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The Milagro hot spot A, close to the Galactic anticenter direction, has beententatively attributed to cosmic rays from a local reservoir (at a distance~100 pc), freely streaming along diverging and smooth magnetic field lines.This is at variance with the geometry of the ~kpc scale Galactic magneticfield, which is known to be aligned with the spiral arms. We investigate theinformation available on the geometry of the magnetic field on the scales (~100pc) of relevance here. The magnetic field immediately upstream of theheliosphere has been investigated by previous authors by modeling theinteraction of this field with the solar wind. At larger distances, we use thedispersion measure and the rotation measure of nearby pulsars (especiallytowards the third Galactic quadrant). Additional information about the localfield towards the North Polar Spur is taken from previous studies of thediffuse radio emission and the polarization of starlight. The asymmetry of theheliosphere with respect to the incoming interstellar medium implies a magneticfield almost orthogonal to the local spiral arm, in the general direction ofhot spot A, but more to the south. This is in good agreement with the nearbypulsar data on the one side, and the North Polar Spur data on the other. Thelocal magnetic field on scales of ~100 parsecs around the Sun seems to beoriented so as to provide a direct connection between the Solar system and apossible site of the Geminga supernova; the residual angular difference and theshape and orientation of the Milagro hot spot can be attributed to the fieldtrailing in the wake of the heliosphere.

The local Galactic magnetic field in the direction of Geminga