! $Id: 5365,v 9.1 1994/07/27 17:08:09 pepsa Exp $ coverpage: title_1: PROBING EXCITATION MECHANISMS AND ABUNDANCES IN YOUNG title_2: MAGELLANIC CLOUD SNRS - CYCLE 4 MED:EARLY ACQ FOR 5607 sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO pi_fname: WILLIAM pi_mi: P. pi_lname: BLAIR pi_inst: 2380 pi_country: USA pi_phone: 410-516-8447 hours_pri: 13.20 num_pri: 6 wf_pc: Y fos: Y off_fname: CHERYL-LEE off_lname: HOWARD off_title: ASSISTANT DEAN off_inst: 2380 off_addr_1: HOMEWOOD RESEARCH ADMINISTRATION off_addr_2: 146 MERRYMAN HALL off_addr_3: 34TH & CHARLES STREETS off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-516-8668 ! end of coverpage abstract: line_1: We will obtain WFPC2 images and FOS spectra of a young, oxygen- line_2: rich supernova remnant called N132D in the Magellanic Cloud. line_3: The images will be used to study fine-scale spatial and ionization line_4: structures within the knotty filaments, and also provide EARLY ACQ line_5: exposures for the spectroscopy. The FOS will be used to obtain line_6: UV/optical spectra of chemically and kinematically distinct knots in line_7: the object. Only HST has the resolution necessary to isolate line_8: individual knots for study. Having UV and optical data with the line_9: same apertures in the same positions will for the first time provide line_10: reliable relative intensities of UV and optical lines for line_11: comparison with theoretical models. This will provide a critical test line_12: of the emission mechanisms and allow us to derive reliable elemental line_13: abundances. The HST data will provide important line_14: tests of theories of nucleosynthesis in massive stars and will allow line_15: an improved understanding of the dynamics of SN explosions and line_16: mixing in the ejecta. ! ! end of abstract general_form_proposers: lname: BLAIR fname: WILLIAM mi: P. inst: 2380 country: USA ! lname: LONG fname: KNOX mi: S. inst: 3470 country: USA ! lname: WINKLER fname: P. FRANK inst: 2680 country: USA ! lname: KIRSHNER fname: ROBERT mi: P. inst: 2170 country: USA ! lname: RAYMOND fname: JOHN mi: C. inst: 2166 country: USA ! lname: MORSE fname: JON mi: A. inst: 3470 country: USA ! lname: DOPITA fname: MICHAEL mi: A. inst: 4140 country: AUSTRALIA ! lname: SUTHERLAND fname: RALPH mi: S. inst: 1764 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We request WFPC2 F502N, F375N, F673N, and F547M exposures of N132D. line_2: These exposures will be used to study small scale structure in the line_3: ejecta that dominates the emission from this object. Knots in Cas A, line_4: for example, range from unresolved to several arcsec in dimension. line_5: Even though N132D is roughly 20x more distant than Cas A, HST will line_6: resolve considerable structure. The F502N exposure will be most line_7: important for this because [O III] 5007 is bright and the HST/WFPC2 line_8: throughput is relatively good. The F375N exposure will allow the line_9: ionization structure of the filaments to be assessed from the [O II]3727 line_10: emission. (Note: this will only be possible for filaments whose radial line_11: velocities are fully within the bandpasses of the filters.) The F673N line_12: exposure will show emission from [S II]6717,6731 for comparison. These line_13: data will also be used as "EARLY ACQ" images, permitting us to make line_14: appropriate choices of FOS aperture sizes and placements to isolate line_15: knots for study. F547M is needed as a "continuum" band to assess the line_16: difference between faint stars and stellar-appearing emission knots line_17: (important since N132D is in the bar of the LMC). Total exposure line_18: through each filter will be split in half for easier line_19: cosmic ray removal. line_20: We will place the 1" circular (or smaller if appropriate) FOS aperture line_21: on three chemically-distinct knots in N132D. line_22: The three positions in N132D are the minimum needed to sample (a) line_23: O-emitting and (b) S-emitting material