  Tiny interstellar dust grains causing the polarization of light from the
nearest stars are deflected sideways in the outer heliosheath regions, along
with the interstellar magnetic field. Observations of optical polarization of
stars beyond the heliosphere nose, suggest the direction of the upwind
interstellar magnetic field is relatively constant. The polarizations of nearby
stars and offset angle between HeI and HeI flowing into the heliosphere have
position angles in galactic coordinates of 30- 40 deg, indicating a local
magnetic field direction inclined by ~55 deg and ~65 deg, respectively, with
respect to the galactic and ecliptic planes. The hot and cold poles of the
measured Cosmic Microwave Background (CMB) dipole moment are nearly symmetric
around the heliosphere nose direction, and the v^{22} quadrupole vector is
directed towards the heliosphere nose. The area vectors of the CMB quadrupole
and ocotopole moments are directed towards the band perpendicular to the
ecliptic plane formed by the alternate locations for the 3 kHz emissions
detected by Voyagers 1 and 2. In the upwind direction, the position angle of
the null plane separating the CMB dipole hot and cold poles is nearly aligned
with the interstellar magnetic field direction at the Sun. Heliospheric
foreground contamination of the low-$\ell$ CMB modes now requires detailed
study.

Astrophysics