| 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. |
