!  File:  4685C.PROP
!  Database:  PEPDB
!  Date:  22-FEB-1994:22:23:39

coverpage:

  title_1:         SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYC3-HIGH
    sci_cat:       COOL STARS
    sci_subcat:    STELLAR ATMOSPHERES
    proposal_for:  GO
    pi_fname:      HOLLIS
    pi_mi:         R.
    pi_lname:      JOHNSON
    pi_inst:       INDIANA UNIVERSITY
    pi_country:    USA
    hours_pri:     16.00
    num_pri:       3
    fos:           Y
    hrs:           Y
    funds_length:  24
    off_fname:     GEORGE
    off_mi:        E.
    off_lname:     WALKER
    off_title:     ASSOC. V. PRESIDENT
    off_inst:      2270
    off_addr_1:    RESEARCH & UNIVERSITY GRADUATE SCHOOL
    off_addr_2:    BRYAN HALL, ROOM 104
    off_city:      BLOOMINGTON
    off_state:     IN
    off_zip:       47405
    off_country:   USA
    off_phone:     (812)-855-6153
! end of coverpage

abstract:

    line_1:        We propose to use the Faint Object Spectrograph (FOS) and the
    line_2:        Goddard High-Resolution Spectrograph (GHRS) on the HST
    line_3:        to obtain ultraviolet spectra of visually bright N-type
    line_4:        carbon stars and late M-giant stars. These spectra, obtainable only
    line_5:        with HST, will be used with theoretical models to infer the
    line_6:        temperature and density structure and the velocity fields of the
    line_7:        outer atmosphere in these evolutionarily advanced, non-mira
    line_8:        giants.  In anticipation of this effort, we have already pushed IUE
    line_9:        to its limit to obtain both low-resolution, and, where possible,
    line_10:       high-resolution spectra of several M, S, and C stars, and these
    line_11:       have been analyzed and published.  Based upon the observed line
    line_12:       profiles and continua, we will construct semi-empirical non-LTE models
    line_13:       in both plane-parallel geometry and spherical geometry, including
    line_14:       velocity fields, by attaching a chromosphere to theoretical
    line_15:       photospheric models.  Two-component models will be studied.
    line_16:       Using these and ab-initio hydrodynamic models, we will examine
    line_17:       the mechanisms responsible for chromospheric heating and mass
    line_18:       loss.  A full range of supporting ground-based observations
    line_19:       will be undertaken to permit us to connect models of the photospheres,
    line_20:       chromospheres, and circumstellar shells.

!
! end of abstract

general_form_proposers:

  lname:           JOHNSON
    fname:         HOLLIS
    title:         PI
    mi:            R.
    inst:          INDIANA UNIVERSITY
    country:       USA

!

  lname:           ALEXANDER
    fname:         DAVID
    mi:            R.
    inst:          WICHITA STATE UNIVERSITY
    country:       USA

!

  lname:           AVRETT
    fname:         EUGENE
    mi:            H.
    inst:          SMITHSONIAN ASTROPHYSICAL OBSERVATORY
    country:       USA

!

  lname:           BROWN
    fname:         ALEXANDER
    inst:          U.COLORADO JILA
    country:       USA

!

  lname:           CARPENTER
    fname:         KENNETH
    mi:            G.
    inst:          NASA GODDARD LASP
    country:       USA

!

  lname:           ERIKSSON
    fname:         KJELL
    inst:          UPPSALA ASTRONOMICAL OBSERVATORY
    country:       SWEDEN
    esa:           Y

!

  lname:           GUSTAFSSON
    fname:         BENGT
    inst:          UPPSALA ASTRONOMICAL OBSERVATORY
    country:       SWEDEN
    esa:           Y

!

  lname:           JORGENSEN
    fname:         UFFE
    mi:            G.
    inst:          NIELS BOHR INSTITUTE
    country:       DENMARK
    esa:           Y

!

  lname:           JUDGE
    fname:         PHILIP
    mi:            D.
    inst:          HIGH ALTITUDE OBSERVATORY
    country:       USA

!

  lname:           LINSKY
    fname:         JEFFREY
    mi:            L.
    inst:          U.COLORADO JILA
    country:       USA

!

  lname:           LUTTERMOSER
    fname:         DONALD
    mi:            G.
    inst:          IOWA STATE UNIVERSITY
    country:       USA

!

  lname:           QUERCI
    fname:         FRANCOIS
    inst:          OBSERVATOIRE MIDI PYRENEES, TOULOUSE
    country:       FRANCE
    esa:           Y

