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Extra info for Astrophysik V: Verschiedenes / Astrophysics V: Miscellaneous
14, 337 (1927). Sect. 12. 25 Spectroscopes. mirror. This circumstance, and the use of paraboloidal mirrors for the concaves, limits the field of view to nearly a single spectrum line. The design provides a wider choice of positions for the dispersing element (grating or prism) than is the case for the Ebert system. A limited extent of the focal surface of good image quality is a common characteristic of all plane grating spectroscopes in use for solar research. The range of wavelengths covered at adequate plate scale (not less than t A/mm for usual solar work) is not more than a few hundred angstroms at best, but for many types of observation of the Sun it would be desirable to record the entire photographic spectrum from 13000 to 2900 A at high dispersion and high resolving power.
And others: Vistas in Astronomy, ed. by A. BEER, Vol. 1, p. 400. London and New York: Pergamon Press 1955. - Several sections contain discussions by different authors of instruments and instrumental problems of solar astronomy. The section by H. VON KLUBER: "Spectroscopic Measurements of Magnetic Fields on the Sun" is exceptionally complete. , and R. v. D. R. WOOLEY: Eclipses of the Sun and Moon, Chap. 9, p. 57. Oxford: Clarendon Press 1937. - Brief descriptions of some of the important instruments used for solar observation at eclipse time.
18. Table. Solar tower teleBlank spaces in the table remain where information to fill them could not be obtained. - Only solar tower telescopes are listed. It is intended to supplement the information in the table by H. GOLLNOW (Naturwiss. 36, 175, 213 (1949)], and to give data for solar tower telescopes not completed at the date of GOLLNOW'S compilation. The telescopes are a) Coelostats. 5 m tower University of Michigan 1940 15 Kanzelhohe University of Graz 1947 16 Rome Monte Mario 1948 17 Capri Fraunhofer Institut 1953 30 18 Co.