By M. S. Davis (auth.), C. Jaschek, G. A. Wilkins (eds.)
The valuable objective of IAU Colloquium No. 35 was once to debate these points of the suggestions of the compilation, evaluate, and distribution of knowledge which are universal to astrometry, photometry and spectrometry of stars and stellar platforms. within the statement of the Colloquium, it was once prompt that there will be distinctive emphasis at the options of qc, and at the criteria for the presentation of numerical info in either published and com puter-readable shape. because the assembly advanced it grew to become transparent that the shortcoming of a customary, unambiguous approach for the identifi cation of stellar items used to be a resource of a lot confusion and inefficiency within the use of latest facts documents. This and different such issues have been the topic of additional discussions through fee five on the common meeting of the overseas Astronomical Union (IAU), which was once held at Grenoble throughout the following fortnight, 24 August - 2 September 1976. The inspiration for the Colloquium was once ready via J. Jung, who used to be then Director of the Centre des Donnees Stellaires at Stras bourg, and G. A. Wilkins, Chairman of the IAU operating staff on Numerical info, and used to be accredited through the IAU govt Committee at the advice of the President of fee five, with the help of Commissions 25, 29 and forty five. The clinical setting up Committee consisted of W. Fricke, B. Hauck, C. Jaschek, J. Jung, B. Kukarkin, P. Lacroute, A. Underhill and G. A. Wilkins (Chair man). The neighborhood setting up Committee consisted of A.
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Additional info for Compilation, Critical Evaluation and Distribution of Stellar Data: Proceedings of the International Astronomical Union Colloquium No. 35, held at Strasbourg, France, 19–21 August, 1976
5. Markowitz, W M, 1973. SI, The International System of Units. Geophysical Surveys l, 217-241. PART II ACQUISITION AND PROCESSING TECHNIQUES THE INFLUENCE OF ACQUISITION TECHNIQUES ON THE COMPILATION OF ASTRONOMICAL DATA Gart Westerhout Astronomy Program University of Maryland College Park, Maryland 20742, USA With the increasing use of electronic rather than photographic data collection, and on-line minicomputers at the telescope, two factors will necessitate a reconsideration of the way in which data are stored at the telescope.
Since that time new programmes for determining trigonometric parallaxes have been started, concentrating mainly on nearby faint objects as white dwarfs and red dwarfs. The catalogues of the US Naval Observatory already have listed several hundreds of new distances determined with the 61-inch reflector at Flagstaff. Furthermore, some lists with spectroscopic and photometric parallaxes have been published. Altogether, about two hundred new stars at least can be added to the collection of objects in the solar neighbourhood.
High-Resolution Spectroscopy. Usually high-resolution spectra are obtained photographically at the Coud~ focus of a telescope. The principal use of Coud~ spectroscopy is for the study of detailed line profiles in a variety of applications. Often, the spectra are traced with a microdensitometer and usually digitized in some form or another for work with stellar atmosphere models. Neither spectra nor tracings end up in internationally accessible data files, although people sometimes acquire older spectra from observatory plate files.
Compilation, Critical Evaluation and Distribution of Stellar Data: Proceedings of the International Astronomical Union Colloquium No. 35, held at Strasbourg, France, 19–21 August, 1976 by M. S. Davis (auth.), C. Jaschek, G. A. Wilkins (eds.)