!

  lname:           QUERCI
    fname:         MONIQUE
    inst:          OBSERVATOIRE MIDI PYRENEES, TOULOUSE
    country:       FRANCE
    esa:           Y

!

  lname:           ROBINSON
    fname:         RICHARD
    mi:            D.
    inst:          COMPUTER SCIENCES CORPORATION
    country:       USA

!

  lname:           WING
    fname:         ROBERT
    mi:            F.
    inst:          OHIO STATE UNIVERSITY
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        Part a)
    line_2:        Two carbon stars of differing spectral class (TX Psc and UU Aur)
    line_3:        will be surveyed using the FOS G270H mode for the 2220-3300 A region.  The Mg
    line_4:        II h&k lines will be observed in the latter star with the G270M GHRS mode,
    line_5:        while Mg II in TX Psc will be observed using GHRS Echelle-B.
    line_8:        A comparison M-star will be observed with G270M/GHRS.
    line_9:        The exposure times are summarized in Section 4.
    line_13:       The project is pure Cycle 3:
    line_14:       Primary Hours:          Parallel Hours:          Exposures:
    line_15:       16.00                       0.0                    8
    line_17:       Part b)
    line_18:       N/A

!

  question:        4
    section:       1
    line_1:        Part a)
    line_2:        To understand mass loss and to model the outer atmospheres (including
    line_3:        chromospheres and circumstellar layers) require detailed profiles of key
    line_4:        spectral lines, which in turn requires high-resolution ultraviolet spectra.  We
    line_5:        have pushed IUE to its limit. That effort has produced low-resolution LWP/LWR
    line_6:        spectra of the brighter R stars of all classes, a few brighter N-type stars,
    line_7:        and several late M giant stars. High-resolution spectra have been obtained in
    line_8:        long exposures for a few bright early-R stars and a few bright M giant stars.
    line_9:        A 13-hour high-resolution LWP exposure of the best N-type star (TX Psc) was
    line_10:       considerably underexposed and showed clearly only the Mg II emission lines
    line_11:       while a few other lines were weakly present (Eriksson et al. 1986).  To make
    line_12:       further progress, it is absolutely necessary to use HST.
    line_14:       Narrow-band photometry and calibrated spectra will be obtained from the ground
    line_15:       at approximately the same time to determine the properties of the underlying
    line_16:       photosphere and the CSE.

!

  question:        4
    section:       2
    line_1:        Part b)
    line_2:        Summary of Exposure Times
    line_4:        Exposure    FOS   ----------------- GHRS -----------------------   Time/
    line_5:        Target  Factor    G270H    G270M/MgII  G270M/CII/FeII/FeII/MgI Ech-B/MgII  Star
    line_7:        TX Psc   1.0      0.25        -                 -                 4.0      4.25
    line_8:        UU Aur   2.3      0.50       2.3                -                  -       2.80
    line_11:       Mu Gem   0.08       -        0.1           0.5+0.25+0.25+0.25      -       1.35
    line_14:       subtotal          0.75       2.4               1.25               4.0      8.40
    line_16:       The total exposure time is 8.40 hours.
    line_17:       The number of targets is 3.
    line_18:       The number of wavelength settings is 8.
    line_19:       The FOS 0.25x2.0 and the GHRS 0.25x0.25 arcsec science apertures are used.
    line_21:       The exposure times for TX Psc are derived using fluxes from IUE observations
    line_22:       taken during 1981, when the star was in a "low" state, to ensure that we obtain
    line_23:       at least the minimum desired S/N of 10.   If the star is brighter at the time

!

  question:        4
    section:       3
    line_1:        of the HST observations, we will be delighted to achieve a higher S/N.  We have
    line_2:        increased exposure times, relative to pre-launch values, by 3.3x for the FOS
    line_3:        exposures and 4.0x for the GHRS (small aperture) exposures, to account for the
    line_4:        effects of spherical aberration.  We require the use of the GHRS small aperture
    line_5:        to preserve the design spectral resolution and the true line profiles.
    line_6:        Monochromatic peak line fluxes, as measured in IUE low-resolution spectra of
    line_7:        TX Psc are:
    line_8:        C II 2325 A     Al II  2670   Fe II 2750 A      Mg II 2800 A
    line_9:        -----------     -----------   ------------      ------------
    line_10:       4.0e-15         3.0e-15       5.0e-15           2.0e-14    ergs/cm2/s/A
    line_12:       The PEAK S/N achieved in the GHRS observations  will be higher than predicted
    line_13:       using these figures directly, since, unlike IUE, GHRS will resolve the lines.
    line_14:       The GHRS exposure times have been checked using the new sensitivities in the
    line_15:       Cycle 3 handbook, modified to account for the improved GHRS SSA sensitivity
    line_16:       recently achieved with an improved centering of targets in the GHRS SSA.
    line_17:       Exposure times for the other targets are scaled, using the observed
    line_18:       U-magnitude, from those calculated for TX Psc.
    line_20:       The total estimated spacecraft time = 15.98 hours

