!   $Id: 5731,v 7.1 1994/10/12 13:14:26 pepsa Exp $

coverpage:

  title_1:         THE NATURE OF GASEOUS LOOPS IN THE MILKY WAY HALO - GO CARRYOVER
    sci_cat:       INTERSTELLAR MEDIUM
    sci_subcat:    ABSORPTION LINES
    proposal_for:  GO/CAR
    cont_id:       3706
    pi_fname:      LAURA
    pi_lname:      DANLY
    pi_inst:       SPACE TELESCOPE SCIENCE INSTITUTE
    pi_country:    USA
    pi_phone:      301-338-4730
    hours_pri:     4.58
    num_pri:       3
    hrs:           Y
    funds_amount:  65412
    funds_length:  12
    off_fname:     PETER
    off_lname:     STOCKMAN
    off_title:     ASSOCIATE DIRECTOR
    off_inst:      SPACE TELESCOPE SCIENCE INSTITUTE
    off_addr_1:    3700 SAN MARTIN DRIVE
    off_city:      BALTIMORE
    off_state:     MD
    off_zip:       21218
    off_country:   USA
    off_phone:     301-338-4730
! end of coverpage

abstract:

    line_1:        Recent evidence has shown that the nature of the gaseous halos of galaxies
    line_2:        both depends upon and contributes to the nature of the underlying disk.
    line_3:        "Galactic fountain" theories propose that hot gas produced in the disk rises to
    line_4:        large scale height where it cools and flows back to the disk in a rain of cool
    line_5:        clouds. Because of their anomolous negative velocities, the high latitude
    line_6:        neutral hydrogen clouds are thought to be the returning gas in this halo
    line_7:        circulation scheme. Most of the infalling gas is found in large, coherent
    line_8:        loop-like structures toward the North Galactic Pole.  We propose to study halo
    line_9:        circulation by observing the kinematics and ionization balance the intermediate
    line_10:       velocity clouds through absorption line observations of both high and low
    line_11:       ionization species. By studying the ionization balance, we hope to determine
    line_12:       the nature of the gas heating and cooling processes. Together with the
    line_13:       kinematic information available through high spectral resolution GHRS data,
    line_14:       we expect to be able to place severe constraints upon galactic circulation
    line_15:       models.

!
! end of abstract

general_form_proposers:

  lname:           DANLY
    fname:         LAURA
    title:         PI
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       U.S.A.

!

  lname:           BENJAMIN
    fname:         ROBERT
    inst:          UNIVERSITY OF TEXAS AT AUSTIN
    country:       U.S.A.

!

  lname:           KUNTZ
    fname:         KIP
    mi:            D.
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       U.S.A.

!

  lname:           ALBERT
    fname:         ELISE
    inst:          UNITED STATES NAVAL ACADEMY
    country:       U.S.A.

!

  lname:           SHAPIRO
    fname:         PAUL
    inst:          UNIVERSITY OF TEXAS AT AUSTIN
    country:       U.S.A.

!
! end of general_form_proposers block

general_form_text:


!

  question:        3
    section:       1
    line_1:        We propose to observe three lines of sight with the GHRS
    line_2:        through the SSA each at three settings of grating G160M. The
    line_3:        line of sights are toward the stars:
    line_5:        HD 121800:  l=113, b=49,  V=9.1, B-V=+0.04, E(B-V)=0.06,
    line_6:        Spectral type B2 V, D=2200 pc, Z=1650 pc
    line_8:        BD+49 2137:  l=134, b=66, V=10.7,
    line_9:        Spectral type B7 V,            Z=1600 pc
    line_11:       BD+38 2182:  l=182, b=62, V=11.2, B-V=-0.22, E(B-V)=0.02,
    line_12:       Spectral type B2 V, D=4600 pc, Z=4100 pc \bigskip The three
    line_13:       grating settings are centered as follows: 1. 1550 \AA.
    line_14:       (Useable range 1534\AA - 1566\AA ) This setting will obtain
    line_15:       the C IV $\lambda$$\lambda$1548-1550 lines. This setting
    line_16:       will also obtain the weak C I line at $\lambda$1560, which
    line_17:       will be used with the HI data to understand the neutral
    line_18:       component.

