0 Assigned ID: 617 ----- Attempting Submission 1 (Fri Apr 07 16:24:30 GMT 2017) ----- HST Phase I Proposal 617 (hh7-11.apt) successfully submitted. Receipt: # 617-1 POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. Really like the Aladdin interface, well done. Helps so much with ORIENTs 1645164946 ----- Attempting Submission 1 (Mon Jul 10 21:49:04 GMT 2017) ----- The warning refers to dithers moving the desired targets to the vignette area of the quad filter. The dithers we chose are small enough that this is not an issue. We have verified that the areas of interest all lie within the unvignetted portion of the quadrant. Proper Motions, Shear, Mass-Loss Rates and C-Shocks in the HH 7-11 Jet We propose to obtain the first complete set of narrow band HST images of the iconic HH 7-11 protostellar jet. Owing to positional errors, both previous attempts to image the system failed to capture the HH 7 bow shock, arguably the best example we have of a well-resolved, strong shock in molecular gas. The proposed observations will tie together the optical and the IR emission in HH 7 and establish whether the molecular gas is heated by a continuous shock or a jump shock, physics of direct relevance to upcoming JWST observations of protostars. HST is needed to measure proper motions, to detect offsets between H-alpha and the forbidden lines that define the directions of shock propagation throughout the flow, and to resolve small scale structures present in the previous images. The portions of the jet imaged in 1995 and 1998 show several curious features, including two `rings' that may result from the jet penetrating through preexisting sheets or filaments. I f this explanation is correct, the shocks in the rings will have expanded perpendicular to the axis of the jet by measurable amounts in the last 20 years. Any shear or entrainment along the jet will manifest itself as differential motions in the shocked gas. Our proposal employs a WFC3 quad filter to measure electron densities at each pixel. Combined with proper motion measurements, these observations will allow us to separate jet material from shocked gas along the cavity, observe dynamical instabilities if they exist behind the shock, and assess the accuracy of simple mass loss calculations that depend solely upon integrated line luminosities. New images in F656N, F631N, F673N will be used in part to define proper motions relative to their counterparts taken as part of GTO 6868 in 1998, and GTO 5779 in 1995. Two orbits in each filter are needed to reach the same depth as the GTO data. The near-IR continuum image was quite useful for identifying cavities in Fig 1, so we would like to redo that as well to see if the cavities have changed. Finally, we plan to use the standard [S II] 6716/ [S II] 6731 line ratio to determine electron densities. Ground-based spectra integrated over the emission imply Ne ranges between about 200 and 1500 cm-3, within the range of the [S II] density diagnostic. The F673N filter includes both [S II] 6716 and [S II] 6731, so to isolate [S II] 6716 (and extract [S II] 6731 from the difference) we propose to use the quad filter FQ672N. This filter has a smaller FOV, but it is just large enough to include all the emission. Stellar Physics 6 false false false false false false SUPPORTED ISM HERBIG-HARO OBJECT JET SHOCK FRONT YES This object was generated by the targetselector and retrieved from the SIMBAD database. 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