SOFIA/FORCAST Observations of Warm Dust in S106: A Fragmented Environment

Abstract

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) × 10^4 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.

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