in the inner ejecta, and ! question: 3 section: 2 line_1: (c) an out-lying filament showing emission in H-alpha, [S II], line_2: and [O III]. We assume exposures with FOS/BL G160L (6000s), and FOS/RD line_3: G270H (3400s), G400H (1000s), and G570H (1400s) at each of the three line_4: positions. G160L is considerably lower resolution than the other line_5: gratings, but covers the FUV range of interest with one grating. line_6: Combined UV/optical data are requested with the same apertures in line_7: the same positions to provide accurate relative line intensities line_8: for comparison with theoretical calculations. ! question: 4 section: 1 line_1: We have worked hard with IUE to obtain the existing UV data on N132D. line_2: These spectra are all lengthy double-shift IUE exposures, but IUE line_3: simply can't resolve individual knots. Hence, blending of material line_4: with differing abundances and physical conditions hampers an accurate line_5: comparison with models. It has also been difficult to accurately line_6: combine optical and UV data taken with different instruments and line_7: with differing aperture sizes and placements. HST will provide line_8: both the spatial resolution and the combined UV/optical coverage line_9: with the same slit in the same position to make a quantitative line_10: difference in the comparison against calculated models. ! question: 5 section: 1 line_1: None. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: Some of the filamentary structures in these objects are extended on the line_2: several arcsec scale and, with our existing ground-based imaging data, line_3: we could measure positions of offset stars and filaments directly. line_4: However, previous experience with EARLY ACQ WFPC exposures has line_5: demonstrated that ground-based data can sometimes be deceptive. Blair line_6: and Davidsen (1993) have shown how an FOS blind offset based on ground- line_7: based images would have "missed" the bulk of the emission in an M33 line_8: supernova remnant, for example. With the amount of time to be spent on line_9: the spectroscopy, we strongly prefer the method of obtaining EARLY ACQ line_10: images and basing the FOS blind offset acquisition on these data. And line_11: of course, the images are of intrinsic interest in their own right for line_12: the spatial and ionization structure they will show. ! question: 9 section: 1 line_1: Here is a listing of other programs involving the scientists on this line_2: proposal, as copied from Phase I submission. line_3: P2417: "CAS A: The Remnant of a Massive Supernova"; Kirshner, Blair, line_4: Long, Winkler, and Raymond line_5: P2563: "SINS--The Supernova INtensive Survey"; Kirshner et al. line_6: P3853: "SINS: The Supernova INtensive Study - 87A revisit" line_7: P4016: "SINS: The Supernova INtensive Study - cyc 1 opportunity" line_8: P4022: "SINS: The Supernova INtensive Study - 87A revisit" line_9: P4252: "SINS: Late Time Observations of SN1992A" line_10: P4528: "SINS: The Supernova INtensive Study - cyc 2 opportunity" line_11: P4445: "SINS: The Supernova INtensize Study - cyc 3" line_12: P2266: "Post Asymptotic Giant Branch Evolution in the Magellanic line_13: Clouds"; Dopita. line_14: P2243: "Shock Wave Structures of HH Objects"; Schwartz et al. line_15: (Raymond Co-I) line_16: P4674: "Molecular Emission in HH47"; Raymond et al. [No Obs. yet] line_17: P3683: "Accretion Disk Mapping in CVs"; Horne et al. (Long and line_18: Raymond Co-Is) line_19: P3836: "Spectroscopic Obs. od Exposed WDs in CVs"; Sion et al. line_20: (Long Co-I) line_21: Other SUPPLEMENTAL or PARALLEL programs not shown. Also, Blair line_22: is involved with some FOS GTO programs, although not as an line_23: "official" Co-I. ! question: 10 section: 1 line_1: Astrophysics at JHU has grown dramatically over the last decade. line_2: The JHU Center for Astrophysical Sciences provides an excellent line_3: research environment, with a fully qualified staff and a wide range line_4: