With the 60-inch reflector at Mount Wilson Observatory, Francis G. Pease obtained the first measurements of the rotation curves of two nearly edge-on spiral galaxies, NGC 4594 (the Sombrero Galaxy) and NGC 224 (the Andromeda Galaxy) in 1916 and 1918, respectively. Pease aligned the spectrograph's slit with the major axes of the galaxies' foreshortened elliptical figures and obtained direct measurements of the Doppler-induced radial velocity components along their axes. This technique originally had been applied in 1895 by James E. Keeler to a rotational analysis of the rings of Saturn. By subtracting out the radial velocities of their centers, Pease obtained their rotational velocities as a function of distance away from the centers. This enabled him to determine that linear relationships existed in both cases, whereby these objects appeared to show evidence of solid-body rotations out to (and beyond) the limits that could be observed spectroscopically (about 2.5 arcminutes from their centers). These relationships contradicted the behaviors of planets that orbited our Sun, and indicated that the objects' mass distributions likewise increased in direct proportion away from the centers. Pease's dynamical results were applied in two independent cases (by Ernst J. Öpik and Knut Lundmark) to a greater understanding of the distance and nature of the 'spiral nebulae' in the aftermath of the 'Great Debate'. Yet, the remaining questions posed by Pease's data were not effectively answered for two decades (or more) until Horace W. Babcock extended spectroscopic investigations into the disk region of the Andromeda Galaxy and showed that those stellar velocities were largely independent of their distances from the center. Along with many other examples, this finding was later confirmed by Vera Rubin and her colleagues and has become one of the leading forms of evidence for the existence of dark matter in galaxies.
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