  Large-scale Extreme-ultraviolet (EUV) waves are frequently observed as an
accompanying phenomenon of flares and coronal mass ejections (CMEs). Previous
studies mainly focus on EUV waves with single wavefronts that are generally
thought to be driven by the lateral expansion of CMEs. Using high
spatio-temporal resolution multi-angle imaging observations taken by the Solar
Dynamic Observatory and the Solar Terrestrial Relations Observatory, we present
the observation of a broad quasi-periodic fast propagating (QFP) wave train
composed of multiple wavefronts along the solar surface during the rising phase
of a GOES M3.5 flare on 2011 February 24. The wave train transmitted through a
lunate coronal hole (CH) with a speed of 840 +/-67 km/s, and the wavefronts
showed an intriguing refraction effect when they passed through the boundaries
of the CH. Due to the lunate shape of the CH, the transmitted wavefronts from
the north and south arms of the CH started to approach each other and finally
collided, leading to the significant intensity enhancement at the collision
site. This enhancement might hint the occurrence of interference between the
two transmitted wave trains. The estimated magnetosonic Mach number of the wave
train is about 1.13, which indicates that the observed wave train was a weak
shock. Period analysis reveals that the period of wave train was $\sim$90
seconds, in good agreement with that of the accompanying flare. Based on our
analysis results, we conclude that the broad QFP wave train was a
large-amplitude fast-mode magnetosonic wave or a weak shock driven by some
non-linear energy release processes in the accompanying flare.
