! File: 2292C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:04:46:51 coverpage: title_1: YOUNG SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS title_2: AND NUCLEOSYNTHESIS IN MASSIVE STARS sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO pi_title: DR. pi_fname: MICHAEL pi_mi: A. pi_lname: DOPITA pi_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES pi_country: AUSTRALIA pi_phone: (011 61) 62 490212 keywords_2: ABUNDANCE, SPECTRAL REGIONS: OPTICAL, UV,SUPERNOVAE: TYPE II hours_pri: 5.00 num_pri: 2 wf_pc: Y foc: Y pi_position: SENIOR FELLOW off_fname: ALEX off_mi: W. off_lname: RODGERS off_title: DIRECTOR off_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES off_addr_1: PRIVATE BAG off_addr_2: WODEN P.O. off_city: WODEN off_state: ACT off_zip: 2606 off_country: AUSTRALIA off_phone: (011 61) 62 490262 off_telex: AA62270 ! end of coverpage abstract: line_1: The young supernova remnants (YSNR) present a unique line_2: opportunity to directly observe the end-points of stellar line_3: evolution. The peculiar spectra of the oxygen-rich type line_4: undoubtedly result from the reheating of material ejected line_5: from deep within the core of a massive progenitor star. This line_6: material is not very well-mixed, so that the spectra of line_7: individual knots can be used to probe the chemical line_8: composition of the region of the progenitor star where they line_9: were produced. Galactic examples of this class are heavily line_10: reddened, so that UV spectroscopy will be difficult. This line_11: proposal is to observe those YSNR in the Magellanic Clouds line_12: which were discovered by us. By imaging with the WF/PC and line_13: by later UV spectroscopy with the FOS, we intend to line_14: determine the excitation mechanism, chemical abundances, line_15: and the chemical stratification in the supernova ejecta. ! ! end of abstract general_form_proposers: lname: BENVENUTI fname: PIERO title: DR. inst: SPACE TELESCOPE COORDINATING FACILITY country: FRG esa: Y ! lname: DANZIGER fname: JOHN title: DR. mi: I. inst: EUROPEAN SOUTHERN OBSERVATORY country: FRG esa: Y ! lname: D'ODORICO fname: SANDRO title: DR. inst: EUROPEAN SOUTHERN OBSERVATORY country: FRG esa: Y ! lname: CHEVALIER fname: ROGER title: DR. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: TUOHY fname: I. title: DR. mi: R. inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: MATHEWSON fname: DONALD title: PROF mi: S. inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: LASKER fname: BARRY title: DR. mi: M. inst: STSCI country: USA ! lname: DOPITA fname: MICHAEL mi: A. inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: In order to maximise the scientific return, within the limited time line_2: given in the Phase I selection, we have elected to make a complete line_3: study of only two of the three targets for which time was awarded. line_4: We are now proposing to make the following observations: line_5: a. For SNR 0102-72.3. line_6: 1. Imaging in the [OIII], [OII], and [SII] lines, and in the line_7: yellow continuum to help identify the fainter filaments line_8: (using the WFC), and, at a later time in a future proposal round line_9: 2. Spectrophotometry in the UV of selected filaments with the FOS. ! question: 4 section: 1 line_1: A spatial resolution of order 20-40 milli arc second is required in line_2: order to resolve the individual knots and filaments, to distingush line_3: them from stars, and to make a proper-motion measurement practical line_4: over a ten-year period at Magellanic Cloud distances. line_5: Only the FOS on the HST is capable of the 1150-2400 angstrom line_6: spectrophotometry with the arc second spatial resolution that will line_7: be required in order to identify the nebular excitation mechanism line_8: and to measure the chemical abundances in individual knots. ! question: 5 section: 1 line_1: Our program falls into two parts, imaging and spectroscopy, line_2: of which the imaging program has so far been awarded time. line_3: The imaging program is designed to provide a high resolution line_4: mapping of our targets in the lines of [OIII], [OII], [OI], line_5: [SII], and H-Beta. line_6: generally chosen so as to give a S/N of between 7 and 30 per pixel line_7: in order that accurate line ratio maps may be constructed. ! question: 6 section: 0 line_1: ! question: 7 section: 1 line_1: The MSSSO investigators will have the prime responsibility for the line_2: analysis phase of the HST observations. It is anticipated that the line_3: reduction of the raw data will be performed at ST ScI; however, we line_4: have installed the IRAF system at MSSSO. line_5: Analysis of calibrated HST data will be undertaken at MSSSO