2015ApJ...814...54A

We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 µm), IRTF/MIRLIN (11.3 and 12.5 µm), and Herschel/PACS (70 and 160 µm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is ≳(9.02±1.01)x10⁴ L_☉, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼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 polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.