  For the first time, we report a large-scale wave that was observed
simultaneously in the photosphere, chromosphere, transition region and low
corona layers of the solar atmosphere. Using the high temporal and high spatial
resolution observations taken by the Solar Magnetic Activity Research Telescope
at Hida Observatory and the Atmospheric Imaging Assembly (AIA) onboard Solar
Dynamic Observatory, we find that the wave evolved synchronously at different
heights of the solar atmosphere, and it propagated at a speed of 605 km/s and
showed a significant deceleration (-424 m/s2) in the extreme-ultraviolet (EUV)
observations. During the initial stage, the wave speed in the EUV observations
was 1000 km/s, similar to those measured from the AIA 1700 {\AA} (967 km/s) and
1600 {\AA} (893 km/s) observations. The wave was reflected by a remote region
with open fields, and a slower wave-like feature at a speed of 220 km/s was
also identified following the primary fast wave. In addition, a type-II radio
burst was observed to be associated with the wave. We conclude that this wave
should be a fast magnetosonic shock wave, which was firstly driven by the
associated coronal mass ejection and then propagated freely in the corona. As
the shock wave propagated, its legs swept the solar surface and thereby
resulted in the wave signatures observed in the lower layers of the solar
atmosphere. The slower wave-like structure following the primary wave was
probably caused by the reconfiguration of the low coronal magnetic fields, as
predicted in the field-line stretching model.

Solar and Stellar Astrophysics