Titlebook: Galactic Radio Astronomy; F. J. Kerr,S. C. Simonson Book 1974 International Astronomical Union 1974 Galaxy.astronomy.interstellar matter.p

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The Observational Evidence for an Intercloud Mediumes, self-absorption features in emission profiles, and absorption profiles in the directions of discrete sources. It is concluded that the intercloud medium in the solar neighbourhood has a temperature between 10. and 10. K, a column density of ~1.4×10. cosec |.| atoms cm., and a brightness temperat

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A Modern Look at ‘Interstellar Clouds’.Interstellar optical absorption lines and H. 21-cm emission lines show a number of very large aggregates with properties similar to those of ‘cloud complexes’. At nonzero velocities especially for . < 0°, exist optical lines which have no Hi counterparts. These are almost certainly produced in low-

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Properties of Neutral Hydrogen Cloudsy means of computerized procedures. Maps of some of the clouds so defined are presented, and their properties discussed. Many clouds are elongated and/or irregular in shape. Histograms of cloud parameters are presented and subjected to statistical analysis. There is evidence for tenuous clouds of la

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Free Electrons Outside H , Regionsbourhood is of the order of 0.03 cm., and does not seem to vary very much between the H. clouds and the intercloud medium, or between the arms and the interarm region. The . thickness of the electron layer in the solar neighbourhood is found to be larger than or of the order of 0.8 kpc. No reliable

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Expanding Shells of Neutral Hydrogen as Birthplaces of Stellar AssociationsA model of the spatial configuration and the kinematics of gas, dust and stars is discussed. The stars of the associations lie outside, close to the shells; gas and stars move outward from a common centre of expansion. If the shells are interpreted as old supernova remnants which have been strongly

Antarctic

Extended OH Emission at 1720 MHZof W43 and W51 show no detectable circular polarization and are about 27 and 32 arcmin in size, respectively. The inferred peak brightness temperatures are 0.6 K for W43 and 2.0 K for W51. This emission may be similar to the nonthermal 1720-MHz emission in dust clouds.

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