Variability and dust filtration in the transition disk J160421.7-213028 observed in optical scattered light

TL;DR

This study uses optical polarised light observations to analyze the structure and dust filtration in the transition disk J160421.7-213028, revealing a gap, an annulus, and a variable dip potentially caused by planet-disk interactions.

Contribution

First detailed optical polarimetric imaging of J160421.7-213028 revealing disk structures and dust filtration effects linked to embedded planets.

Findings

Detected a disk gap from 15 to 40 AU.

Observed a bright annulus at ~61 AU.

Identified a variable dip possibly caused by a planet or disk warp.

Abstract

Context. Some of transition disks show asymmetric structures in thermal sub-millimetre emission and optical scattered light. These structures can be the result of planet(s) or companions embedded in the disk. Aims. We aim to detect and analyse the scattered light of the transition disk J160421.7-213028, identify disk structures, and compare the results with previous observations of this disk at other wavelengths. Methods. We obtained and analysed new polarised intensity observations of the transition disk J160421.7-213028 with VLT/SPHERE using the visible light instrument ZIMPOL at $R'$ band (0.626$\mu$m). We probe the disk gap down to a radius of confidence of 0.1'' (${\sim}15$ AU at 145 pc). We interpret the results in the context of dust evolution when planets interact with the parental disk. Results. We observe a gap from 0.1 to 0.3'' (${\sim}15$ to 40AU) and a bright annulus as previously detected by HiCIAO $H$ band observations at $1.65\mu$m. The radial width of the annulus is around $40$AU, and its centre is at ${\sim}61$AU from the central star. The peak of the reflected light at 0.626$\mu$m is located 20 AU inward of the cavity detected in the submillimetre. In addition, we detect a dip at a position angle of ${\sim}46.2 \pm 5.4^\circ$. A dip was also detected with HiCIAO, but located at ${\sim}85^\circ$. If the dip observed with HiCIAO is the same, this suggests an average dip rotation of ${\sim}12^\circ/$year, which is inconsistent with the local Keplerian angular velocity of $\sim$0.8$^\circ$/yr at $\sim$61AU. Conclusions. The spatial discrepancy in the radial emission in J160421.7-213028 at different wavelengths is consistent with dust filtration at the outer edge of a gap carved by a massive planet. The dip rotation can be interpreted by fast variability of the inner disk and/or the presence of a warp or circumplanetary material of a planet at ${\sim}9.6$ AU.