  Whether BP Piscium (BP Psc) is either a pre-main sequence T Tauri star at d ~
80 pc, or a post-main sequence G giant at d ~ 300 pc is still not clear. As a
first-ascent giant, it is the first to be observed with a molecular and dust
disk. Alternatively, BP Psc would be among the nearest T Tauri stars with a
protoplanetary disk (PPD). We investigate whether the disk geometry resembles
typical PPDs, by comparing polarimetric images with radiative transfer models.
Our VLT/SPHERE/ZIMPOL observations allow us to perform Polarimetric
Differential Imaging; Reference Star Differential Imaging; and Richardson-Lucy
deconvolution. We present the first visible light polarization and intensity
images of the disk of BP Psc. Our deconvolution confirms the disk shape as
detected before, mainly showing the southern side of the disk. In polarized
intensity the disk is imaged at larger detail and also shows the northern side,
giving it the typical shape of high inclination flared disks. We explain the
observed disk features by retrieving the large-scale geometry with MCMax
radiative transfer modeling, which yields a strongly flared model, atypical for
disks of T Tauri stars.
