CO gas inside the protoplanetary disk cavity in HD 142527: disk structure from ALMA

TL;DR

This study uses ALMA observations of CO isotopologues to analyze the gas distribution inside the large cavity of the protoplanetary disk around HD 142527, revealing residual gas and a smaller gas cavity than previously observed.

Contribution

It provides the first spatially and spectrally resolved measurements of gas inside the cavity, showing the gas mass, distribution, and a refined cavity size in HD 142527.

Findings

Residual gas mass inside cavity: 1.5-2 Jupiter masses

Gas cavity extends up to 105 au, smaller than dust cavity

Inclination angle of disk: 28 degrees

Abstract

Inner cavities and annular gaps in circumstellar disks are possible signposts of giant planet formation. The young star HD 142527 hosts a massive protoplanetary disk with a large cavity that extends up to 140 au from the central star, as seen in continuum images at infrared and millimeter wavelengths. Estimates of the survival of gas inside disk cavities are needed to discriminate between clearing scenarios. We present a spatially and spectrally resolved carbon monoxide isotopologue observations of the gas-rich disk HD 142527, in the J=2-1 line of 12CO, 13CO and C18O, obtained with the Atacama Large Millimeter Array (ALMA). We detect emission coming from inside the dust-depleted cavity in all three isotopologues. Based on our analysis of the gas in the dust cavity, the 12CO emission is optically thick, while 13CO and C18O emission are both optically thin. The total mass of residual gas inside the cavity is about 1.5-2 Jupiter masses. We model the gas with an axisymmetric disk model. Our best fit model shows that the cavity radius is much smaller in CO than it is in millimeter continuum and scattered light observations, with a gas cavity that does not extend beyond 105 au (at 3-sigma). The gap wall at its outer edge is diffuse and smooth in the gas distribution, while in dust continuum it is manifestly sharper. The inclination angle, as estimated from the high velocity channel maps, is 28+/-0.5 degrees, higher than in previous estimates, assuming a fix central star mass of 2.2 Solar masses.