! File: 3957C.PROP
! Database: PEPDB
! Date: 20-FEB-1994:01:37:34
coverpage:
title_1: SEARCH FOR INTERSTELLAR MOLECULES IN SPECTRA OF TWO B STARS
title_2: -- CYCLE 2
sci_cat: INTERSTELLAR MEDIUM
proposal_for: GTO/HRS
cont_id: 1200
pi_fname: ANDREW
pi_mi: M.
pi_lname: SMITH
pi_inst: NASA, GODDARD SPACE FLIGHT CENTER
pi_country: USA
pi_phone: (301)286-3900
keywords_1: MOLECULAR CLOUD, INTERSTELLAR MOLECULES
hours_pri: 9.00
num_pri: 2
pi_position: STAFF ASTRONOMER
! end of coverpage
abstract:
line_1: We will probe the chemical and physcial processes in diffuse
line_2: interstellar clouds and look for evidence of
line_3: molecule formation in gas heated by shocks or intense
line_4: ultraviolet radiation. We will observe HD62542, a star in the
line_5: Gum Nebula at seven carousel positions in the medium
line_6: resolution modes. Optical studies indicate that one of
line_7: the components of its interstellar spectrum is characterized
line_8: by high density (approximately 10,000/cubic cm) and highest
line_9: density per unit visual extinction of any star yet studied.
line_10: We will also observe omicron Persei using the echelle, and
line_11: combine the results with previous high quality results
line_12: obtained by the "Copernicus" satellite.
!
! end of abstract
general_form_proposers:
lname: BRUHWEILER
fname: FRED
inst: CATHOLIC UNIVERSITY OF AMERICA
country: USA
!
lname: CARDELLI
fname: JASON
mi: D.
inst: WISCONSIN, UNIVERSITY OF
country: USA
!
lname: SMITH
fname: ANDREW
mi: M.
inst: NASA, GODDARD SPACE FLIGHT CENTER
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: The GHRS will be used. For both o Per and HD62542 we
line_2: propose to look for six molecules, H2O, N2, HCl, CH2, SiO,
line_3: and CS. For o Per, 88 carousel echelle settings are required,
line_4: 14 at medium resolution and 2 at the low resolution. All
line_5: require the FP-SPLIT option. A scheme is used that includes
line_6: using multiple wavelength settings for each molecular line,
line_7: thus sampling different parts of the detector windows
line_8: and diode arrays to minimize fixed pattern noise. For
line_9: HD62542, H2 and CO, will also be included. Medium and low
line_10: resolution will be used, except for one echelle
line_11: observation of the CO (7-0). 32 carousel settings are
line_12: planned. The FP-SPLIT option is used, but varying the
line_13: central wavelength for each molecular feature is not
line_14: considered to be necessary since the anticipated equivalent
line_15: widths should be several mA. When possible, lines of
line_16: interest are placed on a region of the detector to avoid
line_17: defective diodes and to minimize fixed pattern noise.
line_18: For mostmolecules (CO and H2 excepted) the features are weak,
line_19: long exposures and large S/N ratios are required.
line_20: HD62542
line_21: exposures exposures exposures
line_22: Cycle 2
line_23: 101.0,101.1,101.2,101.3,102.0,106.0
!
question: 3
section: 2
line_1:
line_4: Star o Per
line_5: exposures exposures exposures
line_6: Cycle 3
line_7: 1.5, 1.6, 1.7, 6.1, 6.2, 6.3, 20.0, 20.1
line_8: 22.1, 22.2, 22.3, 24.0, 25.0, 26.0, 27.0
line_14: COMMENT CONTINUED FROM TF TARGET NUMBER 1:
line_16: 21 F(2717)=2.7+/-0.3E-10, 22 F(2803)=2.5+/-0.3E-10, 23 F(1768)=6.8+/-2.0E-10,
line_17: 24 F(2889)=2.5+/-0.3E-10, 25 F(1412)=8.6+/-2.0E-10, 26 F(1460)=9.2+/-2.0E-10
!
question: 4
section: 1
line_1: The spectra of few interstellar molecules exist in the optical
line_2: whereas many are found in the HRS range. "Copernicus"
line_3: demonstrated the usefulness of the UV to interstellar studies
line_4: but it possessed neither the resolving power not the
line_5: sensitivity required to measure the column densities of
line_6: molecules other than CO and molecular hydrogen. I.U.E. has
line_7: been successful in observations of faint stars, but
line_8: its resolving power is about a factor of 2 less than that of
line_9: "Copernicus" and its limiting S/N ratio is much too large
line_10: to detect any interstellar molecules other than CO.