!

  question:        5
    section:       1
    line_1:        Wavelength calibration exposures on the internal Pt-lamps are requested for
    line_2:        each GHRS exposure since we require the highest possible wavelength accuracy
    line_3:        in order to measure flow velocities in the chromospheres and circumstellar
    line_4:        shells of our target stars.

!

  question:        6
    section:       1
    line_1:        Special Calibration Requirement(s)
    line_2:        __________________________________
    line_3:        Wavelength calibrations at each GHRS
    line_4:        grating setting (no motion of
    line_5:        carrousel between science and
    line_6:        calibration exposure) are required to
    line_7:        obtain the required wavelength/velocity precision.

!

  question:        7
    section:       1
    line_1:        To support the important HST observations several types of concurrent
    line_2:        ground-based observations will be made. (1) The Swedish wing of the team will
    line_3:        make radio observations of circumstellar gas through CO and HCN lines
    line_4:        (Olofsson, et al., 1987, Astr. Ap., 183, 43) and high-resolution (120,000)
    line_5:        spectroscopic observations of CS matter in the Na D and K I resonance lines
    line_6:        with the new HRS at the Nordic Optical 2.5-m telescope at La Palma.  (2) the
    line_7:        French and Ohio State groups will make concurrent ground-based, high-resolution
    line_8:        spectra in the visual region and ultraviolet regions.  We have already
    line_9:        obtained spectra of the CO fundamental lines in TX Psc, and we hope to
    line_10:       obtain similar spectra for the other stars.
    line_12:       The analysis will proceed in several steps.
    line_14:       (1)  The initial data reduction, calibration, and analysis of the observations
    line_15:       will be done by the GSFC/CSC group (Carpenter, Robinson).  The raw data files
    line_16:       will be wavelength-calibrated using the explicit WAVE observations obtained
    line_17:       along with the science data and transformed onto an absolute flux scale using
    line_18:       the latest radiometric calibration of the GHRS.  Software and techniques
    line_19:       developed by the GHRS IDT will be used to optimize these calibrations. Copies
    line_20:       of both the raw and calibrated spectra will then be sent to all investigators,
    line_21:       and analysis will proceed through parallel and cooperative, independent
    line_22:       ventures.

!

  question:        7
    section:       2
    line_1:        (2) The GSFC/CSC group will perform the initial measurement and analysis of the
    line_2:        UV data, obtaining observed wavelengths, line widths, and detailed line
    line_3:        profiles.  From these results we will infer the turbulent and flow velocities
    line_4:        and velocity gradients in the stellar chromosphere and wind.   This information
    line_5:        will be combined with velocities from visual and radio observations and
    line_6:        deductions from the mass loss rate and mass continuity to yield as complete a
    line_7:        picture as possible of the velocity structure of the photospheric,
    line_8:        chromospheric, and CS regions.  The GSFC/CSC, Boulder, Swedish, and Ohio State
    line_9:        groups will participate.
    line_11:       (3) Photospheric models, including polyatomic molecular opacities, in both
    line_12:       plane-parallel and spherical geometry, will be computed for both carbon stars
    line_13:       and M stars by the Midwest, Danish, French, and Swedish groups.  This will
    line_14:       include experimentation with two-component models.  The SAO group will make
    line_15:       detailed comparisons of synthetic spectra with visual observations, and the
    line_16:       Danish and Swedish groups will do the same in the red and infrared regions.
    line_18:       (4) Careful modeling of the chromospheric temperature structure will be
    line_19:       undertaken, beginning with a carbon star.  (However, to compute
    line_20:       inhomogeneous NLTE models for both C and M stars will surely require
    line_21:       several years.)  A best theoretical photosphere-chromosphere model (including
    line_22:       departures from LTE) will be selected by comparison of predicted fluxes with
    line_23:       observations of both lines and continua.  The Boulder, Indiana, Iowa State,

!

  question:        7
    section:       3
    line_1:        Goddard, and Smithsonian groups currently possess the necessary programs for
    line_2:        NLTE chromospheric modeling, and these groups will work in parallel and in
    line_3:        collaboration in checking NLTE results in this extremely complex research.
    line_5:        (5) At Smithsonian synthetic spectra in the visual and ultraviolet
    line_6:        regions will be calculated and carefully compared to observations.
    line_7:        Comparisons of capacities in red giants and the sun will be made.
    line_9:        (6) Results will be published in a timely fashion.

