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The Kinematics and Age of the Planetary Nebulae in the Large MagellanicCloud

Published online by Cambridge University Press:  25 April 2016

Stephen J. Meatheringham  and
Michael A. Dopita
Stephen J. Meatheringham
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
Michael A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
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Abstract

An HI survey of the Large Magellanic Cloud (LMC) has been reanalyzed to find the transverse velocity of the LMC, and derive an upper limit of 4.5 × 1011 M⊙ for the mass of our Galaxy out to 50 kpc. A rotation curve is derived for the LMC from the HI data giving a best mass estimate of (4.0±0.4)×109 M⊙. Velocity observations of 97 planetary nebulae (PN) in the Large Cloud are used to compare the old and young components. Our results are found to be at odds with an earlier sample of 9 old clusters, which is interpreted as being due to the low number of objects in that sample. The w-component of velocity dispersion of the PN population is 35 km s-1 and that of the HI 10 km s-1. If this difference is a result of stellar diffusion then the average age of the PN population is 1.3 × 109 yr, implying a precursor mass of 1.8 M⊙ and a remnant mass of 0.63 M⊙.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 6 , Issue 4 , 1986 , pp. 464 - 467
Copyright
Copyright © Astronomical Society of Australia 1985

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