Molecular gas in young debris disks

TL;DR

This study identifies and characterizes a second old, gas-rich debris disk similar to 49 Ceti, suggesting a potential new class of evolved circumstellar disks with significant molecular gas content.

Contribution

The discovery of a second 49 Ceti-like debris disk around HD21997, providing evidence for a new class of old, gas-bearing debris disks and challenging existing theories of disk evolution.

Findings

HD21997 is a 30 Myr old gas-rich debris disk.

Both HD21997 and 49 Ceti have extended disks with double-peaked CO profiles.

These disks may represent a new class of evolved gaseous debris disks.

Abstract

Gas-rich primordial disks and tenuous gas-poor debris disks are usually considered as two distinct evolutionary phases of the circumstellar matter. Interestingly, the debris disk around the young main-sequence star 49 Ceti possesses a substantial amount of molecular gas, and possibly represents the missing link between the two phases. Motivated to understand the evolution of the gas component in circumstellar disks via finding more 49 Ceti-like systems, we carried out a CO J=3-2 survey with Atacama Pathfinder EXperiment, targeting 20 infrared-luminous debris disks. These systems fill the gap between primordial and old tenuous debris disks in terms of fractional luminosity. Here we report on the discovery of a second 49 Ceti-like disk around the 30 Myr old A3-type star HD21997, a member of the Columba Association. This system was also detected in the CO(2-1) transition, and the reliable age determination makes it an even clearer example of an old gas-bearing disk than 49 Ceti. While the fractional luminosities of HD21997 and 49 Ceti are not particularly high, these objects seem to harbor the most extended disks within our sample. The double-peaked profiles of HD21997 were reproduced by a Keplerian disk model combined with the LIME radiative transfer code. Based on their similarities, 49 Ceti and HD21997 may be the first representatives of a so far undefined new class of relatively old (>~8 Myr), gaseous dust disks. From our results, neither primordial origin nor steady secondary production from icy planetesimals can unequivocally explain the presence of CO gas in the disk of HD21997.