  Optical spectroscopic monitoring has been conducted of two O stars in the
Small and one in the Large Magellanic Cloud, the spectral characteristics of
which place them in the Of?p category, which has been established in the Galaxy
to consist of oblique magnetic rotators. All of these Magellanic stars show
systematic spectral variations typical of the Of?p class, further strengthening
their magnetic candidacy to the point of virtual certainty. The spectral
variations are related to photometric variations derived from OGLE data by Naze
et al. (2015) in a parallel study, which yields rotational periods for two of
them. Now circular spectropolarimetry is required to measure their fields, and
ultraviolet spectroscopy to further characterize their low-metallicity,
magnetically confined winds, in support of hydrodynamical analyses.
