  The temporal behavior of the very dim optical afterglow of GRB 080503 is at
odds with the regular forward shock afterglow model and a sole kilonova
component responsible for optical emission has been speculated in some
literature. Here we analyze the optical afterglow data available in archive and
construct time-resolved spectra. The significant detection by Keck-I in {\it
G/R} bands at $t\sim 3$ day, which has not been reported before, as well as the
simultaneous Gemini-North {\it r} band measurement, are in favor of a power-law
spectrum that is well consistent with the optical to X-ray spectrum measured at
$t\sim 4.5$ day. However, for $t\leq 2$ day, the spectra are thermal-like and a
straightforward interpretation is a kilonova emission from a neutron star
merger, making it, possibly, the first detection of a very early kilonova
signal at $t\sim 0.05$ day. A non-thermal nature of optical emission at late
times ($t\sim 2$ day), anyhow, can not be ruled out because of the large
uncertainty of the {\it g}-band data. We also propose to classify the neutron
star merger induced optical transients, according to the temporal behaviors of
the kilonova and the non-thermal afterglow emission, into four types. GRB
080503 would then represent the first observation of a sub-group of neutron
star merger driven optical transients (i.e., Type IV) consisting of an early
blue kilonova and an adjacent non-thermal afterglow radiation.
