  Small-scale, cyclic, transverse motions of plasma threads are usually seen in
solar prominences, which are often interpreted as magnetohydrodynamic (MHD)
waves. Here, we observed small-scale decayless transverse oscillations in a
quiescent prominence, and they appear to be omnipresent. The oscillatory
periods of the emission intensity and a proxy for the line-of-sight Doppler
shift are about half period of the displacement oscillations. This feature
agrees well with the fast kink-mode waves in a flux tube. All the moving
threads oscillate transversally spatially in phase and exhibit no significant
damping throughout the visible segments, indicating that the fast kink MHD
waves are persistently powered and ongoing dissipating energy is transferred to
the ambient plasma in the quiet corona. However, our calculations suggest that
the energy taken by the fast kink MHD waves alone can not support the coronal
heating on the quiet Sun.
