  Using the Subaru very deep K'-band imaging and HST WFPC2/NICMOS archival data
of the Hubble Deep Field North, we investigate the evolution of the stellar
mass, color, morphology of galaxies to z ~ 3. We mainly examine the rest-frame
U-V color distribution of galaxies as a function of stellar mass. At 0.3<z<2,
galaxies seem to be divided into the two populations at around the stellar mass
of ~5x10^9 M_solar. The low-mass galaxies have relatively bluer rest U-V color
and their color does not show clear correlation with stellar mass over the
range of 10^8-5x10^9 M_solar. On the other hand, at higher mass, the more
massive galaxies tend to have the redder U-V color. The average U-V color of
the low-mass galaxies becomes bluer gradually with redshift, from U-V ~ 0.2 at
z ~ 0.5 to U-V ~ -0.2 at z ~ 2. On the contrary, the correlation between the
stellar mass and rest U-V color of the high-mass population does not seem to
change significantly between z ~ 0.3 and z ~ 2. At z>2, it is seen that more
massive galaxies tend to have redder U-V color over the range of 10^9-10^10
M_solar. These results suggests that the star formation history of galaxies
depends on their stellar mass very much. The low-mass population is likely to
have relatively long star formation timescale. At the stellar mass larger than
~5x10^9 M_solar, there must be some mechanisms which suppress the star
formation in galaxies at 0<z<2.