line_6: where the software and hardware environment is more than line_7: adequate for this task. line_8: The interpretation of the data, theoretical modelling of the results line_9: and the subsequent preparation of papers will be the joint ! question: 8 section: 0 line_1: ! question: 9 section: 0 line_1: ! question: 10 section: 0 line_1: The manpower, fiscal and hardware resources necessary to carry line_2: through the reduction and interpretation of the data will be supplied line_3: within the internal budget of MSSSO as necessary. Funding will line_4: also be available to support any short overseas visits that may be line_5: necessary to coordinate team members' activities. Similar facilities line_6: and arrangements will also be put in hand at ESA. ! !end of general form text general_form_address: lname: DOPITA fname: MICHAEL mi: A. title: DR. category: PI inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES addr_1: PRIVATE BAG addr_2: WODEN P.O. city: CANBERRA, ACT zip: 2606 country: AUSTRALIA phone: (011 61) 62 490212 telex: AA62270 ! lname: LASKER fname: BARRY mi: M title: DR. category: CON inst: ST SCI addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21212 country: USA phone: (301) 338-4840 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SNR0102-72.3 descr_1: SUPERNOVA REMNANT IN THE SMC pos_1: RA = 01H 02M 25.0S +/- 0.1S, pos_2: DEC = -72D 18' 00" +/- 1" equinox: 1950.0 rv_or_z: V=150 comment_5: KNOTS. comment_7: FINDING CHARTS IN MATHEWSON, ET AL. comment_8: 1983; AP. J. SUPPL. 51, 345. fluxnum_1: 1 fluxval_1: V=22 +/- 1 fluxnum_2: 2 fluxval_2: SURF-LINE(5007)=1.2E-14, W-LINE(5007)=1 fluxnum_3: 3 fluxval_3: SURF-LINE(3727)=1.2E-14, W-LINE(3727)=1 fluxnum_4: 4 fluxval_4: SURF-LINE(6724)=1.0E-15, W-LINE(6724)=1 fluxnum_5: 5 fluxval_5: SURF-LINE(6300)=1.2E-15, W-LINE(6300)=1 fluxnum_6: 6 fluxval_6: V=20 +/- 1 ! targnum: 2 name_1: SNR0525-69.6 name_2: N132D descr_1: SUPERNOVA REMNANT IN THE LMC pos_1: RA = 05H 25M 27.0S +/- 0.1S, pos_2: DEC = -69D 41' 02" +/- 1" equinox: 1950.0 rv_or_z: V=270 comment_5: KNOTS. comment_7: FINDING CHARTS IN MATHEWSON, ET AL. comment_8: 1983; AP. J. SUPPL. 51, 345. fluxnum_1: 1 fluxval_1: V=20 +/- 1 fluxnum_2: 2 fluxval_2: SURF-LINE(5007)=2.4E-14, W-LINE(5007)=1 fluxnum_3: 3 fluxval_3: SURF-LINE(3727)=2.4E-14, W-LINE(3727)=1 fluxnum_4: 4 fluxval_4: SURF-LINE(6724)=2.4E-15, W-LINE(6724)=1 fluxnum_5: 5 fluxval_5: SURF-LINE(6300)=2.4E-15, W-LINE(6300)=1 fluxnum_6: 6 fluxval_6: SURF-LINE(4861)=0.8E-14, W-LINE(6300)=1 fluxnum_7: 7 fluxval_7: V=20 +/- 1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: PCEXP targname: # config: PC opmode: IMAGE aperture: ALL sp_element: # num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: # priority: # param_1: READ = YES, param_2: PRE-FLASH = YES, param_3: CR-SPLIT = NO ! linenum: 2.000 sequence_1: DEFINE sequence_2: WFEXP targname: # config: WFC opmode: IMAGE aperture: ALL sp_element: # num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: # priority: # param_1: READ = YES, param_2: PRE-FLASH = YES, param_3: CR-SPLIT = NO ! linenum: 11.000 sequence_1: USE WFEXP targname: SNR0102-72.3 sp_element: F375N time_per_exp: X1500 s_to_n: 7 fluxnum_1: 3 priority: 2 ! linenum: 12.000 sequence_1: USE WFEXP targname: SNR0102-72.3 sp_element: F492M time_per_exp: X1500 s_to_n: 30 fluxnum_1: 2 priority: 1 ! linenum: 13.000 sequence_1: USE WFEXP targname: SNR0102-72.3 sp_element: F673N time_per_exp: X1000 s_to_n: 8 fluxnum_1: 4 priority: 1 ! linenum: 15.000 sequence_1: USE WFEXP targname: SNR0102-72.3 sp_element: F547M time_per_exp: X120 s_to_n: 100 fluxnum_1: 6 priority: 1 ! linenum: 21.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F375N time_per_exp: X1500 s_to_n: 11 fluxnum_1: 3 priority: 2 ! linenum: 22.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F492M time_per_exp: X400 s_to_n: 20 fluxnum_1: 2 priority: 1 ! linenum: 23.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F487N time_per_exp: X1500 s_to_n: 21 fluxnum_1: 6 priority: 1 ! linenum: 24.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F631N time_per_exp: X1000 s_to_n: 9 fluxnum_1: 4 priority: 1 ! linenum: 25.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F673N time_per_exp: X700 s_to_n: 40 fluxnum_1: 4 priority: 1 ! linenum: 26.000 sequence_1: USE WFEXP targname: SNR0525-69.6 sp_element: F547M time_per_exp: X100 s_to_n: 100 fluxnum_1: 7 priority: 1 ! linenum: 27.000 sequence_1: USE PCEXP targname: SNR0525-69.6 sp_element: F492M time_per_exp: X2300 s_to_n: 24 fluxnum_1: 2 priority: 1 ! linenum: 28.000 sequence_1: USE PCEXP targname: SNR0525-69.6 sp_element: F547M time_per_exp: X260 s_to_n: 100 fluxnum_1: 7 priority: 1 ! ! end of exposure logsheet ! No scan data records found