  Solar pores are efficient magnetic conduits for propagating
magnetohydrodynamic wave energy into the outer regions of the solar atmosphere.
Pore observations often contain isolated and/or unconnected structures,
preventing the statistical examination of wave activity as a function of
atmospheric height. Here, using high resolution observations acquired by the
Dunn Solar Telescope, we examine photospheric and chromospheric wave signatures
from a unique collection of magnetic pores originating from the same decaying
sunspot. Wavelet analysis of high cadence photospheric imaging reveals the
ubiquitous presence of slow sausage mode oscillations, coherent across all
photospheric pores through comparisons of intensity and area fluctuations,
producing statistically significant in-phase relationships. The universal
nature of these waves allowed an investigation of whether the wave activity
remained coherent as they propagate. Utilizing bi-sector Doppler velocity
analysis of the Ca II 8542 {\AA} line, alongside comparisons of the modeled
spectral response function, we find fine-scale 5 mHz power amplification as the
waves propagate into the chromosphere. Phase angles approaching zero degrees
between co-spatial bi-sectors spanning different line depths indicate standing
sausage modes following reflection against the transition region boundary.
Fourier analysis of chromospheric velocities between neighboring pores reveals
the annihilation of the wave coherency observed in the photosphere, with
examination of the intensity and velocity signals from individual pores
indicating they behave as fractured wave guides, rather than monolithic
structures. Importantly, this work highlights that wave morphology with
atmospheric height is highly complex, with vast differences observed at
chromospheric layers, despite equivalent wave modes being introduced into
similar pores in the photosphere.
