!  File:  3746C.PROP
!  Database:  PEPDB
!  Date:  19-FEB-1994:18:10:17

coverpage:

  title_1:         THE COOLING OF THE LOCAL DIFFUSE INTERSTELLAR MEDIUM
    sci_cat:       INTERSTELLAR MEDIUM
    sci_subcat:    LOCAL MEDIUM
    proposal_for:  GO
    pi_fname:      CECILE
    pi_lname:      GRY
    pi_inst:       LABORATOIRE D'ASTRONOMIE SPATIALE
    pi_country:    FRANCE
    pi_phone:      33-91-055927
    hours_pri:     7.22
    num_pri:       18
    hrs:           Y
    off_fname:     PAUL
    off_lname:     CRUVELLIER
    off_title:     DIRECTOR
    off_inst:      LABORATOIRE D'ASTRONOMIE SPATIALE
    off_addr_1:    TRAVERSE DU SIPHON
    off_addr_2:    LES TROIS LUCS
    off_city:      13012 MARSEILLE
    off_country:   FRANCE
    off_phone:     (33) 91 05 59 27
! end of coverpage

abstract:

    line_1:        We want to study the cooling processes of the local interstellar
    line_2:        medium by observing the population of the excited fine-structure states
    line_3:        in the ground electronic level of ionized carbon and neutral atomic
    line_4:        oxygen. Far-IR line emission between these excited states and the ground
    line_5:        states of these ions is the main cooling agent of the cold and warm
    line_6:        neutral atomic gas respectively. The corresponding column densities in
    line_7:        front of bright stars will be obtained from GHRS observations of
    line_8:        electronic transitions originating from these states. In order to study
    line_9:        the structure of the interstellar matter along the lines of sight, other
    line_10:       transitions will be observed with the GHRS and from the ground: this is
    line_11:       necessary to correctly derive the column densities of the different
    line_12:       individual components by fitting the lines with theoretical profiles
    line_13:       and to separate the neutral from the ionized medium along the
    line_14:       lines of sight. A comparison of the results with direct observations of
    line_15:       the FIR fine-structure lines from COBE and later from ISO and SIRTF will
    line_16:       allow to determine to what extent the local interstellar medium is
    line_17:       representative of the general medium at galactic scales, and in
    line_18:       particular to compare the far-UV interstellar radiation fields.

!
! end of abstract

general_form_proposers:

  lname:           GRY
    fname:         CECILE
    title:         PI
    inst:          LABORATOIRE D'ASTRONOMIE SPATIALE
    country:       FRANCE
    esa:           Y

!

  lname:           BOULANGER
    fname:         FRANCOIS
    inst:          OBSERVATOIRE DE PARIS-MEUDON
    country:       FRANCE
    esa:           Y

!

  lname:           LEQUEUX
    fname:         JAMES
    inst:          OBSERVATOIRE DE PARIS-MEUDON
    country:       FRANCE
    esa:           Y

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       1
    line_1:

!

  question:        3
    section:       1
    line_1:        We will record the spectrum of 8 stars at one spectral setting of the
    line_2:        G160M grating. It will be centered at the wavelength of 1312 A to
    line_3:        optimize both the quality of the photocathode at the most important
    line_4:        line (OI* 1304A) and the number of covered interesting spectral lines.
    line_5:        Special care will be taken to get
    line_6:        i) the highest possible resolution : the spectra will be recorded in
    line_7:        the SSA with a substepping of 4, to increase the resolution by
    line_8:        deconvolution.
    line_9:        ii) a very high signal to noise ratio. To overcome the limit due to the
    line_10:       photocathode granularity, we will break down the exposure into  4
    line_11:       subexposures via the FP-split procedure to distinguish between
    line_12:       photocathode granularity and spectral features, and we aim at getting
    line_13:       a  photon noise much smaller than the fixed-pattern noise (>2%)
    line_14:       therefore we calculate the exposure time corresponding to a S/N of
    line_15:       250 for each diode substep (i.e. the total exposure time for
    line_16:       one target will be 4 times this time).

!

  question:        4
    section:       1
    line_1:        These observations (high resolution-spectroscopy in the Far-UV) can
    line_2:        only be done with the GHRS on board the HST. Attempts for using IUE
    line_3:        have been very disappointing for lack of resolution and signal to
    line_4:        noise ratio. Copernicus data have been used in a preliminary study
    line_5:        for CII*, NII* and NII**, but a better S/N ratio is needed to detect
    line_6:        OI*. Nevertheless ground-based observations will be performed to help
    line_7:        defining the line of sight structure.

!

  question:        5
    section:       1
    line_1:        For the faint OI* and OI** lines, there is a possibility of
    line_2:        contamination by telluric lines (In the Xi Per spectrum presented
    line_3:        by Savage in the STScI Newsletter of March 1991, the telluric OI*
    line_4:        is very well seen). We thus ask to make those  observations when the
    line_5:        velocity shift between the earth and the interstellar cloud is not
    line_6:        null (higher than 10 km/s). The allowed observation dates are
    line_7:        specified are requirements.Usually there are two allowed time
    line_8:        intervals in one year.

