29SiO and 30SiO J=1--0 maser signatures in Galactic AGB stars: the impact of third dredge up and turbulence velocity

TL;DR

This study catalogs 43 GHz SiO maser spectra dominated by isotopologue emission in AGB stars, linking these signatures to third dredge-up events and low turbulence velocities affecting maser pumping.

Contribution

It identifies and analyzes the rare iso-dom spectra in SiO masers, proposing a connection to stellar dredge-up processes and turbulence conditions.

Findings

35 iso-dom spectra identified, about 0.2% of SiO maser stars.

Iso-dom sources have bluer infrared colors than typical.

Enhanced isotopologue signatures linked to third dredge-up and low turbulence velocities.

Abstract

J=1--0 SiO masers at 43 GHz have a well-established distinctive signature in asymptotic giant branch (AGB) stars. 28SiO transitions typically dominate these spectra with the v=1 and v=2 emission being especially prominent and ubiquitous. Several predictions about enhanced 29SiO abundances in exotic stars prompt us to catalog the cases where 29SiO maser emission is enhanced compared to 28SiO. Our purpose is to catalog the known cases of 43 GHz spectra dominated by emission from isotopologue transitions (iso-dom spectra), to explore the commonalities in these sources, and to explain the cause of such maser signatures. Our catalog is drawn from SiO maser line ratios in the infrared-color-selected BAaDE survey and supplemented with a literature detection. The BAaDE catalog has cemented the typical signature of 43 GHz SiO masers, showing it is dominated by the v=1 and v=2 lines. Thirty-five iso-dom spectra are identified, meaning that this signature is seen in about 0.2% of our SiO maser-bearing stars. Their infrared colors are blue compared to other sources of the same period, similar to all sources displaying isotopologue masers. It is clear that the iso-dom nature of sources is variable, but unclear whether this is tied to stellar phase. A large abundance abnormality among the iso-dom sources is disfavored as the iso-dom sources do not appear significantly different from other stars which host isotopologue masers. Maser pumping, affecting the population inversions of specific transitions, can instead explain the enhanced signatures. We posit that iso-dom spectra appear in AGB stars which have undergone third-dredge up (enhancing the 29SiO and 30SiO abundance slightly) and which, in addition, are experiencing very low turbulence velocity (<1 km/s), creating a line overlap which pumps the maser transitions very efficiently.