The kinematics of the Small Magellanic Cloud from its field carbon stars

Details The kinematics of the Small Magellanic Cloud from its field carbon stars The kinematics of the Small Magellanic Cloud from its field carbon stars

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...344..210h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 344, Sept. 1, 1989, p. 210-216. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

48

Carbon Stars, Kinematics, Magellanic Clouds, Charge Coupled Devices, Mass To Light Ratios, Planetary Nebulae, Radial Velocity, Star Distribution

Scientific paper

The present velocity survey observed 150 carbon stars in the SMC in the near-IR with an individual precision of + or - 1.8 km/sec. Carbon stars are found to behave kinematically like the planetary nebulae system with which they share a velocity dispersion of about 27 km/sec; they also exhibit the same velocity dispersion as a sample of halo metal-poor giants near NGC 121. The carbon stars and planetary nebulae may belong to a spheroidal system, and indications are found of streaming motions in the wing section between the SMC and LMC.

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