A re-analysis of pulsar rotation measures suggests that the systematic component of the galactic magnetic field is confined to the gas-disc region of the Galaxy (|Z| ≲ 120 pc), and exhibits a reversal in direction towards the inner spiral arm. Estimates are obtained for the direction, intensity and scale height of this systematic component, the distance of the reversal from the Sun, the vertical displacement of the Sun from the magnetoactive midplane, and an approximate value for the intensity of the random magnetic field component.
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Thomson et al. (1980) studied this question.