!

  question:        8
    section:       1
    line_1:
    line_2:        None.

!

  question:        9
    section:       1
    line_1:        part a)
    line_2:        HST GTO Programs on which Carpenter is PI:
    line_4:        GTO 1195:  Outer Atmospheres of Cool Luminous Stars - Cycle 0 (Alpha Ori)
    line_5:        3212:  Outer Atmospheres of Cool Luminous Stars - Cycle 1 (Gamma Cru)
    line_7:        GTO 1198:  Physical Conditions and Velocity Structures in the Red Giant
    line_8:        3934:  Winds in the Binaries CI Cyg and EG And - Cycle 2 (2 targets)
    line_10:       GTO 1199:  Alpha Ori Team Project - Cycle 1
    line_12:       HST GTO programs on which Linsky is PI:
    line_14:       GTO 1175/3943:  Local Interstellar Medium and D/H Ratio
    line_16:       GTO 1176/3964:  The dynamics of stellar chromospheres & transition regions
    line_18:       GTO 1177:  Atmospheres of very inactive K giant stars
    line_20:       GTO 1179/3961:  Hybrid-chromosphere stars
    line_22:       GTO Program 1180:  The chromospheres of the very coolest M dwarf stars

!

  question:        9
    section:       2
    line_1:        HST Programs on which Linsky and/or Carpenter are Co-I's:
    line_2:        :
    line_3:        GTO 1210:  Age dependence of non-radiative heating in stellar chromospheres
    line_5:        GO 2238:  Lyman-ALPHA Observations Of High Radial Velocity Stars
    line_7:        GO 2321:  Search for proton acceleration in flare stars - AU Mic
    line_9:        GO 3626:  Empirical determination of the wind velocity and density laws
    line_10:       for the K supergiant Zeta Aurigae from eclipse ingress spectra
    line_12:       HST programs on which Gustafsson is Co-I:
    line_14:       GO P3479:  Boron in Pop II Dwarfs
    line_16:       THERE ARE NO OBSERVATIONS OF CARBON STARS IN THESE GTO PROGRAMS.
    line_18:       The only M-giant included in these GTO programs is Gamma Cru, in GTO 3212 - a
    line_19:       cycle 1 program which executed late in that cycle.  The observations cover a
    line_20:       broader range of wavelengths and purposes than those planned for the M-stars in
    line_21:       this GO proposal, but they do not include a satisfactory match to the
    line_22:       carbon-star observations for our detailed comparison purposes.

!

  question:        9
    section:       3
    line_1:        SAO program 3023 (Alpha Tau) observations have been used to assess the
    line_2:        feasibility of programs such as these which involve observations of narrow
    line_3:        emission-line sources (see the Ap.J. reference below).
    line_4:        Part b)
    line_5:        The observations of Alpha Tauri in SAO 3023 provided the first direct
    line_6:        measurement of the turbulence in the chromosphere of a cool giant (K5 III), the
    line_7:        discovery of a downflow of the C II] chromospheric plasma, the detection of 25
    line_8:        new emission features in the 2320-2370 A region, and the first evidence for
    line_9:        optically thin emission lines (of CII 2335A) that have extended wings.  Other
    line_10:       results are summarized in the papers listed in part (c).
    line_12:       Highlights of Carpenter GTO (Programs 1195/3212) and SAO results include:
    line_13:       1) the unambiguous detection of a far-UV continuum in Alpha Ori and Gamma Cru,
    line_14:       which will provide a very important and previously unrecognized diagnostic of
    line_15:       their chromospheric plasmas (formation temperature in Alpha Ori ranges from
    line_16:       3500-5000 K and increases steadily with decreasing wavelength); 2) the
    line_17:       discovery of circumstellar CO (4th positive A-X system) absorption bands
    line_18:       superposed on the far-UV continuum from Alpha Ori, providing a probe of regions
    line_19:       of the circumstellar shell not available at visible or IR wavelengths (initial
    line_20:       analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 cm-2); 3) detection of
    line_21:       myriad new Fe II fluorescent line products, producing by Lyman Alpha radiation
    line_22:       in Alpha Ori; 4) a determination that, in Alpha Ori, the resonance lines of OI
    line_23:       and CI are very weak due to self-absorption and that the asymmetries seen in

