  We observed the edge-on, planet-bearing disk of {\beta} Pictoris using T-ReCS
at Gemini to clarify and extend previous observations and conclusions about
this unique system. Our spectroscopy and spectral modeling of the 10-micron
silicate feature constrain the spatial distributions of three representative
dust components (0.1-micron/2.0-micron glassy olivine and crystalline
forsterite) across the inner 20-AU of the disk. We confirm that the 2.0-micron
glassy olivine is strongly peaked in the disk center and that the 0.1-micron
glassy olivine does not show this concentration, but rather is double peaked,
with the peaks on either side of the star. However, we do not see the strong
difference in brightness between those two peaks reported in a previous study.
Although the spatial distribution of the 0.1-micron dust is consistent with the
scenario of a dust-replenishing planetesimal belt embedded in the disk, we note
an alternative interpretation that can explain the spatial distributions of the
0.1-micron and 2.0-micron grains simultaneously and does not require the
planetesimal belt. In addition to the spectroscopy, we also obtained a new 11.7
micron image of the {\beta} Pic disk. By comparing this image with that
acquired in 2003, we confirm the existence and overall shape of the dusty clump
at 52 AU in the SW disk. We speculate that the clump's projected spatial
displacement of ~2.0 AU, a 3.6-{\sigma} result, between two epochs separated by
seven years is due to the Keplerian motion of the clump at an orbital radius of
$54.3^{+2.0}_{-1.2}$ AU.
