# Testing giant planet formation in the transitional disk of SAO 206462 using deep VLT/SPHERE imaging

## TL;DR

This study used high-contrast VLT/SPHERE imaging to search for giant planets in the transitional disk of SAO 206462, setting new detection limits that challenge some previous planet formation hypotheses.

## Contribution

First high-resolution, high-contrast imaging of SAO 206462's disk without post-processing biases, providing stringent constraints on the presence of giant planets and testing recent planet formation predictions.

## Key findings

- No close-in companions detected.
- Detection limits range from ~2-5 to ~4-7 Jupiter masses depending on disk parameters.
- Data do not support the existence of massive planets beyond 0.6 AU in the disk.

## Abstract

Context. The SAO 206462 (HD 135344B) disk is one of the few known transitional disks showing asymmetric features in scattered light and thermal emission. Near-infrared scattered-light images revealed two bright outer spiral arms and an inner cavity depleted in dust. Giant protoplanets have been proposed to account for the disk morphology. Aims. We aim to search for giant planets responsible for the disk features and, in the case of non-detection, to constrain recent planet predictions using the data detection limits. Methods. We obtained new high-contrast and high-resolution total intensity images of the target spanning the Y to the K bands (0.95-2.3 mic) using the VLT/SPHERE near-infrared camera and integral field spectrometer. Results. The spiral arms and the outer cavity edge are revealed at high resolutions and sensitivities without the need for image post-processing techniques, which introduce photometric biases. We do not detect any close-in companions. For the derivation of the detection limits on putative giant planets embedded in the disk, we show that the knowledge of the disk aspect ratio and viscosity is critical for the estimation of the attenuation of a planet signal by the protoplanetary dust because of the gaps that these putative planets may open. Given assumptions on these parameters, the mass limits can vary from ~2-5 to ~4-7 Jupiter masses at separations beyond the disk spiral arms. The SPHERE detection limits are more stringent than those derived from archival NaCo/L' data and provide new constraints on a few recent predictions of massive planets (4-15 MJ) based on the spiral density wave theory. The SPHERE and ALMA data do not favor the hypotheses on massive giant planets in the outer disk (beyond 0.6). There could still be low-mass planets in the outer disk and/or planets inside the cavity.