!

  question:        9
    section:       4
    line_1:        the MgII resonance lines are probably due to different velocity shifts between
    line_2:        the self-absorption and emission in the two lines; and 5) the first direct
    line_3:        measurement of the chromospheric turbulence (24 km/sec) and the detection of a
    line_4:        downflow of about 4 km/sec in chromospheric C II] plasma in Alpha Tau.  High
    line_5:        quality observations of Gamma Cru in program 3212 have recently been acquired
    line_6:        and detailed analysis is now in progress.
    line_8:        GTO Program 1175: Linsky and collaborators obtained SSA echelle spectra of
    line_9:        Capella in the Lyman alpha, FeII, and MgII lines on 15 April 1991. The purpose
    line_10:       was to obtain very accurate measurements of the D/H ratio and interstellar
    line_11:       properties for the 12.5-pc line of sight towards this star. They derived the
    line_12:       ratio D/H = 1.65 (+0.07 -0.18) x 10e-5, temperature 7000 (+/- 200) K, and
    line_13:       turbulent velocity of 1.66 (+/-0.03) km/s. The local D/H ratio was used to
    line_14:       infer the primordial value which is a major constraint on models of the early
    line_15:       universe. Observations of Alpha Cen A and B, Procyon, HR 1099, and a
    line_16:       reobservation of Capella are planned.
    line_18:       GTO Program 1176: Low and moderate dispersion GHRS spectra of Capella were
    line_19:       obtained on 15 April 1991 and of Beta Draconis on 23 April 1992. The Capella
    line_20:       observations show downflowing transition region gas from both stars in the
    line_21:       system and intersystem lines of many different ions that allow the
    line_22:       determination of the electron density as a function of the temperature of the
    line_23:       emitting plasma. Observations of Procyon, Epsilon Eri, HR 1099, and Alpha Cen A

!

  question:        9
    section:       5
    line_1:        and B are planned. The Beta Draconis data are being analyzed.
    line_3:        SV observations of Gamma Draconis obtained on 6 April 1991 by Carpenter et al.
    line_4:        provide clear evidence of such high temperature lines as CIV and SIIV in the
    line_5:        atmosphere of this hybrid-chromosphere star. The surface fluxes in the 100,000
    line_6:        K plasma lines are the smallest ever observed in any star.
    line_8:        GO Program 2321: Evidence for proton beams was obtained by Woodgate et
    line_9:        al. from
    line_10:       GHRS spectra of AU Mic during a flare. This discovery was described
    line_11:       in a recent NASA press release and in an ApJ paper.
    line_13:       There have been no observations yet in any of the other programs.
    line_15:       Part c)
    line_16:       Results have been presented:  in the Ap.J. & MNRAS, at AAS meeting (1/91, 5/91
    line_17:       & 1/92), the HST Joint Discussion at the IAU General Assembly (7/91), the 7th
    line_18:       Cambridge Cool Star Workshop (10/91), and at both HST Workshops (5/91 & 7/92),
    line_19:       including two invited reviews (AAS 1/91 and Cool Star Workshop 10/91).
    line_21:       "First Results from the Goddard High Resolution Spectrograph:  The Chromosphere
    line_22:       of Alpha Tauri",  Carpenter, K. G., Robinson, R., Wahlgren, G., Ake, T., Linsky,
    line_23:       J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991.

!

  question:        9
    section:       6
    line_1:        "Si II Emission Line Diagnostics,"  Judge, P. G., Carpenter, K. G., and
    line_2:        Harper, G.M., MNRAS, 253, 123, 1991.
    line_4:        "Early Scientific Results from the Goddard High Resolution Spectrograph"
    line_5:        Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91.
    line_7:        "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau"
    line_8:        Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J.,
    line_9:        in `The First Year of HST Observations,' 1991.
    line_11:       "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly
    line_12:       Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91.
    line_14:       "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G.,  in
    line_15:       `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar  Systems, and
    line_16:       the Sun,' in press, 1992.
    line_18:       "Molecular Absorption in the UV Spectrum of Alpha Ori,"  Wahlgren, G. M.,
    line_19:       Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh
    line_20:       Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ed. M. Giampapa
    line_21:       and J. Bookbinder, A.S.P. Conference Series, in press, 1992.

