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Maintained by LG |
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S106Klaus W. Hodapp Nicola Schneider To appear in Handbook of Star Forming Regions S106 is a bipolar nebula illuminated and excited by a central star called S106 IR. Depending on its distance (literature values range from 500 pc to 5.7 kpc) this is a late O to early B star. There is evidence that S106 is physically associated with the molecular cloud complex of Cygnus X. The bipolar nebula is the dominant feature in an embedded cluster of young stars forming in a molecular cloud. The bipolar morphology is visible from optical wavelengths into radio wavelengths, implying that it is not caused by foreground extinction. Instead, it is caused by the shadowing effect of a small disk surrounding the exciting star that projects into the surrounding molecular cloud and confines ionizing radiation to the lobes. With the discovery of new star formation sites in S106, i.e. YSOs in the S106 cluster, additional sub-clusters, the Class 0 source S106 FIR, and dense cold cores as reservoirs for new stars, S106 can nowadays be seen as a region of active star formation. This view revises earlier interpretations of radio and molecular line observations that saw S106 IR as a single massive protostar with a large accretion disk. |
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