  The discovery of ubiquitous low-frequency (3-5mHz) Alfvenic waves in the
solar chromosphere (with Hinode/SOT), and corona (with CoMP and the Solar
Dynamics Observatory, SDO) has provided some insight into the non-thermal
energy content of the outer solar atmosphere. However, many questions remain
about the true magnitude of the energy flux carried by these waves. Here we
explore the apparent discrepancy in the resolved coronal Alfvenic wave
amplitude (~0.5km/s) measured by the Coronal Multi-channel Polarimeter (CoMP)
compared to those of the Hinode and the SDO near the limb (~20km/s). We use a
blend of observational data and a simple forward model of Alfvenic wave
propagation to resolve this discrepancy and determine the Alfvenic wave energy
content of the corona. Our results indicate that enormous line-of-sight
superposition within the coarse spatio-temporal sampling of CoMP hides the
strong wave flux observed by Hinode and SDO and leads to the large non-thermal
line broadening observed. While this scenario has been assumed in the past, our
observations with CoMP of a strong correlation between the non-thermal line
broadening with the low amplitude, low frequency Alfvenic waves observed in the
corona provide the first direct evidence of a wave-related non-thermal line
broadening. By reconciling the diverse measurements of Alfvenic waves we
establish large coronal non-thermal linewidths as direct signatures of the
hidden, or "dark", energy content in the corona, and provide preliminary
constraints on the energy content of the wave motions observed.
