Abstract
ABSTRACT We present (R-I)KC photometry based on optical spectrophotometry, and JHK photometry for the carbon stars suspected of being CH stars discovered by Hartwick & Cowley (1988) in the field of the LMC. These carbon stars are shown to be more luminous than the red gian branch tip of the Galactic Population II giants and CH stars, and therefore are not members of the old stallar population in the LMC. The man bolometric magnitude for this sample is Mbol=5.3 while the brightest members reach Mbol=6.2. These carbon stars are significantly bluer and somewhat brighter in the mean than the LMC carbon stars disovered by Blanco et al. (1980). We argue that the luminosity and color distributions in htis paper, as well as the kinematic properties presented by Cowley & Hartwick (1991) are consistent with the association of this sample of carbon stars, possibly with ages near 108 years. The enhancement of resonance of s-processed elements as reported by Harwick & Cowley (1988) are reminiscent of the possible enhancements of these elements in Galactic N stars, and are consistent with the prediciton of the "third dredge-up" phase in the evolution of intermediate-mass AGB giants.
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