By L. Woltjer (auth.), Massimo Capaccioli (eds.)
The thought of keeping a colloquium on Schmidt telescopes (techniques and technological know-how) originated from the commentary that, within the final ten years and despite the awesome advancements and achievements during this box of astronomical examine, there were no particular chance for the specialists to fulfill jointly, make the purpose at the state-of-the-art, talk about and coordinate destiny plans. for that reason, Prof. L. Rosino, one of many pioneers within the use of wide-field telescopes, pushed additionally via the want of honouring the over 4 a long time of task of the Asiago Observatory, proposed to the administrative Committee of the foreign Astronomical Union to sponsor a colloquium on 'Astronomy with Schmidt style telescopes I to be held at Asiago on the finish of the summer time of 1983. information about the composition of the medical Organizing Committee and the sponsoring enterprises are given in Prof. Rosino's 'Welcome to the members • The granting of this notion used to be the start of a ' variety of complications tor the participants of the neighborhood Organizing Committee, R. Barbon, F. Ciatti, P. Rafanelli and myself. If, organlzationwise, the colloquium was once winning, this can be really a result of beneficiant efforts of my colleagues of the SOC and to the effective association of the Linta Park, the lodge web hosting the meeting.
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Extra resources for Astronomy with Schmidt-Type Telescopes: Proceedings of the 78th Colloquium of the International Astronomical Union, Asiago, Italy, August 30–September 2, 1983
With regard to the former, further improvements in photographic plates certainly would be important. The introduction of CCD-type detectors, however, could make a qualitative change. At present, CCDs are still small (few cm 2 ), but there does not appear to be, in pr inciple, any objection to fitting the curved focal place of a Schmidt telescope with a mosaic of CCDs. Also the data handling problem probably would not be an obstacle ~ decade from now. One may wonder, however, whether pushing the Schmidt images a further 2-3 magnitudes fainter would justify the cost of such an approach.
G. Morgan, 1983). Galaxies also give useful information; apart from the fairly obvious application to emission line galaxies, it turns out that even the low dispersion prism permits the determination of galaxy r~1shifts using the 4000~ feature to an accuracy of around 3000 km s, for the study of super-clustering (Clowes, Cooke et al. , this meeting). NON-SURVEY PROGRAMMES In this review I have concentrated on the various sky surveys being done by the UK Schmidt Telescope. However no more than half of the usable telescope time is devoted to survey work.
The layout of the Schmidt dark room is a result of experience gained at other observatories and, in particular, at the ESO Sky Atlas Laboratory and encompasses several features which contribute to the safe handling of large astronomical plates in complete darkness (cf. West and Dumoulin 1974). Dust contamination is efficiently reduced by a high standard air conditioning system with adequate filters. g. in the case of the plates for the ESO (R) Survey. This puts considerable strain upon the personnel.
Astronomy with Schmidt-Type Telescopes: Proceedings of the 78th Colloquium of the International Astronomical Union, Asiago, Italy, August 30–September 2, 1983 by L. Woltjer (auth.), Massimo Capaccioli (eds.)