!

  question:        9
    section:       7
    line_1:        "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with the
    line_2:        Goddard High Resolution Spectrograph,"  Carpenter, K. G.,  Robinson, R. D.,
    line_3:        Wahlgren, G. M., Linsky, J. L., Brown, A.,  in  Science with the Hubble
    line_4:        Space Telescope (European Southern Observatory), eds. P. Benvenuti and
    line_5:        E. Schreier, in press, 1992.
    line_7:        "The Far-UV Spectrum of alpha Ori,"  Carpenter, K. G., Robinson, R. D.,
    line_8:        Wahlgren, G. M., Linsky, J.L., and Brown, A., Ap. J., submitted, 1992.
    line_10:       `GHRS observations of the local interstellar medium and the deuterium/hydrogen
    line_11:       ratio along the line of sight towards Capella,' Linsky, J.L., Brown, A.,
    line_12:       Gayley, K., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, S.,
    line_13:       and Heap, S. R., Astrophysical Journal, to appear 10 Jan 1993.
    line_15:       `The hydrogen Lyman alpha emission of Capella', Ayres, T.R., Brown, A., Gayley,
    line_16:       K.G., and Linsky, J.L., Astrophysical Journal, to appear 10 Jan 1993.
    line_18:       `GHRS Far-ultraviolet spectra of coronal and noncoronal stars: Capella and
    line_19:       Gamma Draconis', Linsky, J.L., Brown, A., and Carpenter, K.G., in The First
    line_20:       Year of HST Observations, ed. A.L. Kinney and J.C. Blades (Baltimore: Space
    line_21:       Telescope Science Institute), p. 70 (1991).
    line_23:       `The Deuterium abundance in the local interstellar medium', Linsky, J.L.to

!

  question:        9
    section:       8
    line_1:        appear in Highlights of the IAU, Vol. 9.
    line_3:        `Ultraviolet observations of stellar coronae: early results from HST', Linsky,
    line_4:        J.L., to appear in Memorie della Societa Astronomica Italiana.
    line_6:        `Ultraviolet observations of stellar coronae; early results from the Hubble
    line_7:        Space Telescope', Linsky, J.L., IAU Joint Commission VI on `Solar and Stellar
    line_8:        Coronae', Buenos Aires, Argentina, to be published.
    line_10:       `Deuterium abundance in the local interstellar medium', Linsky, J.L. in IAU
    line_11:       Joint Discussion VII on `First Results from the Hubble Space Telescope', Buenos
    line_12:       Argentina, to be published.
    line_14:       `GHRS observations of the local interstellar medium and the deuterium/hydrogen
    line_15:       ratio toward Capella', Linsky, J.L., in Science with the Hubble Space
    line_16:       Telescope (European Southern Observatory), in press.
    line_18:       `New stellar plasma determinations by the GHRS: The transition regions of
    line_19:       Capella and Gamma Draconis', Linsky, J.L., Wood, B., and Brown, A., in Science
    line_20:       with the Hubble Space Telescope (European Southern Observatory), in press.

!

  question:        10
    section:       1
    line_1:        Indiana University (I.U.) has been very generous in providing much time on its
    line_2:        computing facilities.  Programs, data, and facilities for computing model
    line_3:        atmospheres are in use at I.U., Wichita, Copenhagen, Toulouse, and Uppsala.
    line_4:        Programs for constructing non-LTE model chromospheres are available at HAO,
    line_5:        JILA, Iowa St., GSFC, and Smithsonian.  Radio and optical telescopes for
    line_6:        concurrent observations are available in Sweden, France, ESO-La Silla, and the
    line_7:        United States (Ohio State U.). Software developed by the GHRS IDT will be
    line_8:        available at NASA-GSFC, as well as VAX computing facilities, for reduction and
    line_9:        measurement of GHRS and FOS spectra.

