  PTFO 8-8695b (CVSO 30b) is a young planet candidate whose host star is a
$\sim$ 2.6 Myr-old T-Tauri star, and there have been continuous discussions
about the nature of this system. To unveil the mystery of this system, we
observed PTFO8-8695 for around five years at optical and infrared bands
simultaneously using Kanata telescope at the Higashi-Hiroshima Observatory.
Through our observations, we found that the reported fading event split into
two: deeper but phase-shifted "dip-A" and shallower but equiphase "dip-B".
These dips disappeared at different epochs, and then, dip-B reappeared. Based
on the observed wavelength dependence of dip depths, a dust clump and a
precessing planet are likely origins of dip-A and B, respectively. Here we
propose "a precessing planet associated with a dust cloud" scenario for this
system. This scenario is consistent with the reported change in the depth of
fading events, and even with the reported results, which were thought to be
negative evidence to the planetary hypothesis, such as the past non-detection
of the Rossiter-McLaughlin effect. If this scenario is correct, this is the
third case of a young (<3 Myr) planet around a pre-main sequence star. This
finding implies that a planet can be formed within a few Myr.
