!  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