!

  question:        3
    section:       2
    line_1:        2. 1403 \AA. (Useable range 1387\AA - 1419\AA ) This setting
    line_2:        will obtain the Si IV $\lambda$$\lambda$1393,1402 lines.
    line_3:        Comparing these line strengths to the C IV line strengths is
    line_4:        a principle diagnostic for hot gas.
    line_6:        3. 1249 \AA. (Useable range 1233\AA - 1265\AA )  This
    line_7:        setting will obtain the N V $\lambda$1238-1242 lines. The
    line_8:        high ionization potential of N V (77.5 eV) means that this
    line_9:        line is a good diagnostic of hot gas. This setting will also
    line_10:       obtain the strong low ionization lines S II $\lambda$1250,
    line_11:       $\lambda$1253, $\lambda$1259, Si II $\lambda$1260. These low
    line_12:       ionization lines are important diagnostics of the "warm"
    line_13:       gas, as their spread of f-values allows a wide range of
    line_14:       sensitivity.
    line_16:       The exposure times were chosen to achieve S/N=50 and
    line_17:       detection limits of about 4 mA for the HD 121800 line of
    line_18:       sight, and S/N=30 and detection limits of about 7 mA for the
    line_19:       BD+49 2137 and BD+38 2182 lines of sight. These signal to
    line_20:       noise ratios will be appropriate for modeling, and will be

!

  question:        3
    section:       3
    line_1:        adequate for the comparison with Space Telescope archive
    line_2:        data for HD 93512. There are exposures of HD 121800
    line_3:        scheduled as part of GO program No.2257, however, the GO
    line_4:        (Blair Savage) has not yet determined how to reshape his
    line_5:        program in the light of the changest in the observatory
    line_6:        capabilities. If there are exposures of HD 121800 taken as
    line_7:        part of that program, we will utilize the archival spectra
    line_8:        when they become available.

!

  question:        4
    section:       1
    line_1:        High resolution, high S/N observations of a range of ions
    line_2:        (including C IV, Si IV and N V) are necessary to study the
    line_3:        nature of the ionization in the IV arch.  Previous data
    line_4:        taken with the IUE satellite are shown in Figure 3.  While
    line_5:        the data are tantalizing, they lack sufficient resolution
    line_6:        and S/N to address the specific objectives of this proposal.
    line_7:        In order to observe the highly ionized species at high
    line_8:        resolution (about 13 km/s) and high S/N (S/N$\sim$30 for BD
    line_9:        +38 2182 and BD +49 2137;  S/N$\sim$50 for HD 121800) we
    line_10:       require the capabilities of the GHRS on HST.
    line_12:       Over the past decade, we have pursued studies of galactic
    line_13:       halo gas using ground based optical, 21-cm H I, and IUE
    line_14:       ultraviolet observations. Results from these extensive
    line_15:       studies have laid the groundwork for the scientific
    line_16:       objectives of this proposal.  However, only the proposed HST
    line_17:       observations will result in sufficiently high quality cloud
    line_18:       column densities and velocites to compare with specific
    line_19:       predictions of models for cooling gas. No ground based
    line_20:       facilities or other space based facilities are capable of
    line_21:       provided the data required to address the scientific issues
    line_22:       outlined in this proposal.

!

  question:        5
    section:       1
    line_1:        Wave calibrations are required for all nine GHRS spectra
    line_2:        (3 spectra for each of 3 stars).  see below.

!

  question:        6
    section:       1
    line_1:        Wave calibrations are required for all nine GHRS spectra
    line_2:        (3 spectra for each of 3 stars).  This was not included
    line_3:        in the Phase I proposal, but is now recognized as
    line_4:        critical to the success of the program.  Absolute velocity
    line_5:        calibration to about 2-3 km/s is required.  Each wave
    line_6:        calibration must be performed with no gap immediately
    line_7:        preceeding each spectral exposure.

!


!


!

  question:        8
    section:       1
    line_1:        This proposal is one of several programs (including an
    line_2:        accepted GO program; see Question 8) designed to study gas
    line_3:        in the environments of galaxies.  These programs have been
    line_4:        tailored specifically to meet the objectives outlined in the
    line_5:        P.I.'s (accepted) Hubble Fellowship proposal.  The goal of
    line_6:        the Hubble Fellowship research is to study gas which is in
    line_7:        the vicinity of a variety of galaxies, and is therefore
    line_8:        subjected to a range of interstellar and intergalactic
    line_9:        environments.  Central to this research is a detailed study
    line_10:       of the production and maintenance of Milky Way halo gas,
    line_11:       where we can expect to obtain the highest quality data and
    line_12:       develop the most detailed models.  Accurate means to
    line_13:       interpret quantitative spectroscopic data are critical to
    line_14:       the interpretation of QSO absorption lines.
    line_16:       Related Cycle 2 proposals include:
    line_18:       $\bullet$ ``Spectroscopic Investigations of a Possible
    line_19:       Galactic Chimney" (Danly, L, Albert, C. E., and Kuntz, K.
    line_20:       D.)

