2024A&A...683A..18M

Context. Many reflected light images of protoplanetary disks have been obtained with ground-based high-contrast instruments. Quantitative measurements of the reflected radiation provide strong constraints on the scattering dust which can clarify the dust particle evolution in these disks and the composition of the forming planets.
Aims. We derived the wavelength dependence of the polarized reflectivity ${\left( {{{\hat Q}_\varphi }/{I_ \star }} \right)_\lambda }$ or color for a sample of disks to contrain the dust based on these data. Further we searched for systematic differences in the dust properties between subgroups of disks.
Methods. We selected from the ESO archive polarized imaging for 11 protoplanetary disks obtained at visible and near-infrared wavelengths with the SPHERE/ZIMPOL and SPHERE/IRDIS high contrast instruments. All disks have bright and well-resolved structures, such as rings or spirals, which allow accurate determinations of the intrinsic polarized reflectivity ${{\hat Q}_\varphi }/{I_ \star }$ at multiple wavelengths. For this, we corrected the observations for the smearing effects caused by the point spread functions (PSFs) of the individual dataset with a novel correction procedure applicable to inclined disks. For the 11 disks, we derived a total of 31 ${{\hat Q}_\varphi }/{I_ \star }$ values for wavelengths from 0.62 μm (R band) to 2.2 μm (Ks band) and compared our results, if possible, with previous determinations. For each disk, we derived a polarized reflectivity color η_V/IR between a visible band λ < 1 μm and a near-IR band λ > 1 μm and other wavelength combinations. We also consider model calculations for the polarized reflectivity colors η for protoplanetary disks to constrain the scattering properties of the dust.
Results. The polarized reflectivities for the investigated disks structures are at a typical level between Q_φ/I_★ ∼ 0.1% to 1.0%. These values depend strongly on the observing conditions and a correction for the PSF smearing effects is essential to obtain the intrinsic values ${{\hat Q}_\varphi }/{I_ \star }$. Corrected values ${{\hat Q}_\varphi }/{I_ \star }$ are on average about a factor of 1.6 higher than the observed values. We checked the accuracy of the PSF calibrations procedure with simulations and literature data, and show that the large systematic errors in the observational values are reduced to a relative level ${\rm{\Delta }}{{\hat Q}_\varphi }/{{\hat Q}_\varphi } \approx 10{\rm{\% }}$ or even less. The high accuracy yields wavelength gradients for the polarized reflectivity ${\left( {{{\hat Q}_\varphi }/{I_ \star }} \right)_\lambda }$ or colors η which are significantly different between different objects. We find in our sample for all disks around Herbig stars (HD 169142, HD 135344B, HD 100453, MWC 758, and HD 142527) a red color η_v/IR > 0.5, while four out of six disks around T Tauri stars (PDS 70, TW Hya, RX J1615, and PDS 66) are gray -0.5 < η_V/IR < 0.5. The red colors support the presence of rather compact dust grains, while the absence of blue colors (except for the near-infrared color of PDS 66) is not compatible with very porous aggregates composed of small monomers. We suspect, that the very red colors η_V/IR ≈ 2 obtained for LkCa 15 and MWC 758 could be the result of an "extra" reddening of the radiation illuminating the disk caused by absorbing hot dust near the star. We discuss the prospects of further improvements for the derivation of dust properties in these disks if the fractional polarization 〈p_ψ〉 or other parameters of the reflected light are also taken into account in future studies.