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We observed the edge-on, planet-bearing disk of {\beta} Pictoris using T-ReCSat Gemini to clarify and extend previous observations and conclusions aboutthis unique system. Our spectroscopy and spectral modeling of the 10-micronsilicate feature constrain the spatial distributions of three representativedust components (0.1-micron/2.0-micron glassy olivine and crystallineforsterite) across the inner 20-AU of the disk. We confirm that the 2.0-micronglassy olivine is strongly peaked in the disk center and that the 0.1-micronglassy 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 strongdifference in brightness between those two peaks reported in a previous study.Although the spatial distribution of the 0.1-micron dust is consistent with thescenario of a dust-replenishing planetesimal belt embedded in the disk, we notean alternative interpretation that can explain the spatial distributions of the0.1-micron and 2.0-micron grains simultaneously and does not require theplanetesimal belt. In addition to the spectroscopy, we also obtained a new 11.7micron image of the {\beta} Pic disk. By comparing this image with thatacquired in 2003, we confirm the existence and overall shape of the dusty clumpat 52 AU in the SW disk. We speculate that the clump's projected spatialdisplacement of ~2.0 AU, a 3.6-{\sigma} result, between two epochs separated byseven years is due to the Keplerian motion of the clump at an orbital radius of$54.3^{+2.0}_{-1.2}$ AU.

The Mineralogy and Structure of the Inner Debris Disk of {\beta} Pictoris