!

  question:        6
    section:       1
    line_1:        None

!

  question:        7
    section:       1
    line_1:        We will get from the ST ScI the calibrated science data which is
    line_2:        provided as the output of the Routine Science Data Processing (RSDP)
    line_3:        and Calibration Data Base Software (CDBS) at the Institut.
    line_4:        The data reduction can be made at any of the proposing institutes
    line_5:        which possess adequate facilities, with the help if necessary of the
    line_6:        ESA ST/ECF in Garching. The data analysis will be done using an
    line_7:        interactive program for line-profile fitting of which we have a
    line_8:        considerable experience.

!

  question:        8
    section:       1
    line_1:        None

!

  question:        9
    section:       1
    line_1:        P 2078 "A search for primordial gas; is IZw18 a young galaxy?"
    line_2:        PI J. Lequeux
    line_3:        Not related to present project
    line_4:        Observations not yet done
    line_5:        no publication yet (see above)

!

  question:        10
    section:       1
    line_1:        All resources to be provided by the proposer's institutes
    line_2:        At least one student will be dedicated to the project.

!
!end of general form text

general_form_address:

  lname:           GRY
    fname:         CECILE
    category:      PI
    inst:          LABORATOIRE D'ASTRONOMIE SPATIALE
    addr_1:        TRAVERSE DU SIPHON
    addr_2:        LES TROIS LUCS
    city:          13012 MARSEILLE
    country:       FRANCE
    phone:         (33) 91 05 59 27
    telex:         420 584 ASTROSP F

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        HD149038
    name_2:        MU-NOR
    descr_1:       A,105,G,513
    pos_1:         RA=16H 34M 04.86S +/-.05S,
    pos_2:         DEC=-44D 02' 42.8"  +/-.1"
    equinox:       2000
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     -0.000667
    dec_pm_val:    -0.0050
    rv_or_z:       V = +5
    fluxnum_1:     1
    fluxval_1:     V=4.87 +/-.1
    fluxnum_2:     2
    fluxval_2:     B-V=+0.10 +/- .02
    fluxnum_3:     3
    fluxval_3:     F-CONT(1300)=5.0 +/-.3 E-10

!

    targnum:       2
    name_1:        HD149757
    name_2:        ZET-OPH
    descr_1:       A,104,G,513
    pos_1:         RA=16H 37M 09.398S +/-.01S,
    pos_2:         DEC=-10D 34' 02.79"  +/-.1"
    equinox:       2000
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     0.000800
    dec_pm_val:    0.0230
    rv_or_z:       V = -15
    fluxnum_1:     1
    fluxval_1:     V = 2.57 +/-.1
    fluxnum_2:     2
    fluxval_2:     B-V = +0.02 +/- .02
    fluxnum_3:     3
    fluxval_3:     F-CONT(1300) = 4.0 +/-.3 E-9

!

    targnum:       3
    name_1:        HD30614
    name_2:        ALP-CAM
    descr_1:       A,105,G,513
    pos_1:         RA = 04H 54M 02.966S +/-.01S,
    pos_2:         DEC = +66D 20' 33.45"  +/-.1"
    equinox:       2000
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     -0.000333
    dec_pm_val:    0.0290
    rv_or_z:       V = +6.1
    fluxnum_1:     1
    fluxval_1:     V = 4.29 +/-.01
    fluxnum_2:     2
    fluxval_2:     B-V = +0.04 +/- .01
    fluxnum_3:     3
    fluxval_3:     F-CONT(1300) = 6.9 +/-.1 E-10

!

    targnum:       4
    name_1:        HD165024
    name_2:        TET-ARA
    descr_1:       A,113,G,508
    pos_1:         RA = 18H 06M 37.78S +/-.05S,
    pos_2:         DEC = -50D 05' 29.0"  +/-.1"
    equinox:       2000
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     -0.000733
    dec_pm_val:    -0.0170
    rv_or_z:       V = +3.4
    fluxnum_1:     1
    fluxval_1:     V = 3.66 +/-.01
    fluxnum_2:     2
    fluxval_2:     B-V = -.09 +/- .01
    fluxnum_3:     3
    fluxval_3:     F-CONT(1300) = 2.2 +/-.1 E-9

!

    targnum:       5
    name_1:        HD214680
    name_2:        10LAC
    descr_1:       A,104,G,508
    pos_1:         RA = 22H 39M 15.60S +/-.01S,
    pos_2:         DEC = 39D 03' 01.21"  +/-.1"
    equinox:       2000
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1950.00
    ra_pm_val:     -0.002067
    dec_pm_val:    0.0290
    an_prlx_val:   0.0050
    rv_or_z:       V = -9.7
    fluxnum_1:     1
    fluxval_1:     V = 4.90 +/-.02
    fluxnum_2:     2
    fluxval_2:     B-V = -0.20 +/- .02
    fluxnum_3:     3
    fluxval_3:     F-CONT(1300) = 2.4 +/-.3 E-9

