!__Proposal-Section__ !6122 ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6122,v 8.1 1995/11/22 20:16:03 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Christian Ready ! Phone: 410 338-4546 , E-mail: ready@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Mon Dec 19 08:24:50 EST 1994 ! Proposal_Information ! Section 4 Title: High-Resolution Imaging of Shocks in 30 Doradus Proposal_Category: GO Scientific_Category: Interstellar Medium Cycle: 5 Investigators PI_name: You-Hua Chu PI_Institution: University of Illinois CoI_Name: Bart Wakker CoI_Institution: University of Illinois Contact: ! Y or N (designate at most one contact) CoI_Name: Sean Points CoI_Institution: University of Illinois Contact: ! Y or N (designate at most one contact) CoI_Name: Mordecai Mac Low CoI_Institution: University of Illinois Contact: ! Y or N (designate at most one contact) CoI_Name: Robert Kennicutt CoI_Institution: University of Arizona Contact: ! Y or N (designate at most one contact) CoI_Name: Chris Smith CoI_Institution: Cerro Tololo InterAmerican Obs Contact: ! Y or N (designate at most one contact) CoI_Name: Dominik Bomans CoI_Institution: Sternwarte der Universitaet Bonn Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) 30 Doradus in the Large Magellanic Cloud is the nearest giant H II region. It provides a unique opportunity to study the interactions between a large number of massive stars and the interstellar medium. It contains large shell structures that emit bright diffuse X-rays and show shocked material at DeltaV up to 300 kms. HST WFPC2 images only exist for the central 2min point5 of 30 Dor, where the interstellar and stellar conditions are vastly different from those in the supershells in outlying regions. Therefore, we request WFPC2 images of three of these shells in the H Alpha S II and O III emission lines. With the high spatial resolution we can for the first time image SNR shocks in superbubbles, study the cloudy medium of a giant H II region, map cloud-cloud collisions, model a supershell around a cluster, and search for circumstellar shells around massive stars. Questions ! Free format text (please update) Observing_Description: We were awarded three orbits for one target. We select Target 3 in our Phase I proposal. We will take WFPC2 images with 6 filters: three centered on nebular lines - F656N, F502N, and F673N, and three centered on stellar continumm - F336W, F555W, and F814W. The continuum images will be used to study stellar photometry and the line images will be used to study the physical structure of shocked gas and ioonization fronts. The exposure times are: F656N - 20 min with CR-SPLIT; F502N - 20 min with CR-SPLIT; F673N - 50 min with CR-SPLIT; F336W - 10 sec, 200 sec with CR-SPLIT; F555W - 4 sec, 40 sec, and 2x200 sec; F814W - 5 sec, 200 sec with CR-SPLIT. We want the PC centered on a small cluster and the WFC centered on a fast-expanding shell. Therefore, we want the PC to be at the north, and the chevron of the WFC to be pointing south. Exposure times were estimated using the description provided by Biretta (1994, personal communication) to obtain a desired S/N ratio of 3 per WFPC2 WF pixel. Exposure times of 20 minutes using filters F502N and F656N allow us to detect limiting emission measures of 1550 and 495 cm^-6 pc, respectively. This corresponds to fluxes of 2.9times10^-15 and 9.4times10^-16 erg cm^-2 sec^-1 arcsec^-2. An exposure time of 50 minutes with filter F673N allows us to detect down to an emission measure of 7000, 700, and 300 cm^-6 pc for assumed the S II to H Alpha\ ratio of 0.03, 0.3, and 0.7, respectively. Our analysis of flux-calibrated echelle data of 30 Dor (Chu and Kennicutt 1994) shows that the mean emission measures in this region are 19000 cm^-6 pc, and the shocked components have emission measures of a few 10^2 to a few 10^3. Thus, we will be able to observe the fainter structures in this region. 30 Dor can be observed in CVZ 2-3 times a year. If the observations are carried out in CVZ, we can make the observations more efficient. Real_Time_Justification: None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: NGC2070-NW-SHELL Alternate_Names: 30DOR-NW-SHELL Description: ISM, HII Region, SNR Position: ! Most common specification format is RA=5H 38M 17.0S +/- 0.37S, DEC=-69D 04' 02.0" +/- 5.0", PLATE-ID=06B0 Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=12.5 ! Include at least V and B-V B-V=-0.06 Comments: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ORIENTation 0D TO 10D ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN