. Carnegie Institution of Washington publication. le for the superposition of non-reversed spectra, REVERSED AND NON-REVERSED SPECTRA. 35 under conditions where the paths of the component rays may have anylength whatever. It is thus an essential extension to the method (fig. 21)given in the preceding report (PPf, prisms; M, N, mirrors; Gp, Ives prismgrating; T, telescope), where the path-differences were essentially small andthe spectra reversed. In figure 22, P is the first prism cleaving the white beam L, diffracted bythe slit of the collimator. M and N are the opaque mirrors, the former on
. Carnegie Institution of Washington publication. le for the superposition of non-reversed spectra, REVERSED AND NON-REVERSED SPECTRA. 35 under conditions where the paths of the component rays may have anylength whatever. It is thus an essential extension to the method (fig. 21)given in the preceding report (PPf, prisms; M, N, mirrors; Gp, Ives prismgrating; T, telescope), where the path-differences were essentially small andthe spectra reversed. In figure 22, P is the first prism cleaving the white beam L, diffracted bythe slit of the collimator. M and N are the opaque mirrors, the former on amicrometer. For greater ease in adjustment, the second prism P is hereright-angled, though this is otherwise inconvenient, since the angle 8 = 90° — <pis too large. The rays reflected from P impinge normally on the reflectinggrating G (D = 200X10^) and are observed by a telescope at T. P, P, M,and N are all provided with the usual three adjustment screws. P must becapable of being raised and lowered and moved fore and aft. The field is 21. 22
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