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We investigated the distribution of resolved asymptotic giant branch (AGB)stars over a much larger area than covered by previous near-infrared studies inthe nearby dwarf elliptical galaxy NGC 205. Using data obtained with the WIRCamnear-infrared imager of the CFHT, we selected the AGB stars in the JHKscolor-magnitude diagrams, and separated the C stars from M-giant stars in theJHKs color-color diagram. We identified 1,550 C stars in NGC 205 with a meanabsolute magnitude of M_Ks = -7.49 \pm 0.54, and colors of (J - Ks) = 1.81 \pm0.41 and (H - Ks) = 0.76 \pm 0.24. The ratio of C stars to M-giant stars wasestimated to be 0.15 \pm 0.01 in NGC 205, and the local C/M ratios for thesouthern region are somewhat lower than those for the northern region. The (J -Ks) color distributions of AGB stars contain the main peak of the M-giant starsand the red tail of the C stars. A comparison of the theoretical isochronemodels with the observed color distribution indicates that most of the brightM-giant stars in NGC 205 were formed at log(t_yr) \sim 9.0-9.7. The logarithmicslope of the M_Ks luminosity function for M-giant stars was estimated to be0.84 \pm 0.01, which is comparable with dwarf elliptical galaxies NGC 147 andNGC 185. Furthermore, we found that the logarithmic slopes of the M_Ksluminosity function for C and M-giant stars are different to places, implying adifferent star formation history within NGC 205. The bolometric luminosityfunction for M-giant stars extends to M_bol = -6.0 mag, and that for C starsspans -5.6 < M_bol < -3.0. The bolometric luminosity function of C stars isunlikely to be a Gaussian distribution and the mean bolometric magnitude of Cstars is estimated to be M_bol = -4.24 \pm 0.55, which is consistent with ourresults for dwarf elliptical galaxies NGC 147 and NGC 185.

Near-infrared properties of asymptotic giant branch stars in nearby dwarf elliptical Galaxy NGC 205