Spectropolarimetry of symbiotic stars: AG Draconis.

We present a series of spectropolarimetric observations of the symbiotic system AG Dra and focus on the polarization in the λ6825 and λ7082 lines, which are due to Raman scattering of OVI λλ1032,1038 emission. The polarization in the Raman lines is variable and the polarization angle shows periodic changes which are linked to the orbital motion even if the object goes into outburst. From the rotation in the line polarization angle, we find for the orbit inclination i=120° (105°-140°). This implies for a reasonable total mass of the binary system that the hot component's mass lies in the range 0.17-0.52M_sun_. This mass is rather low but not in real conflict with the interpretation that the hot component is a CO white dwarf and that the AG Dra system underwent in the past a Barium star type mass transfer episode. Our observations cover the 1994 outburst phase. During outburst the OVI radiation increased strongly while the Raman scattered radiation remained practically constant. This decrease in Raman efficiency is probably due to a reduction of available H^0^ scatterers as a consequence of the enlarged ionization during outburst. We detect intrinsic continuum polarization which is at least partly locked to the orbital motion and therefore also seems to be induced by a scattering process.