Observations of the polarization and brightness distribution of the galactic non-thermal radio emission are used in conjunction with other evidence to deduce the structure of the interstellar magnetic field within about 1.5 kpc of the Sun. Analysis of the different sources of information and different regions of the sky consistently indicates that the magnetic field is curved and convergent in the region considered, when drawn projected onto the galactic plane. There is also some evidence on the components of the field not parallel to the plane, and the thickness of the magnetic disk is discussed. The magnetic field structure deduced is apparently related to the local stellar spiral arm.