Detection of rotational CO emission from the red-supergiants in the Large Magellanic Cloud. Issue Volume 11:Issue A29B(2015) (27th October 2016)

• Record Type: Journal Article
• Authors: Matsuura, Mikako; Sargent, B.; Swinyard, Bruce; Yates, J.A.; Royer, P.; Barlow, M.J.; Boyer, M.L.; Decin, L.; Khouri, Theo; Meixner, Margaret; van Loon, J.Th.; Woods, P.M.
• Editors: Benvenuti, Piero
• Is Part Of: Proceedings of the International Astronomical Union. Volume 11:Issue A29B(2015)
• Page Start: 459
• Page End: 459
• Publication Date: 2016-10-27
• Subjects: (stars:) circumstellar matter, -- stars: mass-loss, -- stars: massive, -- ISM: molecules, -- (galaxies:) Magellanic Clouds, -- stars: AGB and post-AGB; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921316005834
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: It is yet well understood how mass-loss rates from evolved stars depend on metallicities. With a half of the solar metallicity and the distance of only 50 kpc, the evolved stars of the Large Magellanic Cloud (LMC) are an ideal target for studying mass loss at low metallicity. We have obtained spectra of red-supergiants in the LMC, using the Hershel Space Observatory, detecting CO thermal lines fro J =6–5 up to 15–14 lines. Modelling CO lines with non-LTE Radiative transfer code suggests that CO lines intensities can be well explained with high gas-to-dust ratio, with no obvious reduction in mass-loss rate at the LMC. We conclude that the luminosities of the stars are primary factors on mass-loss rates, rather than the metallicity.