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Detection of rotational CO emission from the red-supergiants in the Large Magellanic Cloud

Published online by Cambridge University Press:  27 October 2016

Mikako Matsuura ,
B. Sargent ,
Bruce Swinyard ,
J.A. Yates ,
P. Royer ,
M.J. Barlow ,
M.L. Boyer ,
L. Decin ,
Theo Khouri  and
Margaret Meixner
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Mikako Matsuura
Affiliation:
School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, UK University College London, London WC1E 6BT, UK
B. Sargent
Affiliation:
Center for Imaging Science and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 54 Lomb Memorial Drive, Rochester, NY 14623, USA
Bruce Swinyard
Affiliation:
University College London, London WC1E 6BT, UK Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire, OX11 0QX, UK
J.A. Yates
Affiliation:
University College London, London WC1E 6BT, UK
P. Royer
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D B-2401, 3001 Leuven, Belgium
M.J. Barlow
Affiliation:
University College London, London WC1E 6BT, UK
M.L. Boyer
Affiliation:
Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
L. Decin
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D B-2401, 3001 Leuven, Belgium Astronomical Institute Anton Pannekoek, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, The Netherlands
Theo Khouri
Affiliation:
Onsala Space Observatory, Dept. of Radio and Space Science, Chalmers University of Technology, 43992, Onsala, Sweden
Margaret Meixner
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA The Johns Hopkins University, Department of Physics and Astronomy, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA
J.Th. van Loon
Affiliation:
School of Physical & Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK
P.M. Woods
Affiliation:
Astrophysics Research Centre, School of Mathematics & Physics, Queen's University, University Road, Belfast BT7 1NN, UK
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Abstract

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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.

Keywords

(stars:) circumstellar matterstars: mass-lossstars: massiveISM: molecules(galaxies:) Magellanic Cloudsstars: AGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 459
Copyright
Copyright © International Astronomical Union 2016