!
!end of general form text

general_form_address:

  lname:           JOHNSON
    fname:         HOLLIS
    mi:            R.
    category:      PI
    inst:          Indiana University
    addr_1:        ASTRONOMY DEPT., SW 319
    city:          BLOOMINGTON
    state:         IN
    zip:           47405
    country:       USA
    phone:         (812)-855-6915
    telex:         272-279

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        HD223075
    name_2:        TX-PSC
    descr_1:       A,144
    pos_1:         RA=23H46M23.525S+/-1.0",
    pos_2:         DEC=+03D29'12.5"+/-1.0"
    equinox:       2000.0
    pm_or_par:     Y
    pos_epoch_bj:  J
    pos_epoch_yr:  2000.00
    ra_pm_val:     -0.002004
    ra_pm_unct:    0.000067
    dec_pm_val:    -0.0250
    dec_pm_unct:   0.0010
    rv_or_z:       V=+11
    comment_1:     (N0;  C6,2) CARBON STAR
    fluxnum_1:     1
    fluxval_1:     V=5.04,TYPE=NOC62
    fluxnum_2:     2
    fluxval_2:     F(2799)=2.0E-14

!

    targnum:       2
    name_1:        HD46687
    name_2:        UU-AUR
    descr_1:       A,144
    pos_1:         RA=06H36M32.83S+/-1.0",
    pos_2:         DEC=+38D26'43.8"+/-1.0"
    equinox:       2000.0
    pm_or_par:     Y
    pos_epoch_bj:  J
    pos_epoch_yr:  2000.00
    ra_pm_val:     -0.000851
    ra_pm_unct:    0.000085
    dec_pm_val:    -0.0170
    dec_pm_unct:   0.0010
    rv_or_z:       V=+12
    comment_1:     (N3;  C5,3) CARBON STAR
    fluxnum_1:     1
    fluxval_1:     V=5.29,TYPE=N3C53
    fluxnum_2:     2
    fluxval_2:     F(2799)=8.7E-15

!

    targnum:       3
    name_1:        HD44478
    name_2:        MU-GEM
    descr_1:       A,142
    pos_1:         RA=06H22M57.62S+/-1.0",
    pos_2:         DEC=+22D30'48.8"+/-1.0"
    equinox:       2000.0
    pm_or_par:     Y
    pos_epoch_bj:  J
    pos_epoch_yr:  2000.00
    ra_pm_val:     0.003969
    ra_pm_unct:    0.000072
    dec_pm_val:    -0.1120
    dec_pm_unct:   0.0010
    rv_or_z:       V=+14
    comment_1:     (M3 III COMPARISON STAR)
    fluxnum_1:     1
    fluxval_1:     V=2.88,TYPE=M3-III
    fluxnum_2:     2
    fluxval_2:     F(2799)=2.50E-13

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      HD223075
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      4.3
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  1.0S
    priority:      1
    req_1:         CYCLE 3 / 1.0-44.0;
    req_2:         ONBOARD ACQ FOR 1.1;
    req_3:         SPATIAL SCAN;
    req_4:         SEQ 1-2 NO GAP;
    req_5:         GROUP 1-6 WITHIN 2D
    comment_1:     TX PSC IS COMMON NAME OF OBJECT

!

    linenum:       1.100
    targname:      HD223075
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      1.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  2.0S
    priority:      1
    req_1:         ONBOARD ACQ FOR 1.2;
    req_2:         SPATIAL SCAN;

!

    linenum:       1.200
    targname:      HD223075
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      0.5
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  3.0S
    priority:      1
    param_1:       SCAN-STEP-X=0.35,
    param_2:       SEARCH-SIZE-X=3,
    param_3:       SCAN-STEP-Y=0.35,
    param_4:       SEARCH-SIZE-Y=3
    req_1:         ONBOARD ACQ FOR 1.3;

!

    linenum:       1.300
    targname:      HD223075
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      0.25X2.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  10.0S
    priority:      1
    req_1:         ONBOARD ACQ FOR 2.0;
    req_2:         SPATIAL SCAN;

!

    linenum:       2.000
    targname:      HD223075
    config:        FOS/RD
    opmode:        ACCUM
    aperture:      0.25X2.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       3
    time_per_exp:  5.0M
    priority:      1

!

    linenum:       3.000
    targname:      HD223075
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  40.0S
    fluxnum_1:     1
    priority:      1
    param_1:       LOCATE=YES,
    param_2:       BRIGHT=RETURN,
    param_3:       SEARCH-SIZE=5
    req_1:         ONBOARD ACQ FOR 4.000;
    req_2:         SEQ 3 - 6
    comment_1:     USE STEP-TIME = 1.6 SEC.
    comment_2:     EXPECT ROUGHLY 640-1120 CTS/1.6S

!

    linenum:       4.000
    targname:      HD223075
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      0.25
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  60S
    fluxnum_1:     1
    priority:      1
    req_1:         ONBOARD ACQ FOR 5.0-6.0
    comment_1:     STEP-TIME = 2.4 SEC (FROM SIB)

!

    linenum:       5.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    ECH-B
    wavelength:    2799
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 6 NO SLEW;
    req_2:         SEQ 5-6 NO GAP

!

    linenum:       6.000
    targname:      HD223075
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    ECH-B
    wavelength:    2799
    num_exp:       24
    time_per_exp:  10.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=7,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 24 EXP'S.

