Mid-infrared JWST spectra of carbon stars in the Large Magellanic Cloud

G.C. Sloan (STScI, UNC), B. Aringer (Uppsala Univ., Univ. Vienna), K.E. Kraemer (Boston College), J. Cami (Univ. of Western Ontario), K. Eriksson (Uppsala Univ.), S. Höfner (Uppsala Univ.), K. Justtanont (Chalmers Univ. of Tech.), E. Lagadec (Obs de la Côte d'Azur), P. Marigo (Univ. Padova), M. Matsuura (Cardiff Univ.), I. McDonald (Univ. Manchester), E.J. Montiel (U.S. Naval Obs.), R. Sahai (JPL), A.A. Zijlstra (Univ. of Manchester)

2026, ApJ, submitted

Full manuscript available locally (PDF)

Mid-infrared spectra from the Medium-Resolution Spectrometer on the James Webb Space Telescope have revealed the molecular chemistry of carbon stars in the Large Magellanic Cloud with better resolution and sensitivity than previously possible. Our sample spans a range of dust-production rates and includes three relatively dust-free semi-regular variables and six dustier Mira variables. All were observed 15-20 years earlier with the Infrared Spectrograph on the Spitzer Space Telescope at lower spectral resolution. The new spectra show that the C₃ molecule is responsible for a strong absorption band centered at 5.2 µm. CS is clearly present in some of the sample, especially the stars with less dust. HCN also appears to be present. Some of the spectra have changed significantly between the Spitzer epoch and the MRS observations in 2023 and 2024, and in most cases, these changes can be attributed to the stellar pulsation cycle. One exception is the disappearance of a dust emission feature at ~18 µm in one of the Miras. The new data identify a dip in the spectra centered at 10 µm, which could arise from either an unknown carrier or variable molecular emission to the red and blue. The presence of this spectral structure on the short-wavelength side of the SiC dust emission feature at ~11.3 µm combined with the broad C₂H₂ band centered at 14 µm raise the possibility that some previously reported detections of weak SiC dust emission in other carbon stars may not be real.

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Last modified 2 March, 2026. © Gregory C. Sloan and others.