!
question: 5
section: 1
line_1: No real-time observations are required.
!
question: 6
section: 1
line_1: A single wavelength scale calibration is required for each
line_2: target in order to relate line velocities measured with the
line_3: GHRS to measurements of other instruments. Accuracies on
line_4: the order to +/- 0.5 km/s an d +/- 2.2 km/s for the high
line_5: and medium resolving power modes can be realized. Determining
line_6: cloud component radial velocities relative to measured background
line_7: star velocities is unreliable because the stellar lines are
line_8: are broadened by rotation and blending. The wavelength scale
line_9: calibration should be performed immediately following a science
line_10: observation for the same carousel position to avoid any time
line_11: dependent variations of the wavelength scale due, for example,
line_12: to temperature fluctuations or positional variations of the
line_13: stellar image in the science apertures. Otherwise, there is
line_14: no requirement for ambiguous observations or uninterrupted
line_15: exposures.
!
question: 7
section: 1
line_1: These will be designed to determine column densities of both molecular and
line_2: atomic species with a view toward finding abundances. Both curve-of-growth and
line_3: profile fitting techniques will be employed. In some cases it is
line_4: possible using comparatively few reaction channels to draw
line_5: conclusions regarding the details of relevant gas phase
line_6: chemistry, and to a limited extent, the physical conditions of
line_7: the cloud)s) in which the molecules are embedded. Such species
line_8: include HCl, SiO, and CS. Other species such as H2O, N2 and
line_9: CH2 will require analyses involving large arrays of chemical
line_10: reactions since the chemistry of Hydro-carbons and oxygen-
line_11: bearing molecules is complex. Cloud models will be constructed
line_12: in which chemical equililbrium is established and in which the
line_13: chemistry is time dependent as during the passage of an MHD shock.
line_14: The success of this analysis will depend on the
line_15: quality and quantity of our measurements as well as on the availability of
line_16: reasonably accurate rate constants.
!
question: 10
section: 1
line_1: Both computer hardware and software will be available at NASA/GSFC for data
line_2: analysis.
!
question: 13
section: 1
line_1: This program constitutes a search for molecules in diffuse interstellar clouds.
line_2: The High Resolution Spectrograph will be used to observe portions
line_3: of the spectrum of HD62542 at medium resolving power and
line_4: portions of the spectrum of o Per at both high and medium
line_5: resolving power. The scientific goal is to study molecule
line_6: formation mechanisms in diffuse interstellar clouds.
!
!end of general form text
general_form_address:
lname: SMITH
fname: ANDREW
mi: M.
category: PI
inst: NASA, GODDARD SPACE FLIGHT CENTER
city: GREENBELT
state: MD
zip: 20771
country: USA
phone: 301-344-8648
telex: 89675
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: HD23180
name_2: OMICRON-PER
descr_1: B1 III STAR SHOWING
descr_2: INTERSTELLAR
descr_3: MOLECULAR SPECTRUM
pos_1: RA=3H44M19.1S+/-0.1S,
pos_2: DEC=+32D17'18"+/-1.0"
equinox: 2000
pm_or_par: Y
pos_epoch_bj: J
pos_epoch_yr: 2000.00
ra_pm_val: 0.000533
ra_pm_unct: 0.000133
dec_pm_val: -0.0090
dec_pm_unct: 0.0020
an_prlx_val: 0.0230
rv_or_z: V=+18.5
comment_1: 11 F(1335)=8.7+/-2.0E-10
comment_2: 12 F(1341)=8.7+/-2.0E-10
comment_3: 13 F(1657)=8.2+/-2.0E-10
comment_4: 14 F(1914)=4.0+/-0.6E-10
comment_5: 15 F(2190)=2.7+/-0.3E-10
comment_6: 16 F(2242)=2.4+/-0.3E-10
comment_7: 17 F(2266)=2.8+/-0.3E-10
comment_8: 18 F(2313)=2.8+/-0.3E-10
comment_9: 19 F(2344)=2.9+/-0.3E-10
comment_10: 20 F(2576)=3.2+/-0.3E-10
fluxnum_1: 1
fluxval_1: V=3.83+/-0.02,TYPE=B1III,E(B-V)=0.31
fluxnum_2: 2
fluxval_2: F(1216)=1.0+/-0.3E-10
fluxnum_3: 3
fluxval_3: F(1222)=2.0+/-0.5E-10
fluxnum_4: 4
fluxval_4: F(1227)=2.5+/-0.6E-10
fluxnum_5: 5
fluxval_5: F(1241)=7.9+/-2.0E-10
fluxnum_6: 6
fluxval_6: F(1257)=7.9+/-2.0E-10
fluxnum_7: 7
fluxval_7: F(1273)=7.9+/-2.0E-10
fluxnum_8: 8
fluxval_8: F(1290)=9.0+/-2.0E-10
fluxnum_9: 9
fluxval_9: F(1302)=7.0+/-2.0E-10
fluxnum_10: 10
fluxval_10: F(1310)=1.0+/-0.2E-9
!
