! File: 3621C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:14:10:27 coverpage: title_1: THE PARTIALLY BURNED EJECTA OF SUPERNOVA 1006 sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO pi_fname: CHI-CHAO pi_lname: WU pi_inst: COMPUTER SCIENCES CORPORATION pi_country: USA pi_phone: 301-572-3637 hours_pri: 7.13 num_pri: 1 fos: Y funds_amount: 67697 funds_length: 12 off_fname: ROSELLE off_lname: HARDE off_title: SR. CONTRACTS ADMIN. off_inst: COMPUTER SCIENCES CORPORATION off_addr_1: SYSTEM SCIENCES DIVISION off_addr_2: 4061 POWDER MILL ROAD off_city: CALVERTON off_state: MD off_zip: 20705 off_country: USA off_phone: (301) 572-3637 ! end of coverpage abstract: line_1: We propose to use the FOS to observe a 17th mag sdOB star situated line_2: behind the young remnant of the Type Ia SN 1006 in order to study the line_3: absorption spectrum of the SNR. IUE spectra show strong, broad Fe II UV line_4: absorption features, along with several Si, and possibly S and O lines line_5: redshifted by about 5000 km/sec. These features have provided the line_6: first direct observational evidence for high velocity, heavy element line_7: enriched ejecta within a young Type Ia SNR. In the first GO cycle, we were line_8: granted "high priority" HST time to observe the Fe II lines with the FOS line_9: (2200-2800 angstroms). Here, we request time to observe the Si II, III, IV, line_10: O I, S II, and possibly other lines which appear at shorter wavelengths line_11: (1200-1600 angstroms). These lines have been observed and reobserved by us line_12: with IUE, but the noisiness of the IUE spectra has made interpretation of line_13: features inevitably uncertain. The HST FOS spectrum will have about 10 line_14: times better S/N and 5 times better resolution which are essential to line_15: establish accurate profiles, equivalent widths, and wavelengths. Accurate line_16: HST measurements will: (1) confirm unambiguously the presence of partially line_17: burned heavy element material in SN 1006; and (2) provide firm evidence of line_18: the mass, composition, velocity distribution, and ionization state of this line_19: material. A rigorous and quantitative analysis of these features will line_20: substantially advance the understanding of Type Ia SN. ! ! end of abstract general_form_proposers: lname: WU fname: CHI-CHAO title: PI inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: CRENSHAW fname: D. MICHAEL inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: FESEN fname: ROBERT mi: A. inst: DARTMOUTH COLLEGE country: USA ! lname: HAMILTON fname: ANDREW mi: J. inst: UNIVERSITY OF COLORADO country: USA ! lname: LEVENTHAL fname: MARVIN inst: BELL LABORATORIES country: USA ! lname: MCCOLLOUGH fname: MICHAEL inst: COMPUTER SCIENCES CORPORATION country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The FOS blue detector will be used with the G130H line_2: grating and the 1.0 arcsec circular aperture to line_3: obtain a UV spectrum in the range 1150 - 1600 line_4: angstroms. The spectrum will have a resolution of line_5: R = 1000 and a signal-to-noise ratio of S/N = 60 line_6: per angstrom (30 per channel using substeps of 4). line_7: The 1.0 arcsec aperture provides the best line_8: combination of throughput and resolution for this line_9: project. ! question: 4 section: 1 line_1: HST is the only telescope capable of obtaining UV line_2: spectra with the high S/N and resolution that is line_3: required for this project. The IUE satellite has line_4: already been used to observe this target five line_5: times, and the data have been exhaustively line_6: processed and merged in an attempt to improve the line_7: S/N ratio. Further progress can only be made with line_8: the proposed FOS observation. ! question: 7 section: 1 line_1: The FOS data will analyzed with the Vaxstation purchased for the analysis of the line_2: cycle 1 observations; STSDAS will be used for the initial data reduction and line_3: analysis. IUE spectra have indicated that the underlying stellar spectrum is line_4: almost featureless, consistent with the star's sdOB classification. Thus, the line_5: absorption spectrum of SN 1006 should be straightforward to identify and isolate line_6: from stellar spectral features. Stellar lines that are detected will be line_7: identified and measured using available stellar templates. Interstellar lines line_8: not associated with the SNR will also be identified, by virtue of their line_9: narrowness. The