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Polarimetric interferometry is a method allowing the study of thedistribution of polarized flux at diffraction-limited resolution. Its basicobservable is the ratio $\mathcal{R}$ of the visibilities of the object in twoorthogonal polarizations. Here, we demonstrate how this observables can bemeasured with the SPeckle Polarimeter (SPP) of the 2.5-m telescope. The SPP isa combination of a dual-beam polarimeter and an EMCCD-based visible-rangespeckle interferometer. We propose a simple method for the correction of$\mathcal{R}$ for the instrumental polarization and polarization differentialaberrations of the telescope. The polarized intensity image can be estimatedfrom $\mathcal{R}$ under the assumption that the object is a point-likeunpolarized source plus a faint extended polarized envelope. The phase of$\mathcal{R}$ can be used for measurement of the polaroastrometric signal - thedifference between the photocentres of orthogonally polarized images of theobject. We investigate both possibilities using observations of unpolarizedstars and stars with a significant polarized circumstellar environment -$\mu$~Cep and RY~Tau.

Differential speckle polarimetry at Cassegrain and Nasmyth foci