targnum: 3
name_1: HD62542
name_2: SAO218917
descr_1: B5 V STAR IN THE
descr_2: GUM NEBULA
pos_1: RA=7H 40M 58.073S+/-0.05",
pos_2: DEC=-42D 06' 36.16"+/-0.7"
equinox: 1950
pm_or_par: Y
pos_epoch_bj: B
pos_epoch_yr: 1950.00
ra_pm_val: -0.001000
ra_pm_unct: 0.000080
dec_pm_val: 0.0170
dec_pm_unct: 0.0012
fluxnum_1: 1
fluxval_1: V=8.04, TYPE=B5V, B-V=0.17
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 101.000
targname: HD62542
config: HRS
opmode: ACQ
aperture: 2.0
sp_element: MIRROR-N2
num_exp: 1
time_per_exp: 5S
fluxnum_1: 1
priority: 1
param_2: BRIGHT=RETURN,
param_3: SEARCH-SIZE=5
req_1: ONBOARD ACQ FOR 101.1-117;
req_2: CYCLE 2/101-117
!
linenum: 101.100
targname: HD62542
config: HRS
opmode: ACQ/PEAKUP
aperture: 2.0
sp_element: MIRROR-N2
num_exp: 1
time_per_exp: 20.4S
s_to_n: 10
fluxnum_1: 1
priority: 1
req_1: ONBOARD ACQ FOR 106-117;
req_2: CYCLE 2
!
linenum: 106.000
targname: HD62542
config: HRS
opmode: ACCUM
aperture: 0.25
sp_element: G160M
wavelength: 1234.86
num_exp: 33
time_per_exp: 5.8M
s_to_n: 30
priority: 1
param_1: STEP-PATT=4,
param_2: FP-SPLIT=STD
req_1: CYCLE 2
comment_1: MOLECULAR H2O
!
linenum: 108.000
targname: HD62542
config: HRS
opmode: ACCUM
aperture: 0.25
sp_element: G160M
wavelength: 1284.20
num_exp: 20
time_per_exp: 5.8M
s_to_n: 42
priority: 1
param_1: STEP-PATT=4,
param_2: FP-SPLIT=STD
req_1: CYCLE 2
comment_1: MOLECULAR HCL,N2
!
linenum: 109.000
targname: WAVE
config: HRS
opmode: ACCUM
aperture: 0.25
sp_element: G160M
wavelength: 1344.27
num_exp: 1
time_per_exp: 30S
priority: 1
param_1: STEP-PATT=4
req_1: CALIB FOR 109.1; CYCLE 2;
req_2: SEQ 109.0-109.1 NO GAP
!
linenum: 109.100
targname: ^
config: ^
opmode: ^
aperture: ^
sp_element: ^
wavelength: 1344.27
num_exp: 10
time_per_exp: 5.8M
s_to_n: 22
priority: 1
param_1: STEP-PATT=4,
param_2: FP-SPLIT=STD
req_1: CYCLE 2
comment_1: MOLECULAR C2,CLI,OI,CII
!
linenum: 110.000
targname: HD62542
config: ^
opmode: ^
aperture: ^
sp_element: ^
wavelength: 1400.42
num_exp: 20
time_per_exp: 5.8M
s_to_n: 42
priority: 1
param_1: STEP-PATT=4,
param_2: FP-SPLIT=STD
req_1: CYCLE 2
comment_1: MOLECULAR CH2
!
linenum: 117.000
targname: ^
config: ^
opmode: ^
aperture: ^
sp_element: G270M
wavelength: 2586.76
num_exp: 10
time_per_exp: 5.8M
s_to_n: 42
priority: 1
param_1: STEP-PATT=4,
param_2: FP-SPLIT=STD
req_1: CYCLE 2
comment_1: MOLECULAR CS
!
! end of exposure logsheet
! No scan data records found