  In this paper, we report our multi-angle observations of the transverse
oscillation of a prominence and a filament induced by an EUV wave originating
from the farside of the Sun on 2014 September 1. The prominence oscillation was
simultaneously observed by both Atmospheric Imaging Assembly (AIA) onboard the
Solar Dynamics Observatory (SDO) spacecraft and Extreme-UltraViolet Imager
(EUVI) onboard the Behind Solar Terrestrial Relations Observatory (STEREO)
spacecraft. The speed of the shock travelling in the interplanetary space
exceeds that of the EUV wave, and the coronal dimming area experiences minimal
growth. This indicates that the shock wave is driven by the CME, while the EUV
wave freely propagates after the lateral motion of the CME flanks has stopped.
The observed oscillation direction of the prominence, determined through
three-dimensional reconstruction, further supports this point. Moreover, The
detailed investigation of the oscillations in the prominence and filament
induced by the EUV wave reveals initial amplitudes of 16.08 and 2.15 Mm,
periods of 1769 and 1863 s, damping time scales of 2640 and 1259 s, and damping
ratios of 1.49 and 0.68, respectively. The radial component of magnetic field,
as derived from the prominence and filament oscillation measurements, was
estimated to be 5.4 G and 4.1 G, respectively. In turn, utilizing the onset
times of both the prominence and filament oscillation, the average speeds of
the EUV wave are determined to be 498 km s$^{-1}$ and 451 km s$^{-1}$,
respectively.
