We present a comprehensive analysis of a bright, long duration (T 90 ∼ 257 s) GRB 110205A at redshift z = 2.22. The optical prompt emission was detected by Swif t/UVOT, ROTSE-IIIb and BOOTES telescopes when the GRB was still radiating in the γ-ray band, with optical lightcurve showing correlation with γ-ray data. Nearly 200 s of observations were obtained simultaneously from optical, Xray to γ-ray (1 eV -5 MeV), which makes it one of the exceptional cases to study the broadband spectral energy distribution during the prompt emission phase. In particular, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard synchrotron emission model in the fast cooling regime. Shortly after prompt emission (∼ 1100 s), 14.0) optical emission hump with very steep rise (α ∼ 5.5) was observed which we interpret as the the reverse shock emission. It is the first time that the rising phase of a reverse shock component has been closely observed. The full optical and X-ray afterglow lightcurves can be interpreted within the standard reverse shock (RS) + forward shock (FS) model. In general, the high quality prompt and afterglow data allow us to apply the standard fireball model to extract valuable information including the radiation mechanism (synchrotron), radius of prompt emission (R GRB ∼ 3 × 10 13 cm), initial Lorentz factor of the outflow (Γ 0 ∼ 250), the composition of the ejecta (mildly magnetized), as well as the collimation angle and the total energy budget.