  We investigated the distribution of resolved asymptotic giant branch (AGB)
stars over a much larger area than covered by previous near-infrared studies in
the nearby dwarf elliptical galaxy NGC 205. Using data obtained with the WIRCam
near-infrared imager of the CFHT, we selected the AGB stars in the JHKs
color-magnitude diagrams, and separated the C stars from M-giant stars in the
JHKs color-color diagram. We identified 1,550 C stars in NGC 205 with a mean
absolute magnitude of M_Ks = -7.49 \pm 0.54, and colors of (J - Ks) = 1.81 \pm
0.41 and (H - Ks) = 0.76 \pm 0.24. The ratio of C stars to M-giant stars was
estimated to be 0.15 \pm 0.01 in NGC 205, and the local C/M ratios for the
southern 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 stars
and the red tail of the C stars. A comparison of the theoretical isochrone
models with the observed color distribution indicates that most of the bright
M-giant stars in NGC 205 were formed at log(t_yr) \sim 9.0-9.7. The logarithmic
slope of the M_Ks luminosity function for M-giant stars was estimated to be
0.84 \pm 0.01, which is comparable with dwarf elliptical galaxies NGC 147 and
NGC 185. Furthermore, we found that the logarithmic slopes of the M_Ks
luminosity function for C and M-giant stars are different to places, implying a
different star formation history within NGC 205. The bolometric luminosity
function for M-giant stars extends to M_bol = -6.0 mag, and that for C stars
spans -5.6 < M_bol < -3.0. The bolometric luminosity function of C stars is
unlikely to be a Gaussian distribution and the mean bolometric magnitude of C
stars is estimated to be M_bol = -4.24 \pm 0.55, which is consistent with our
results for dwarf elliptical galaxies NGC 147 and NGC 185.