of research expertise within its membership. line_5: JHU/CAS operates a computer center which is responsible for a wide line_6: range of services to its users, from maintenance of networks and line_7: machines to upgrades of software (including IRAF/STSDAS) to I/O devices line_8: and services. The PI has a SPARCstation 10 which has been purchased line_9: with monies from various NASA-related research grants he has received. line_10: This will provide state-of-the-art computer support for reduction and line_11: analysis of these data. No hardware is requested with this proposal, line_12: although some support of ongoing maintenance on this machine will be line_13: requested. line_14: STScI and the Harvard-Smithsonian Center for Astrophysics are, of line_15: course, first rate astronomical research institutions with state-of- line_16: the-art facilities, including computer hardware and software line_17: technicians, photo labs, and libraries, all of which will provide line_18: support as needed. line_19: At Middlebury College, the astronomical image-processing laboratory line_20: has a network of three Sparcstations running IRAF/STSDAS. These are line_21: now used for analysis of optical and X-ray data obtained by faculty and line_22: students at major ground- and space-based observatories, as well as line_23: images from a CCD camera mounted on a local 0.4-m telescope. Many ! question: 10 section: 2 line_1: Middlebury undergraduates develop substantial expertise in astronomical line_2: image processing. Not only would access to HST data be stimulating line_3: to them, but they will also be able to make a genuine contribution to line_4: the analysis. line_5: All resources required by Dopita will be provided by Mt Stromlo and line_6: Siding Spring Observatories. He has a SPARC II which will be used in line_7: the modelling. ! !end of general form text general_form_address: lname: Blair fname: William mi: P. category: PI inst: 2380 addr_1: 237 BLOOMBERG CENTER addr_2: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_3: JOHNS HOPKINS UNIVERSITY city: Baltimore state: MD zip: 21218 country: USA phone: 410-516-8447 telex: 410-516-8260 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: N132D descr_1: H, descr_2: 506 pos_1: RA = 05H 25M 26.0S +/- 3", pos_2: DEC = -69D 40' 48" +/- 3" equinox: 1950 pos_epoch_bj: B pos_epoch_yr: 1950.00 comment_1: CORRECTED CENTER OF EXTENDED SNR comment_2: EMISSION; USE FOR WFPC2 IMAGES. comment_3: CENTERS SW OF BRT. OPTICAL ARC. fluxnum_1: 1 fluxval_1: SURF-LINE(5007) = 2.6 +/- 0.5 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: N132D config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F502N wavelength: 5013 num_exp: 2 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG -6.8,-11.8; req_3: SAME POS FOR 2-4 AS 1; req_4: ORIENT 203D +/- 10D; comment_1: EARLY ACQ FOR PROGRAM 5607 comment_2: THE FOS EXPOSURES HAVE BEEN SPLIT ! linenum: 2.000 targname: N132D config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F375N wavelength: 3737 num_exp: 2 time_per_exp: 2000S priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG -6.8,-11.8; comment_1: EARLY ACQ AND SCIENCE EXPOSURE. comment_2: THE FOS EXPOSURES HAVE BEEN SPLIT comment_3: FROM THIS PROGRAM ! linenum: 3.000 targname: N132D config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F673N wavelength: 6732 num_exp: 2 time_per_exp: 1800S priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG -6.8,-11.8; comment_1: EARLY ACQ AND SCIENCE EXPOSURE. comment_2: THE FOS EXPOSURES HAVE BEEN SPLIT comment_3: FROM THIS PROGRAM ! linenum: 4.000 targname: N132D config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F547M wavelength: 5479 num_exp: 1 time_per_exp: 900S priority: 1 req_1: CYCLE 4; req_2: POS TARG -6.8,-11.8; comment_1: EARLY ACQ AND SCIENCE EXPOSURE. comment_2: USE TO DISCRIMINATE STARS. comment_3: THE FOS EXPOSURES HAVE BEEN SPLIT comment_4: FROM THIS PROGRAM ! ! end of exposure logsheet ! No scan data records found