! File: 4481C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:13:59:57 coverpage: title_1: THE NATURE OF THE INTERSTELLAR MEDIUM AROUND SN 1987A sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_fname: FREDERICK pi_mi: C. pi_lname: BRUHWEILER pi_inst: THE CATHOLIC UNIVERSITY OF AMERICA hours_pri: 7.75 num_pri: 2 hrs: Y funds_length: 12 off_fname: MONSIGNOR JOHN off_mi: F. off_lname: WIPPEL off_title: ACADEMIC VICE PRES. off_inst: THE CATHOLIC UNIVERSITY OF AMERICA off_addr_1: 620 MICHIGAN AVENUE N. E. off_city: WASHINGTON D. C. off_zip: 20064 off_country: USA off_phone: (202)319-5244 ! end of coverpage abstract: line_1: The extreme initial brightness of SN 1987A allowed the IUE and ground-based line_2: observatories to obtain an unsurpassed dataset for interstellar (IS) absorption line_3: lines for the LMC; it provided a unique opportunity to probe the IS line_4: environment of supernova. However, several unanswered questions remain. First, line_5: were the unusually strong C IV and Si IV features seen in the IUE spectrum line_6: formed in a UV flash of the supernova or did they pre-exist the explosion as line_7: the diffuse \[O III\] emission and 800 O stars in the vicinity suggest\? line_8: Second, what is the origin of the strong optical \[Fe X\] absorption seen toward line_9: SN 1987A\? In an effort to answer these questions, we will use the GHRS, in the line_10: G160M, G200M, and echelle-B modes to probe the directions toward two LMC stars, line_11: Sk -69 203 and Sk -69 209a, that lie within 50 pc of SN 1987A in the plane of line_12: the sky. These stars are uncontaminated by the UV flash or circumstellar line_13: nebula and likely share the same interstellar environment as SN 1987A. We will line_14: search for strong C IV (1548,1550A) in these stars to assess if the strong C IV line_15: predated SN 1987A. We will also observe high ionization N V (1238,1242A), line_16: which cannot be produced by normal stellar photoionization, to place line_17: constraints on the formation of \[Fe X\] and the distribution of hot coronal line_18: gas near SN 1987A. We will observe Zn II and Fe II to determine the depletion line_19: patterns in the 10-24 expected discrete components along the line_20: line-of-sight. ! ! end of abstract general_form_proposers: lname: BRUHWEILER fname: FREDERICK title: PI mi: C. inst: THE CATHOLIC UNIVERSITY OF AMERICA country: USA ! lname: FITZURKA fname: MICHELLE mi: A. inst: THE CATHOLIC UNIVERSITY OF AMERICA country: USA ! lname: SMITH fname: ANDREW mi: M. inst: NASA/GODDARD SPACE FLIGHT CENTER country: USA ! lname: MARAN fname: STEPHEN mi: P. inst: NASA/GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We have selected two UV bright stars nearest to SN 1987A in the LMC line_2: accessible at moderate dispersion with the GHRS( Sk -69 209a line_3: HD269828; WN3-5 M_v=10.9 and Sk -69 203 (B0.5 I; M_v=12.2). line_4: The projected lines-of-sight toward Sk -69 203 and Sk -69 209a line_5: pass within 35 and 50 pc of SN 1987A, assuming (d_LMC=50 kpc). line_6: observations would sample lines-of-sight free of any effects of a line_7: UV-flash or CS-envelope and probe the ambient interstellar line_8: environment of SN 1987A. line_9: The GHRS observations of the two LMC stars 1987A will line_10: provide data at S/N ~ 20 through the large science aperture (LSA). line_11: The data will be obtained using G160M, G200M, and ECH-B gratings. line_12: The echelle-B will be centered at 2379A to obtain data line_13: for two Fe II lines (2382.76 and 2373.74A) for expected vel. range, line_14: spanning a factor of 10 in f-value. The G200M at 2045A will line_15: sample Zn II doublet at 2026.14 and 2062.66A. As a bonus, we will line_16: also sample Cr II, Mg I, and Co II at the same grating settings. line_17: Blending of high velocity Zn II and Cr II can be acounted for in the line_18: data analysis. We will sample C IV doublet at 1550A and C I lines line_19: near 1560A with a single G160M setting. We will line_20: use the deduced absorption from the low-lying J-levels in C I to line_21: obtain pressures in intervening diffuse clouds (Smith et al. 1991). line_22: A G160M exposure, centered at 1250A, will sample absorption line_23: from the N V, Mg II, S II, and Si II from 1238 to 1260. ! question: 4 section: 1 line_1: Observations of these two targets with the IUE in 1987 showed that line_2: neither bright enough to give