Detection of Rotational Co Emission from the Red-Supergiants in the Large Magellanic Cloud
Paper in 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.
Author
M. Matsuura
Cardiff University
UCL
B. Sargent
Rochester Institute of Technology
B. Swinyard
Rutherford Appleton Laboratory
UCL
J. A. Yates
UCL
P. Royer
KU Leuven
M. J. Barlow
UCL
M. Boyer
NASA Goddard Space Flight Center
L. Decin
Astronomical Institute Anton Pannekoek
KU Leuven
Theo Khouri
Chalmers, Earth and Space Sciences, Onsala Space Observatory
M. Meixner
STScI
Johns Hopkins University
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 53-56978-2-7598-1907-2 (ISBN)
Subject Categories (SSIF 2011)
Astronomy, Astrophysics and Cosmology
Roots
Basic sciences
DOI
10.1051/eas/1571010
ISBN
978-2-7598-1907-2