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For the first time, we report a large-scale wave that was observedsimultaneously in the photosphere, chromosphere, transition region and lowcorona layers of the solar atmosphere. Using the high temporal and high spatialresolution observations taken by the Solar Magnetic Activity Research Telescopeat Hida Observatory and the Atmospheric Imaging Assembly (AIA) onboard SolarDynamic Observatory, we find that the wave evolved synchronously at differentheights of the solar atmosphere, and it propagated at a speed of 605 km/s andshowed a significant deceleration (-424 m/s2) in the extreme-ultraviolet (EUV)observations. During the initial stage, the wave speed in the EUV observationswas 1000 km/s, similar to those measured from the AIA 1700 {\AA} (967 km/s) and1600 {\AA} (893 km/s) observations. The wave was reflected by a remote regionwith open fields, and a slower wave-like feature at a speed of 220 km/s wasalso identified following the primary fast wave. In addition, a type-II radioburst was observed to be associated with the wave. We conclude that this waveshould be a fast magnetosonic shock wave, which was firstly driven by theassociated coronal mass ejection and then propagated freely in the corona. Asthe shock wave propagated, its legs swept the solar surface and therebyresulted in the wave signatures observed in the lower layers of the solaratmosphere. The slower wave-like structure following the primary wave wasprobably caused by the reconfiguration of the low coronal magnetic fields, aspredicted in the field-line stretching model.

Simultaneous Observations of a Large-Scale Wave Event in the Solar Atmosphere: From Photosphere to Corona