We present mid-IR ( 19 – 37 \mu m ) imaging observations of S106 from SOFIA/FORCAST , complemented with IR observations from Spitzer /IRAC ( 3.6 – 8.0 \mu m ) , IRTF/MIRLIN ( 11.3 and 12.5 \mu m ) , and Herschel /PACS ( 70 and 160 \mu m ) .
We use these observations , observations in the literature , and radiation transfer modeling to study the heating and composition of the warm ( \sim 100 K ) dust in the region .
The dust is heated radiatively by the source S106 IR , with little contributions from grain-electron collisions and Ly- \alpha radiation .
The dust luminosity is \gtrsim ( 9.02 \pm 1.01 ) \times 10 ^ { 4 } ~ { } L _ { \odot } , consistent with heating by a mid- to late-type O star .
We find a temperature gradient ( \sim 75 - 107 K ) in the lobes , which is consistent with a dusty equatorial geometry around S106 IR .
Furthermore , the SOFIA observations resolve several cool ( \sim 65 - 70 K ) lanes and pockets of warmer ( \sim 75 - 90 K ) dust in the ionization shadow , indicating that the environment is fragmented .
We model the dust mass as a composition of amorphous silicates , amorphous carbon , big grains , very small grains , and PAHs .
We present the relative abundances of each grain component for several locations in S106 .