resulting 1006 SNR absorption spectrum will be analyzed by line_10: fitting the observed lines simultaneously. Free parameters of this fitting line_11: procedure will include continuum shape, ion abundances, and velocity line_12: distributions of ground state species for C I, C II, C IV, O I, Si II, Si III, line_13: Si IV, S II, and possibly other intermediate mass ions. The FOS spectra will line_14: also be compared to IUE spectra to determine if changes in line strengths and line_15: profiles have occurred over the decade during which SN 1006 has been observed. line_16: This will indicate whether the ejecta are distributed smoothly or in knots. line_17: Fully reduced data and preliminary analysis results will be sent to Hamilton, line_18: who will compare the spectral results to detailed predictions of Type Ia SNe line_19: using the most up-to-date available models. This effort will involve running line_20: hydrodynamic simulations of SN Ia ejecta evolved into an appropriate line_21: interstellar medium; computing the resulting nonequilibrium ionization, UV, and line_22: X-ray emission of the shocked ejecta; and following self-consistently the line_23: time-dependent photoionization and radiative transfer through unshocked ejecta. ! question: 9 section: 1 line_1: Proposal # 2434 (related) PI: Wu line_2: A Study of the Chemical Composition and Velocity Structure line_3: of the Young Supernova Remnant AD 1006 line_4: Status: FOS observations were obtained in August 1991. line_6: Proposal # 2298 (not related) PI: Burstein line_7: Stellar Content of Galaxies and Globular Clusters line_8: Status: Early WFPC images were taken in early August 1991. line_10: Proposal # 2416 (not related) PI: Dufour line_11: Imagery and Spectroscopy of Super Metal Poor Galaxies line_12: Status: Early WFPC images were taken in mid-July 1991. line_14: Proposal # 2955 (not related) PI: Fesen line_15: Nighttime Measurement of Nitric Oxide line_16: Status: Observation has not yet been scheduled. line_18: Proposal # 1170 (GTO, not related) PI: Boggess line_19: UV Spectroscopy of Low-Redshift Active Galaxies line_20: Status: No useful spectra have been obtained despite two line_21: attempts due to HST hardware and software problems. ! question: 10 section: 1 line_1: line_2: CSC personnel have access to VAX mainframe line_3: computers and peripherals at several sites for line_4: basic data reduction and analysis. Data analysis line_5: software, including STSDAS and spectral analysis line_6: packages based on the Interactive Data Language line_7: (IDL) are also available. There is a large number line_8: of astronomers at CSC available for expert advice line_9: to an investigator on observational techniques, line_10: detector calibration, data analysis, and line_11: theoretical modeling. CSC also provides a pool of line_12: research assistants and data technicians as well line_13: as administrative and secretarial support for line_14: research programs. ! !end of general form text general_form_address: lname: WU fname: CHI-CHAO category: PI inst: COMPUTER SCIENCES CORPORATION addr_1: SPACE TELESCOPE SCIENCE INSTITUTE addr_2: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: (301) 338-4770 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: STAR-1503-4159 descr_1: A,108 pos_1: PLATE-ID=02F5, pos_2: RA=15H 02M 53.186S +/- 0.5", pos_3: DEC=-41D 59' 16.43" +/- 0.5" equinox: 2000 comment_1: HAS AN 18.5 MAG STAR 8 ARCSEC comment_2: AWAY. fluxnum_1: 1 fluxval_1: V=16.74 +/- 0.05 fluxnum_2: 2 fluxval_2: B-V=-0.14 +/- 0.02 fluxnum_3: 3 fluxval_3: F-CONT(2000)=5.0 +/- 2.0 E-15 fluxnum_4: 4 fluxval_4: F-CONT(2400)=4.5 +/- 1.0 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4000)=1.5 +/- 0.5 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: STAR-1503-4159 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: BRIGHT=200000, param_2: FAINT=660 req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 2 / 1-4; req_3: GROUP 1-4 WITHIN 36H; ! linenum: 2.000 targname: STAR-1503-4159 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 300M s_to_n: 40 fluxnum_1: 3 priority: 1 ! linenum: 3.000 targname: STAR-1503-4159 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18S fluxnum_1: 1 priority: 1 param_1: BRIGHT=200000, param_2: FAINT=660 req_1: ONBOARD ACQ FOR 4; ! linenum: 4.000 targname: STAR-1503-4159 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 168M fluxnum_1: 3 priority: 1 ! ! end of exposure logsheet ! No scan data records found