A 2 au resolution view by ALMA of the planet-hosting WISPIT 2 disk

TL;DR

This study uses high-resolution ALMA observations to analyze the dust ring structure around WISPIT 2, setting constraints on circumplanetary emission and implications for the planet's influence on the disk.

Contribution

First high-resolution ALMA imaging of WISPIT 2's disk revealing a narrow dust ring and constraining circumplanetary emission near WISPIT 2b.

Findings

Detected a narrow dust ring at 144.4 au with 7.2 au width.

Ruled out bright point-like circumplanetary emission at WISPIT 2b's location.

WISPIT 2b is interior to the dust ring, suggesting additional companions or different planetary properties.

Abstract

We present deep, high spatial resolution interferometric observations of 0.88 mm continuum emission from the TYC 5709-354-1 system, hereafter WISPIT 2, obtained with the goal of detecting circumplanetary emission in the vicinity of the newly discovered WISPIT 2b planet. Observations with the most extended baseline configuration offered by ALMA, achieving an angular resolution of $25 \times 17$ mas ($3.3 \times 2.2$ au), revealed a single, narrow ring with a deprojected radius of 144.4 au and width of 7.2 au, and no evidence of circumplanetary emission within the cavity. Injection and recovery tests demonstrate that these observations can rule out point-like emission at the location of WISPIT 2b brighter than $\approx 45$ $\mu$Jy at the $3\sigma$ level. While these data can rule out PDS 70c like circumplanetary emission, the upper limit is consistent with empirical mass-flux relationships extrapolated from the stellar regime. Visibility modeling of the continuum ring confirms that WISPIT 2b lies significantly interior to the mm dust ring, raising doubts about the ability of WISPIT 2b to be the only driver of the dust structure. Possible solutions include either another lower mass companion, residing between WISPIT 2b and the cavity edge, likely in the gap seen by SPHERE at $\sim130$ au, or that WISPIT 2b is either substantially more massive than IR-photometry based estimates ($\sim15$ $M_{\rm Jup}$) or on a moderately eccentric orbit. The combination of observations sensitive to the gas and dust distributions on larger spatial scales and dedicated hydrodynamical modeling will help differentiate between scenarios.