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J, H, and K' images are used to investigate the asymptotic giant branch (AGB)content of the Local Group dwarf elliptical galaxy NGC 205. The AGB on the (K,H-K) and (K, J-K) color-magnitude diagrams consists of two sequences: anear-vertical plume of giants with spectral types K and M, and a red armcontaining C stars. There are 320 C stars with M_bol < -4.1 and J-K > 1.5within 2 arcmin of the nucleus. C stars account for 10% of the integratedluminosity of AGB stars brighter than M_bol = -3.75 near the center of NGC 205,and this is in excellent agreement with what is measured in intermediate-ageclusters in the LMC. The most luminous AGB star has M_bol = -6.5, althoughvariability introduces an uncertainty of a few tenths of a magnitude when usingthis as an estimate of the AGB-tip brightness. Comparisons with models suggestthat the brightest AGB stars formed within the past 0.1 Gyr, and that theprevious episode of star formation occured a few tenths of a Gyr earlier. Theseresults are consistent with star formation in NGC 205 being triggered byinteractions with M31. These data also demonstrate that near-infrared imagingprovides an efficient means of identifying C stars in nearby galaxies.Comment: 16 pages of text; 8 postscript figures; will appear in Ap

The Asymptotic Giant Branch of NGC 205: The Characteristics of Carbon Stars and M Giants Identified fromJHK′ Images