  The early optical emission of the moderately high redshift ($z=3.08$) GRB
060607A shows a remarkable broad and strong peak with a rapid rise and a
relatively slow power-law decay. It is not coincident with the strong
early-time flares seen in the X-ray and gamma-ray energy bands. There is weak
evidence for variability superposed on this dominant component in several
optical bands that can be related to flares in high energy bands. While for a
small number of GRBs, well-sampled optical flares have been observed
simultaneously with X-ray and gamma ray pulses, GRB 060607A is one of the few
cases where the early optical emission shows no significant evidence for
correlation with the prompt emission. In this work we first report in detail
the broad band observations of this burst by Swift. Then by applying a simple
model for the dynamics and the synchrotron radiation of a relativistic shock,
we show that the dominant component of the early emissions in optical
wavelengths has the same origin as the tail emission produced after the main
gamma ray activity. The most plausible explanation for the peak in the optical
light curve seems to be the cooling of the prompt after the main collisions,
shifting the characteristic synchrotron frequency to the optical bands. It
seems that the cooling process requires a steepening of the electron energy
distribution and/or a break in this distribution at high energies. The sharp
break in the X-ray light curve at few thousands of seconds after the trigger,
is not observed in the IR/optical/UV bands, and therefore can not be a jet
break. Either the X-ray break is due to a change in the spectrum of the
accelerated electrons or the lack of an optical break is due to the presence of
a related delayed response component (Abbreviated).
