Context : We investigate the linear polarization produced by interstellar dust aligned by the magnetic field in the solar neighborhood ( d < 50 pc ) .
We also look for intrinsic effects from circumstellar processes , specifically in terms of polarization variability and wavelength dependence .

Aims : We aim to detect and map dust clouds which give rise to statistically significant amounts of polarization of the starlight passing through the cloud , and to determine the interstellar magnetic field direction from the position angle of the observed polarization .

Methods : High-precision broad-band ( BVR ) polarization observations are made of 361 stars in spectral classes F to G , with detection sensitivity at the level of or better than 10 ^ { -5 } ( 0.001 % ) .
The sample consists of 125 stars in the magnitude range 6-9 observed at the 2.2 m UH88 telescope on Mauna Kea , 205 stars in the magnitude range 3-6 observed at the Japanese ( Tohoku ) T60 telescope on Haleakala , and 31 stars in the magnitude range 4-7 observed at the 1.27 m H127 telescope of the Greenhill Observatory , Tasmania .
Identical copies of the Dipol-2 polarimeter are used on these three sites .

Results : Statistically significant ( > 3 \sigma ) polarization is found in 115 stars , and > 2 \sigma detection in 178 stars , out of the total sample of 361 stars .
Polarization maps based on these data show filament-like patterns of polarization position angles , which are related to both the heliosphere geometry , the kinematics of nearby clouds , and the Interstellar Boundary EXplorer ( IBEX ) ribbon magnetic field .
From long-term multiple observations , a number ( \sim 20 ) of stars show evidence of intrinsic variability at the 10 ^ { -5 } level .
This can be attributed to circumstellar effects ( e.g. , debris disks and chromospheric activity ) .
The star HD 101805 shows a peculiar wavelength dependence , indicating size distribution of scattering particles different from that of a typical interstellar medium .
Our high-S/N measurements of nearby stars with very low polarization also provide a useful dataset for calibration purposes .

Conclusions :