CO rotational line emission in very red carbon stars in the Magellanic Clouds

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Abstract
Stars of low and intermediate initial mass lose most of their stellar mass at the end of their lives during the asymptotic giant branch (AGB) phase. Determining their gas and dust mass-loss rates (MLRs) is crucial for quantifying the contribution of evolved stars to the life cycle of dust and gas in the Universe. The Atacama Large Millimeter/submillimeter Array was used to observe 38 carbon stars (C stars) in the large Magellanic cloud (LMC) and three C stars in the small Magellanic cloud (SMC) in the CO J= 2–1 line. Line profiles were fitted to derive stellar velocities and wind-expansion velocities ( V exp ). CO emission is detected in two C stars in the SMC and 33 C stars in the LMC, extending earlier work from 2016 that detected CO emission from a total of four C stars observed in the LMC. This is the first detection of carbon monoxide around an AGB star in the SMC. One object in the LMC shows emission in 13 CO. The windexpansion velocity ranges from ∼7.5 to ∼30 km s −1 . Archival data were used to determine the pulsation periods as well as construct and model the spectral energy distributions using two dust radiative transfer codes. Mass-loss rates were independently derived from these two codes as well as from the intensity of the CO line, using a simple formula. On average, the dust-based MLRs higher than the MLRs based on the CO line by a factor of 1.6. Additional CO data in other transitions, combined with proper modelling, is required to further investigate this possible discrepancy. Mass-loss rates, pulsation periods, and expansion velocities were compared to a sample of Galactic C stars. There is a strong bias, as the Magellanic Cloud targets sample the highest MLRs and luminosities, yet they represent only a minority of stars in a Galactic sample. Comparing this sample with a similarly extreme set of Galactic stars with periods longer than 500 days, we identify no correlation between metallicity and either the MLR or V exp .

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