useful high dispersion spectra with line_3: IUE. Therefore, the GHRS on HST is required for this research. ! question: 5 section: 1 line_1: N/A ! question: 6 section: 1 line_1: We will only require wavelength calibrations at the specified line_2: wavelength settings as presented in exposure logsheet. ! question: 7 section: 1 line_1: All data will be reduced and analyzed using software at either line_2: NASA/GSFC or CUA that has developed by the P-I or members of the line_3: GHRS Support Group at GSFC. line_4: The procedure for data reduction and analysis is as follows: line_6: After the individual FP-SPLITS have been co-added, the line_7: accompanying wavelength calibrations will be used to place all line_8: the data on an accurate wavelength (velocity) scale. line_10: We will use profile fitting in the velocity frame to determine line_11: the number of absorption components along the line-of-sight. In line_12: addition to curve-of-growth techniques, we will adopt the line_13: formulation of Savage and Sembach (1991) to present line_14: column density versus velocity (see Savage et al. 1991 for line_15: application to GHRS data). Presented in this way, the data line_16: quickly and easily show how elemental depletion varies along the line_17: line-of-sight from component to component. line_19: The two lines-of-sight toward Sk -69 203 and Sk -69 209a line_20: will be compared with those obtained from IUE data for line_21: SN 1987A. This direct comparison will determine which, if any, line_22: velocity components of C IV seen in the IUE actually were line_23: produced via a UV-flash of the supernova. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: Seven refereed publications, none directly related to this program. ! question: 10 section: 1 line_1: The PI and graduate students at CUA are working with members line_2: of the GHRS/IDT at NASA with access to NASA line_3: computing facilities. Also, CUA has same software installed on line_4: comparable, but faster machines at CUA. line_5: Moreover, the PI, along with several capable graduate line_6: students, has developed the necessary software for the complete line_7: analysis of data requested in this proposal. ! !end of general form text general_form_address: lname: Bruhweiler fname: Frederick mi: C. category: PI inst: The Catholic University of America addr_1: Physics Department - 200 Hannan Hall addr_2: 620 Michigan Avenue N. E. city: Washington D. C. zip: 20064 country: USA phone: (202)319-5315 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SK-69D203 name_2: GSC09162.00629 descr_1: B,105 pos_1: RA = 05H 35M 27.31S +/- 0.1S, pos_2: DEC = -69D 13' 52.2" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V=12.2 fluxnum_2: 2 fluxval_2: F-CONT(1240)=1.9 E-13 ! targnum: 2 name_1: SK-69D209A name_2: GSC09162.00137 descr_1: B,105 pos_1: RA = 05H 35M 59.69S +/- 0.1S, pos_2: DEC = -69D 11' 52.2" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V=10.9 fluxnum_2: 2 fluxval_2: F-CONT(1240)=4.8 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: SK-69D203 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_3: BRIGHT=RETURN req_1: CYCLE 3 /1.0-7.1; req_2: ONBOARD ACQ FOR 1.1; comment_1: STEP-TIME=0.2 S ! linenum: 1.100 targname: SK-69D203 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2.1-7.1; comment_2: STEP-TIME=0.2S ! linenum: 2.100 targname: SK-69D203 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1247 num_exp: 5 time_per_exp: 345.6S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=4 ! linenum: 3.100 targname: SK-69D203 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 9 time_per_exp: 345.6S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=4 ! linenum: 4.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 60S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=4 ! linenum: 5.100 targname: SK-69D203 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 2045 num_exp: 5 time_per_exp: 345.6S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=4 ! linenum: 6.100 targname: SK-69D203 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B24 wavelength: 2379.29 num_exp: 7 time_per_exp: 217.6S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 7.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B24 wavelength: 2379.29 num_exp: 1 time_per_exp: 60S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 ! ! end of exposure logsheet ! No scan data records found