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

November 2015 • 2015ApJ...814...54A

Authors • Adams, J. D. • Herter, T. L. • Hora, J. L. • Schneider, N. • Lau, R. M. • Staguhn, J. G. • Simon, R. • Smith, N. • Gehrz, R. D. • Allen, L. E. • Bontemps, S. • Carey, S. J. • Fazio, G. G. • Gutermuth, R. A. • Guzman Fernandez, A. • Hankins, M. • Hill, T. • Keto, E. • Koenig, X. P. • Kraemer, K. E. • Megeath, S. T. • Mizuno, D. R. • Motte, F. • Myers, P. C. • Smith, H. A.

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) × 10⁴ 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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Sean Carey

Senior Scientist