# A Close-up View of the Young Circumbinary Disk HD 142527

## TL;DR

This study uses ALMA observations to analyze the structure and dynamics of the young circumbinary disk HD 142527, revealing dust and gas asymmetries, potential dust trapping, and a possible third companion within the cavity.

## Contribution

First detailed ALMA analysis of dust and gas distribution in HD 142527, highlighting dust trapping and potential third companion detection.

## Key findings

- High azimuthal contrast in dust and gas density
- Radial Gaussian profiles for gas and dust surface densities
- Detection of a possible third companion within the cavity

## Abstract

We present ALMA observations of the 0.88 millimeter dust continuum, 13CO, and C18O J=3-2 line emission of the circumbinary disk HD142527 at a spatial resolution of about 0.25". This system is characterized by a large central cavity of roughly 120 AU in radius, and asymmetric dust and gas emission. By comparing the observations with theoretical models, we find that the azimuthal variations in gas and dust density reach a contrast of 54 for dust grains and 3.75 for CO molecules, with an extreme gas-to-dust ratio of 1.7 on the dust crescent. We point out that caution is required in interpreting continuum subtracted maps of the line emission as this process might result in removing a large fraction of the line emission. Radially, we find that both the gas and dust surface densities can be described by Gaussians, centered at the same disk radius, and with gas profiles wider than for the dust. These results strongly support a scenario in which millimeter dust grains are radially and azimuthally trapped toward the center of a gas pressure bump. Finally, our observations reveal a compact source of continuum and CO emission inside the dust depleted cavity at about 50 AU from the primary star. The kinematics of the CO emission from this region is different from that expected from material in Keplerian rotation around the binary system, and might instead trace a compact disk around a third companion. Higher angular resolution observations are required to investigate the nature of this source.