  We analyze data from the Helioseismic Magnetic Imager (HMI) and the
Atmospheric Imaging Assembly (AIA) instruments on board the Solar Dynamics
Observatory (SDO) to characterize the spatio-temporal acoustic power
distribution in active regions as a function of the height in the solar
atmosphere. For this, we use Doppler velocity and continuum intensity observed
using the magnetically sensitive line at 6173 \AA\ as well as intensity at 1600
\AA\ and 1700 \AA. We focus on the power enhancements seen around AR 11330 as a
function of wave frequency, magnetic field strength, field inclination and
observation height. We find that acoustic halos occur above the acoustic cutoff
frequency and extends up to 10 mHz in HMI Doppler and AIA 1700 \AA\
observations. Halos are also found to be strong functions of magnetic field and
their inclination angle. We further calculate and examine the spatially
averaged relative phases and cross-coherence spectra and find different wave
characteristics at different heights.