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.100
    targname:      HD149038
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-A2
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       BRIGHT=65000
    param_3:       FAINT=1000
    param_4:       LOCATE=DEF
    req_1:         ONBOARD ACQ FOR 1.2;
    req_2:         AT 4-SEP-92 +/- 62D;
    req_4:         CYCLE 2 / 1.1-8.2;
    comment_1:     AVOID OBSERVING WHEN THE EARTH
    comment_2:     HAS SAME RADIAL VELOCITY AS THE
    comment_3:     INTERSTELLAR CLOUD.
    comment_4:     ALLOWED PERIODS : DEC 19 TO MAY 22
    comment_5:     OR : JULY 4 TO NOV 5
    comment_6:     ALTERNATE AT 6-MAR-93 +/- 77D

!

    linenum:       1.200
    targname:      HD149038
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1312
    num_exp:       3
    time_per_exp:  13.3M
    s_to_n:        200
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=5
    param_2:       FP-SPLIT=STD
    param_3:       COMB=FOUR
    param_4:       DOPPLER=ON

!

    linenum:       2.100
    targname:      HD149757
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-A2
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       BRIGHT=65000
    param_3:       FAINT=2000
    param_4:       LOCATE=DEF
    req_1:         ONBOARD ACQ FOR 2.2;
    req_2:         AT 1-SEP-92 +/- 36D;
    comment_1:     AVOID OBSERVING WHEN THE EARTH
    comment_2:     HAS SAME RADIAL VELOCITY AS THE
    comment_3:     INTERSTELLAR CLOUD.
    comment_4:     ALLOWED PERIODS : NOV 25 TO JUNE 10
    comment_5:     OR : JULY 27 TO OCT 7
    comment_6:     ALTERNATE  AT 3-MAR-93 +/- 98D;

!

    linenum:       2.200
    targname:      HD149757
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1312
    num_exp:       1
    time_per_exp:  7M
    s_to_n:        250
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=5
    param_2:       FP-SPLIT=STD
    param_3:       COMB=FOUR
    param_4:       DOPPLER=ON

!

    linenum:       3.100
    targname:      HD30614
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-A2
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       BRIGHT=65000
    param_3:       FAINT=1000
    param_4:       LOCATE=DEF
    req_1:         ONBOARD ACQ FOR 3.2;
    req_2:         AT 13-SEP-92 +/- 73D;
    comment_1:     AVOID OBSERVING WHEN THE EARTH
    comment_2:     HAS SAME RADIAL VELOCITY AS THE
    comment_3:     INTERSTELLAR CLOUD.
    comment_4:     ALLOWED PERIODS : JAN 14 TO MAY 9
    comment_5:     OR : JULY 2 TO NOV 26
    comment_6:     ALTERNATE AT 12-MAR-93 +/- 57D

!

    linenum:       3.200
    targname:      HD30614
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1312
    num_exp:       2
    time_per_exp:  15M
    s_to_n:        250
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=5
    param_2:       FP-SPLIT=STD
    param_3:       COMB=FOUR
    param_4:       DOPPLER=ON

!

    linenum:       4.100
    targname:      HD165024
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-A2
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       BRIGHT=65000
    param_3:       FAINT=1000
    param_4:       LOCATE=DEF
    req_1:         ONBOARD ACQ FOR 4.2;
    req_2:         AT 21-SEP-92 +/- 53D;
    comment_1:     AVOID OBSERVING WHEN THE EARTH
    comment_2:     HAS SAME RADIAL VELOCITY AS THE
    comment_3:     INTERSTELLAR CLOUD.
    comment_4:     ALT AT:21-MAR-93 +/- 86D
    comment_5:     ALLOWED : JULY 30 TO NOVEMBER 13
    comment_6:     OR: DECEMBER 25 TO JUNE 15

!

    linenum:       4.200
    targname:      HD165024
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1312
    num_exp:       2
    time_per_exp:  7M
    s_to_n:        250
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=5
    param_2:       FP-SPLIT=STD
    param_3:       COMB=FOUR
    param_4:       DOPPLER=ON

!

    linenum:       8.100
    targname:      HD214680
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-A2
    time_per_exp:  1.8S
    priority:      1
    param_1:       SEARCH-SIZE=3
    param_2:       BRIGHT=65000
    param_3:       FAINT=1000
    param_4:       LOCATE=DEF
    req_1:         ONBOARD ACQ FOR 8.2;
    req_2:         AT 21-DEC-92 +/- 100D;
    comment_1:     AVOID OBSERVING WHEN THE EARTH
    comment_2:     HAS SAME RADIAL VELOCITY AS THE
    comment_3:     INTERSTELLAR CLOUD.
    comment_4:     ALLOWED PERIODS : SEP 10 TO APR 2
    comment_5:     OR : MAY 4 TO AUG 9
    comment_6:     ALTERNATE AT 21-JUN-93 +/- 48D

!

    linenum:       8.200
    targname:      HD214680
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1312
    num_exp:       2
    time_per_exp:  7M
    s_to_n:        250
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=5
    param_2:       FP-SPLIT=STD
    param_3:       COMB=FOUR
    param_4:       DOPPLER=ON

!
! end of exposure logsheet

! No scan data records found