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It is shown how present uncertainties in the ability to compute collisional cross sections for rotational transitions can lead to order of magnitude errors in the interpretation of the observed antenna temperatures for rotational emission lines from interstellar clouds. The framework within which improved cross sections can be derived is described

Data from solar line of sight velocity measurements are presented to demonstrate the existence of a synodic signal with a 6.5 m/sec amplitude. Recordings of alternate measurements of the resonantly scattered light intensity were made at 1 sec intervals and a mean ratio for the laboratory and solar lines was calculated over a 42 sec interval

An automatic and fast procedure was implemented to determine Te and log g from the comparison of the UV S 2/68 spectra with the Kurucz models. The method has been applied to all A and F stars with (B-V)0 greater than or equal to 0 and luminosity classes III, IV, IV-V, and V, included in the Ultraviolet Bright-Star Spectrophotometric Catalogue. From

Calculations of atmospheric transmission through the M (5 microns) atmospheric window, at a resolution of 10 to the 3rd power are presented for sites at the Observatorio del Teide, Tenerife and the NHO, La Plama in the Canary Islands. We use a standard midlatitude atmospheric model and absorption line strengths for the known molecular species