  We present an estimation of lifetimes of massive galaxies with distinct UV
colors at $0.5 \le z \le 2.5$ in the COSMOS/UltraVISTA field. After dividing
the galaxy sample into subsamples of red sequence (RS), blue cloud (BC), and
green valley (GV) galaxies in different redshift bins, according to their
rest-frame extinction-corrected UV colors, we derive their lifetimes using
clustering analyses. Several essentials that may influence the lifetime
estimation have been explored, including the dark matter (DM) halo mass
function (HMF), the width of redshift bin, the growth of DM halos within each
redshift bin, and the stellar mass. We find that the HMF difference results in
scatters of $\sim0.2$ dex on lifetime estimation; adopting a redshift bin width
of $\Delta z = 0.5$ is good enough to estimate the lifetime; and no significant
effect on lifetime estimation is found due to the growth of DM halos within
each redshift bin. The galaxy subsamples with higher stellar masses generally
have shorter lifetimes; however, the lifetimes among different subsamples at z
> 1:5 tend to be independent of stellar mass. Consistently, the
clustering-based lifetime for each galaxy subsample agrees well with that
inferred using the spectral energy distribution modeling. Moreover, the
lifetimes of the RS and BC galaxies also coincide well with their typical gas
depletion timescales attributed to the consumption of star formation.
Interestingly, the distinct lifetime behaviors of the GV galaxies at $z \le
1.5$ and $z>1.5$ can not be fully accounted for by their gas depletion
timescales. Instead, this discrepancy between the lifetimes and gas depletion
timescales of the GV galaxies suggests that there are additional physical
processes, such as feedback of active galactic nuclei, accelerating the
quenching of GV galaxies at high redshifts.
