Polarimeters have resolved dozens of protoplanetary disks in polarized intensities. Disks that exhibit variable illuminations in the outer regions provide new means of investigating the innermost...Show morePolarimeters have resolved dozens of protoplanetary disks in polarized intensities. Disks that exhibit variable illuminations in the outer regions provide new means of investigating the innermost regions and give valuable insight on physical processes inherent in terrestrial planet formation. The PDS 66 has a close to face-on view of its disk which inhabits ring- and gab-like structures. In this research, we further investigated these tructures by using SPHERE/IRDIS polarimetric differential imaging in H- and J band to obtain the Stokes Q, U, and I image. We linked earlier found rotational timescale of roughly 22 years to a Jupiter mass-like planet in the inner disk, but we need new observations to exclude timescales shorter than our two year baseline. In addition, we probed the dust content by fitting an adjusted Henyey-Greenstein model to the scattering phase function and found a difference in g values and polarization fractions at 90 scattering angles for the north and south side of the disk at gnorth = 0.22, pnorth = 16.33, gsouth = 0.15, and psouth = 13.49. These results, in combination with an enhanced surface brightness of 30% in the north relative to the south side of the disk at scattering angles of 90, suggest an asymmetric particle distribution throughout the disk. We further confirmed literature results on the inclination and position angle of the outer ring and found a stello-centric offset of 49.8 mas, which contradicts expectations in previous literatureShow less
Context. Much data from the integral field spectroscope (IFS) of SPHERE, the high contrast imager of the VLT, of circumstellar disks is yet unpublished, since this data is always collected in...Show moreContext. Much data from the integral field spectroscope (IFS) of SPHERE, the high contrast imager of the VLT, of circumstellar disks is yet unpublished, since this data is always collected in parallel with IRDIS, which is much easier to reduce and analyze. Aims. We search for a good and reliable way to reduce raw IFS data and study the effects of different post-processing methods on the morphology of protoplanetary disks. Methods. We used the common pipeline of ESO to reduce spatially resolved spectral IFS data (YJ band) of RXJ1615.3-3255 and applied classical ADI, classical SDI and classical RDI on the data. Results. We detected a ring, an arc and an inner disk component in both the ADI and SDI image, the ring is detected in the RDI image as well. We conclude that we can trust the SDI data the best around the minor axis of the ring since ADI and RDI have to deal with self-subtraction and over subtraction in that region, the other parts of the ring can be trusted the best in the ADI and RDI data. The disk signal appears to be red, but further research is needed to conclude whether this effect is astrophysical or not.Show less
