! 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