Water isotopologues in the circumstellar envelopes of M-type AGB stars⋆
1 Department of Physics and AstronomyInstitute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
2 Onsala Space Observatory, Department of Earth and Space Sciences, Chalmers University of Technology, 439 92 Onsala, Sweden
3 Monash Centre for Astrophysics, School of Physics & Astronomy, Monash University, Victoria 3800, Australia
4 Research School of Astronomy & Astrophysics, the Australian National University, Canberra ACT 2611, Australia
Received: 14 November 2016
Accepted: 7 February 2017
Aims. In this study we intend to examine rotational emission lines of two isotopologues of water: H217O and H218O. By determining the abundances of these molecules, we aim to use the derived isotopologue – and hence oxygen isotope – ratios to put constraints on the masses of a sample of M-type AGB stars that have not been classified as OH/IR stars.
Methods. We have used detailed radiative transfer analysis based on the accelerated lambda iteration method to model the circumstellar molecular line emission of H217O and H218O for IK Tau, R Dor, W Hya, and R Cas. The emission lines used to constrain our models came from Herschel/HIFI and Herschel/PACS observations and are all optically thick, meaning that full radiative transfer analysis is the only viable method of estimating molecular abundance ratios.
Results. We find generally low values of the 17O/18O ratio for our sample, ranging from 0.15 to 0.69. This correlates with relatively low initial masses, in the range ~ 1.0 to 1.5 M⊙ for each source, based on stellar evolutionary models. We also find ortho-to-para ratios close to 3, which are expected from warm formation predictions.
Conclusions. The 17O/18O ratios found for this sample are at the lower end of the range predicted by stellar evolutionary models, indicating that the sample chosen had relatively low initial masses.
Key words: stars: AGB and post-AGB / circumstellar matter / stars: fundamental parameters
© ESO, 2017