OH/IR stars and their superwinds as observed by the Herschel Space Observatory ^⋆

¹ Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
e-mail: kay.justtanont@chalmers.se
² European Space Astronomy Centre, ESA, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
³ University College London, Dept. of Physics & Astronomy, Gower Street, London, WC1E 6BT, UK
⁴ Space Science and Technology Department, Rutherford Appleton Laboratory, Oxfordshire OX11 0QX, UK
⁵ SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
⁶ Sterrenkundig Instituut Anton Pannekoek, Universiteit van Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands

Received: 1 May 2013
Accepted: 7 June 2013

Abstract

Aims. In order to study the history of mass loss in extreme OH/IR stars, we observed a number of these objects using CO as a tracer of the density and temperature structure of their circumstellar envelopes.

Methods. Combining CO observations from the Herschel Space Observatory with those from the ground, we trace mass loss rates as a function of radius in five extreme OH/IR stars. Using radiative transfer modelling, we modelled the dusty envelope as well as the CO emission. The high-rotational transitions of CO indicate that they originate in a dense superwind region close to the star while the lower transitions tend to come from a more tenuous outer wind which is a result of the mass loss since the early AGB phase.

Results. The models of the circumstellar envelopes around these stars suggest that they have entered a superwind phase in the past 200–500 years. The low ¹⁸O/¹⁷O (~0.1 compared to the solar abundance ratio of ~5) and ¹²C/¹³C (3–30 cf. the solar value of 89) ratios derived from our study support the idea that these objects have undergone hot-bottom burning and hence that they are massive M ≥ 5  M_⊙ AGB stars.