  We apply computational seismic holography to high-frequency helioseismic
observations of the quiet Sun from SDO/HMI to locate predominant sources of
seismic emission with respect to the structure of the solar granulation. The
regions of greatest seismic emission are the edges of photospheric granules.
Seismic emission from regions whose continuum brightnesses are 95-100% of the
mean, as resolved by HMI, are about 2.5 times as emissive as regions whose
brightnesses are 100-104% of the mean. The greater seismic emissivity from
regions whose brightnesses are somewhat less than the mean is roughly in line
with expectations from an understanding that attributes most seismic emission
to cool plumes plummeting from the edges of granules. However, seismic emission
from regions whose continuum brightnesses significantly exceed 104% of the mean
is also remarkably high. This unexpected feature of high-frequency seismic
emission from the solar granulation begs to be understood.
