. C. Simonson III (eds.)
'Galactic Radio Astronomy' was once selected because the topic of this Symposium, which used to be held along side the IAU basic meeting that came about in Sydney in August 1973, mostly since it is a truly appropriate Southern Hemisphere subject. This ends up in half from the benefits of a southern situation in learning the Galaxy and partly from the lengthy organization of Australia with radio astronomy. Following the final meeting, the Symposium used to be held on the Surf air Inter nationwide lodge in Maroochydore, Queensland, from three to 7 September, 1973. The convention members have been successfully remoted from the remainder of the realm in the course of the Symposium, and the superb spring climate and geographical scenario resulted in the advance of an surprisingly solid rapport. The Symposium used to be backed through 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. turbines, 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, sorted the preparations in very superb kind. The Symposium used to be supported financially through the IAU, the Australian Academy o~ technological know-how, the CSIRO department of Radiophysics, Union Carbide Australia constrained, and the technological know-how starting place for Physics in the college of Sydney.
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For a single 21-cm line profile taken at the position of the star this feature is not distinguishable as a distinct peak and would only appear as a weak, extended line wing. HD 34816 (1=215°) has a weak, large diameter feature nearby (1=206 to 214°); in Figure 3a the star seems to be located in the boundary region of this feature. Again, for a single 21-cm line profile this feature would appear only as an extended line wing, even at the most intense position near 1= 210°. zlI ',:i'Ij .. " . '-- .
2c-d. ,: ... ".. I ~~~~ o ________________________________ 270 ~ I B 0 ____ .. -~ ~~_ o (c) Regions referred to in the text. (d) The locations of dust clouds catalogued by Lynds (1962). Made from computer cards recently generated by Lynds. o Velo cit y. k m/sec Figs. 3a-b. Contour maps of antenna temperature vs. galactic longitude and velocity, for fixed galactic latitude. Each covers a star showing an interstellar CaD line with no corresponding Hlline. The position of the star and the velocity of the line are located at the tip of the arrow.
F - ,~. ~ 'W IV rn ~ ffi (j o .. '" . , -JO -,. '0 ,. 'oL-----______ 90 L Figs. 2c-d. ,: ... ".. I ~~~~ o ________________________________ 270 ~ I B 0 ____ .. -~ ~~_ o (c) Regions referred to in the text. (d) The locations of dust clouds catalogued by Lynds (1962). Made from computer cards recently generated by Lynds. o Velo cit y. k m/sec Figs. 3a-b. Contour maps of antenna temperature vs. galactic longitude and velocity, for fixed galactic latitude. Each covers a star showing an interstellar CaD line with no corresponding Hlline.