Constraining wave propagation throughout the solar atmosphere with IBIS, ALMA and IRIS

The heating mechanism of the solar chromosphere is still an open scientific question. We present observational constraints on the high-frequency (acoustic) wave contribution to the chromospheric heating. We utilize a unique combination of observations from NSO's Dunn Solar Telescope and the Atacama Large Millimeter Array obtained on April 23rd 2017 to estimate the high-frequency wave flux in the lower solar atmosphere. We extend this study to the upper chromosphere and the transition region with archival IRIS data. We infer the wave flux through comparison of the observations with synthetic observables from the time-dependent hydrodynamic RADYN code. Our findings are able to constrain the wave flux at higher altitudes in the solar atmosphere than previous works using similar approaches. Furthermore, the different diagnostics we use form at different heights, which allow us to explore the propagation and dissipation of waves with height. We will discuss future plans to extend this work with more advanced modeling and additional observations with the upcoming Innoue Solar Telescope (DKIST).