The ALMA detection of CO rotational line emission in AGB stars in the Large Magellanic Cloud

M.A.T. Groenewegen (Royal Obs. Belgium), W.H.T. Vlemmings (Chalmers Univ.), P. Marigo (Univ. of Padova), G.C. Sloan (Cornell, Univ. North Carolina, STScI), L. Decin (Univ. of Leuven), M.W. Feast (SAAO), S.R. Goldman (Keele Univ.), K. Justtanont (Chalmers Univ.), F. Kerschbaum (Univ. of Vienna), M. Matsuura (Cardiff Univ.), I. McDonald (Univ. of Manchester), H. Olofsson (Chalmers Univ.), R. Sahai (Caltech), P.R. Wood (ANU), A.A. Zijlstra (Univ. of Manchester), J. Bernard Salas (The Open Univ.), M.L. Boyer (STScI), L. Guzman-Ramirez (ESO, Leiden Univ.), O.C. Jones (STScI), E. Lagadec (Obs de la Cote d'Azur), M. Meixner (STScI), M.G. Rawlings (East Asian Obs.), & S. Srinivasan (ASIA-A)

2016, A&A, 596, 50

Full manuscript available locally (PDF) or from the arXiv (1609.09647).

Low- and intermediate-mass stars lose most of their stellar mass at the end of their lives on the asymptotic giant branch (AGB). Determining gas and dust mass-loss rates (MLRs) is important in quantifying the contribution of evolved stars to the enrichment of the interstellar medium. Attempt to, for the first time, spectrally resolve CO thermal line emission in a small sample of AGB stars in the Large Magellanic Cloud. The Atacama Large Millimeter Array was used to observe 2 OH/IR stars and 4 carbon stars in the LMC in the CO J= 2-1 line. We present the first measurement of expansion velocities in extragalactic carbon stars. All four C-stars are detected and wind expansion velocities and stellar velocities are directly measured. Mass-loss rates are derived from the DUSTY code modelling the spectral energy distribution and Spitzer/IRS spectrum. Gas-to-dust ratios are derived that make the predicted velocities agree with the observed ones. The expansion velocities and MLRs are compared to a Galactic sample of well-studied relatively low MLRs stars supplemented with “extreme” C-stars that have properties more similar to the LMC targets. Gas MLRs derived from a simple formula are significantly smaller than derived from the dust modelling, indicating an order of magnitude underestimate of the estimated CO abundance, time-variable mass loss, or that the CO intensities in LMC stars are lower than predicted by the formula derived for Galactic objects. This could be related to a stronger interstellar radiation field in the LMC. Although the LMC sample is small and the comparison to Galactic stars is nontrivial because of uncertainties in their distances (hence luminosities) it appears that for C stars the wind expansion velocities in the LMC are lower than in the solar neighbourhood, while the MLRs appear similar. This is in agreement with dynamical dust-driven wind models.

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