!

  question:        8
    section:       2
    line_1:
    line_2:        $\bullet$ ``A detailed Study of Nearby Ly$\alpha$ Systems"
    line_3:        (Urry, C. M., Boggess, A., Maraschi, L., Danly, L.,
    line_4:        Bruhweiler, F. C., Falomo, R., Grady, C. A., Tanzi, E. G.,
    line_5:        and Treves, A.)
    line_7:        $\bullet$ ``The Distance of High Velocity Clouds"  (Wakker,
    line_8:        B. P., Danly, L., Schwarz, U. J., and Van Woerden, H.)
    line_10:       $\bullet$ ``Quasar Absorption Line Studies of Starburst
    line_11:       Galaxy Enviornments" (Norman, C. N., Blades, J. C., Danly,
    line_12:       L., and Heckman, T. J.)

!

  question:        9
    section:       1
    line_1:        \ques{\phantom{8.} a. List HST program numbers and titles,
    line_2:        and specify whether they are related to this project or
    line_3:        not.}
    line_5:        Proposal No. 2644, ``The Environments of Starburst Galaxies:
    line_6:        Absorption-Line Studies of Galactic Outflows
    line_8:        This GO program is related to the objectives of this
    line_9:        proposal as described in Question 7.
    line_11:       \ques{\phantom{8.} b. Summarize the main results obtained
    line_12:       from previous related programs.}
    line_14:       The data have not yet been obtained
    line_16:       \ques{\phantom{8.} c. List publications resulting from the
    line_17:       above data (Format:  Title, Authors, Journal, Volume, Page,
    line_18:       and Year.)}
    line_20:       N/A (see 8b)

!

  question:        10
    section:       1
    line_1:        The Space Telescope Science Institute has a wide variety of
    line_2:        hardware and software systems to support the research
    line_3:        proposed here.  These include STSDAS, IDL, and KDAF which
    line_4:        are supported on both the VAX cluster and the Sun
    line_5:        Workstations.

!
!end of general form text

general_form_address:

  lname:           DANLY
    fname:         LAURA
    category:      PI
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    addr_1:        3700 SAN MARTIN DRIVE
    city:          BALTIMORE
    state:         MD
    zip:           21218
    country:       USA
    phone:         301-338-4422
    telex:         684-9101-STSCI-411

!
! end of general_form_address records

fixed_targets:

    targnum:       10
    name_1:        HD121800
    name_2:        GSC04177-00880
    descr_1:       A,110,
    descr_2:       G,508,510,
    pos_1:         PLATE-ID=01BR,
    pos_2:         RA= 13H 55M 15.4S +/- 0.2S,
    pos_3:         DEC= +66D 7' 0.7" +/- 1"
    equinox:       J2000
    rv_or_z:       V=13
    fluxnum_1:     1
    fluxval_1:     V=9.1, TYPE=B2V, E(B-V)=0.06
    fluxnum_2:     2
    fluxval_2:     B-V=-0.17
    fluxnum_3:     3
    fluxval_3:     F-CONT(1240) = 16 E-11
    fluxnum_4:     4
    fluxval_4:     F-CONT(1400) = 1 E-10
    fluxnum_5:     5
    fluxval_5:     F-CONT(1550) = 9 E-11

!

    targnum:       20
    name_1:        BD+49D2137
    name_2:        GSC03458-00650
    descr_1:       G,508,510,
    descr_2:       A,110,
    pos_1:         PLATE-ID=024D,
    pos_2:         RA= 12H 25M 0.4S +/- 0.1S,
    pos_3:         DEC= +49D 8' 30.4" +/- 1"
    equinox:       J2000
    rv_or_z:       V=115
    fluxnum_1:     1
    fluxval_1:     V=10.7, TYPE=B7V, E(B-V)=0.02
    fluxnum_2:     2
    fluxval_2:     B-V=-0.14
    fluxnum_3:     3
    fluxval_3:     F-CONT(1240) = 2 E-12
    fluxnum_4:     4
    fluxval_4:     F-CONT(1400) = 18 E-13
    fluxnum_5:     5
    fluxval_5:     F-CONT(1550) = 17 E-13

