The kinematics of an old stellar population in the Large Magellanic Cloud - The CH stars

Details The kinematics of an old stellar population in the Large Magellanic Cloud - The CH stars The kinematics of an old stellar population in the Large Magellanic Cloud - The CH stars

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...334..135h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 1, 1988, p. 135-143. NSF-NSERC-supported research.

Other

46

Carbon Stars, Gas Dynamics, Magellanic Clouds, Radial Velocity, Stellar Motions, Globular Clusters, H I Regions, H Ii Regions

Scientific paper

The authors have obtained radial velocities for 39 CH stars in the LMC for the purpose of identifying a possible extended halo component. The stars were chosen as potential halo tracers in the LMC because Galactic CH stars show a high velocity dispersion perpendicular to the plane indicating an old population. The data suggest that it is reasonable to interpret the CH star velocities in terms of two kinematical components - a component with kinematics similar to those of the LMC planetaries (i.e., a rotating, flattened distribution which resembles the Galactic thick disk), and another component with lower systematic velocity which may be related in some way to the bar of the LMC.

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