| Description |
We plan to resolve the detailed physical and dynamical structure of the massive star forming (SF) region DR21virgulC which has a prominent bipolar outflow visible in 2 micron emission of vibrationally excited H2, tracing hot, shocked gas. While, the shock is hardly affecting most of the molecular line emission of the region (Lane et al. 1990, Ossenkopf et al. 2010), only CII is showing an additional broad blue wing indicating that the CII emission is not only originating from that warm gas, but also from the ionized wind in the blister outflow.H2 and CO are at least partly co-existent and hence should show similar signs of shocks, but surprisingly 13CO(10-9) doesn.t, so many question remains: - Is there any CO that is directly affected by the shock and if so, at at which AV does the shock excitation stop?- Why does CO up to 10-9 show no direct signature of shock heating or outflowing material?- Does the shock only affect H_2 and ionized material?- Which volume of the source is affected/heated by the shock?- Which volume of the source is heated by the UV radiation from the cluster?The aim of this proposal is to understand how shock/outflow and UV radiation from the embedded OB cluster contribute to the excitation of the surrounding material and where exactly the transition from shocked to unshocked material occurs. |