!

    targnum:       30
    name_1:        BD+38D2182
    name_2:        GSC03009-02485
    descr_1:       G,508,510,
    descr_2:       A,110,
    pos_1:         PLATE-ID=01R8,
    pos_2:         RA= 10H 49M 12.9S +/- 0.1S,
    pos_3:         DEC= +38D 0' 14.5" +/- 1"
    equinox:       J2000
    rv_or_z:       V=79
    fluxnum_1:     1
    fluxval_1:     V=11.2, TYPE=B2V, E(B-V)=0.02
    fluxnum_2:     2
    fluxval_2:     B-V=-0.22
    fluxnum_3:     3
    fluxval_3:     F-CONT(1240) = 36 E-13
    fluxnum_4:     4
    fluxval_4:     F-CONT(1400) = 22 E-13
    fluxnum_5:     5
    fluxval_5:     F-CONT(1550) = 17 E-13

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      HD121800
    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_1:       BRIGHT=RETURN
    req_1:         ONBOARD ACQ FOR 1.10;
    req_2:         CYCLE 4 / 1-2.7

!

    linenum:       1.100
    targname:      HD121800
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      0.25
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  5.0S
    fluxnum_1:     1
    priority:      1
    param_1:       SEARCH-SIZE=5
    req_1:         ONBOARD ACQ FOR 1.20 - 1.70;
    req_2:         SEQ 1.2-1.7 NO GAP
    comment_1:     STEPTIME=0.2

!

    linenum:       1.200
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1249
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 1.3;

!

    linenum:       1.300
    targname:      HD121800
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1249
    num_exp:       1
    time_per_exp:  544S
    s_to_n:        50
    fluxnum_1:     3
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5
    comment_1:     EXPOSURE TIME IS NEAREST INTEGER
    comment_2:     LARGER THAN INTEGER MULTIPLE OF 27.2 S

!

    linenum:       1.400
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1403
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 1.5;

!

    linenum:       1.500
    targname:      HD121800
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1403
    num_exp:       1
    time_per_exp:  871S
    s_to_n:        50
    fluxnum_1:     4
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5
    comment_1:     EXPOSURE TIME IS NEAREST INTEGER
    comment_2:     LARGER THAN INTEGER MULTIPLE OF 27.2 S

!

    linenum:       1.600
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1550
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 1.7;

!

    linenum:       1.700
    targname:      HD121800
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1550
    num_exp:       1
    time_per_exp:  1306S
    s_to_n:        50
    fluxnum_1:     5
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5
    comment_1:     EXPOSURE TIME IS NEAREST INTEGER
    comment_2:     LARGER THAN INTEGER MULTIPLE OF 27.2 S

!

    linenum:       2.000
    targname:      BD+49D2137
    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_1:       BRIGHT=RETURN
    req_1:         ONBOARD ACQ FOR 2.10;

!

    linenum:       2.100
    targname:      BD+49D2137
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      0.25
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  5.0S
    fluxnum_1:     1
    priority:      1
    param_1:       SEARCH-SIZE=5
    req_1:         ONBOARD ACQ FOR 2.20 - 2.70;
    req_2:	   SEQ 2.2-2.7 NO GAP
    comment_1:     STEPTIME=0.2

!

    linenum:       2.200
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1249
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 2.3;

!

    linenum:       2.300
    targname:      BD+49D2137
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1249
    num_exp:       1
    time_per_exp:  27.2M
    s_to_n:        30
    fluxnum_1:     3
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5

!

    linenum:       2.400
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1403
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 2.5;

!

    linenum:       2.500
    targname:      BD+49D2137
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1403
    num_exp:       1
    time_per_exp:  27.2M
    s_to_n:        30
    fluxnum_1:     4
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5

!

    linenum:       2.600
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G160M
    wavelength:    1550
    num_exp:       1
    time_per_exp:  DEF
    priority:      1
    param_1:       STEP-PATT=5
    req_1:         CALIB FOR 2.7;

!

    linenum:       2.700
    targname:      BD+49D2137
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G160M
    wavelength:    1550
    num_exp:       1
    time_per_exp:  39.9M
    s_to_n:        30
    fluxnum_1:     5
    priority:      1
    param_1:       FP-SPLIT=STD
    param_2:       STEP-PATT=5

!
!
! end of exposure logsheet

! No scan data records found