Detection of Rotational Co Emission from the Red-Supergiants in the Large Magellanic Cloud
Paper i proceeding, 2015

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 dominant factors on mass-loss rates, rather than the metallicity.


M. Matsuura

Cardiff University

University College London (UCL)

B. Sargent

Rochester Institute of Technology

B. Swinyard

Rutherford Appleton Laboratory

University College London (UCL)

J. A. Yates

University College London (UCL)

P. Royer

KU Leuven

M. J. Barlow

University College London (UCL)

M. Boyer

NASA Goddard Space Flight Center

L. Decin

KU Leuven

Anton Pannekoek Institute for Astronomy

Theo Khouri

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

M. Meixner

Johns Hopkins University

Space Telescope Science Institute (STScI)

J. T. van Loon

Keele University

P. M. Woods

Queen's University Belfast

EAS Publications Series

1633-4760 (ISSN) 1638-1963 (eISSN)

Vol. 71-72 53-56


Astronomi, astrofysik och kosmologi


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