  The suitability of solar pores as magnetic wave guides has been a key topic
of discussion in recent years. Here we present observational evidence of
propagating magnetohydrodynamic wave activity in a group of five photospheric
solar pores. Employing data obtained by the Facility Infrared
Spectropolarimeter at the Dunn Solar Telescope, oscillations with periods on
the order of 5 minutes were detected at varying atmospheric heights by
examining Si I 10827 \r{A} line bisector velocities. Spectropolarimetric
inversions, coupled with the spatially resolved root mean square bisector
velocities, allowed the wave energy fluxes to be estimated as a function of
atmospheric height for each pore. We find propagating magnetoacoustic sausage
mode waves with energy fluxes on the order of 30 kW/m$^{2}$ at an atmospheric
height of 100 km, dropping to approximately 2 kW/m$^{2}$ at an atmospheric
height of around 500 km. The cross-sectional structuring of the energy fluxes
reveals the presence of both body- and surface-mode sausage waves. Examination
of the energy flux decay with atmospheric height provides an estimate of the
damping length, found to have an average value across all 5 pores of $L_d
\approx 268$km, similar to the photospheric density scale height. We find the
damping lengths are longer for body mode waves, suggesting that surface mode
sausage oscillations are able to more readily dissipate their embedded wave
energies. This work verifies the suitability of solar pores to act as efficient
conduits when guiding magnetoacoustic wave energy upwards into the outer solar
atmosphere.