!

    linenum:       11.000
    targname:      HD46687
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      4.3
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  1.0S
    priority:      1
    req_1:         CYCLE 3 / 1.0-44.0;
    req_2:         ONBOARD ACQ FOR 11.1;
    req_3:         SPATIAL SCAN;
    req_4:         SEQ 11-12 NO GAP;
    req_5:         GROUP 11-16 WITHIN 2D
    comment_1:     UU AUR IS COMMON NAME OF OBJECT

!

    linenum:       11.100
    targname:      HD46687
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      1.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  2.0S
    priority:      1
    req_1:         ONBOARD ACQ FOR 11.2;
    req_2:         SPATIAL SCAN;

!

    linenum:       11.200
    targname:      HD46687
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      0.5
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  3.0S
    priority:      1
    param_1:       SCAN-STEP-X=0.35,
    param_2:       SEARCH-SIZE-X=3,
    param_3:       SCAN-STEP-Y=0.35,
    param_4:       SEARCH-SIZE-Y=3
    req_1:         ONBOARD ACQ FOR 11.3;

!

    linenum:       11.300
    targname:      HD46687
    config:        FOS/RD
    opmode:        ACQ/PEAK
    aperture:      0.25X2.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       1
    time_per_exp:  10.0S
    priority:      1
    req_1:         ONBOARD ACQ FOR 12.0;
    req_2:         SPATIAL SCAN;

!

    linenum:       12.000
    targname:      HD46687
    config:        FOS/RD
    opmode:        ACCUM
    aperture:      0.25X2.0
    sp_element:    G270H
    wavelength:    2750
    num_exp:       6
    time_per_exp:  5.0M
    priority:      1

!

    linenum:       13.000
    targname:      HD46687
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  80.0S
    fluxnum_1:     1
    priority:      1
    param_1:       LOCATE=YES,
    param_2:       BRIGHT=RETURN,
    param_3:       SEARCH-SIZE=5
    req_1:         ONBOARD ACQ FOR 14.000;
    req_2:         SEQ 13 - 16 NO GAP
    comment_1:     STEP-TIME = 3.2 SEC.
    comment_2:     EXPECT ABOUT 800 CTS/3.2S

!

    linenum:       14.000
    targname:      HD46687
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      0.25
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  120S
    fluxnum_1:     1
    priority:      1
    req_1:         ONBOARD ACQ FOR 15.0-16.0
    comment_1:     STEP-TIME = 4.8 SEC (FROM SIB)

!

    linenum:       15.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2810
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 16 NO SLEW;
    req_2:         SEQ 15-16 NO GAP

!

    linenum:       16.000
    targname:      HD46687
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2810
    num_exp:       28
    time_per_exp:  5.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 28 EXP'S.

!

    linenum:       33.000
    targname:      HD44478
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  80.0S
    fluxnum_1:     1
    priority:      1
    param_1:       LOCATE=YES,
    param_2:       BRIGHT=RETURN,
    param_3:       SEARCH-SIZE=5
    req_1:         ONBOARD ACQ FOR 34.000;
    req_2:         SEQ 33 - 35;
    req_3:         GROUP 33 - 44 WITHIN 1D
    comment_1:     MU GEM IS COMMON NAME FOR HD44478
    comment_2:     STEP-TIME = 3.2 SEC.
    comment_3:     EXPECT 192 CTS/3.2 SEC

!

    linenum:       34.000
    targname:      HD44478
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      0.25
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  10S
    fluxnum_1:     1
    priority:      1
    req_1:         ONBOARD ACQ FOR 35.0-44.0
    comment_1:     STEP-TIME = 0.4 SEC (FROM SIB)

!

    linenum:       35.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2810
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 36 NO SLEW;
    req_2:         SEQ 35-36 NO GAP

!

    linenum:       36.000
    targname:      HD44478
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2810
    num_exp:       2
    time_per_exp:  5.0M
    s_to_n:        12
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 2 EXP'S.

!

    linenum:       37.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2335
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 38 NO SLEW;
    req_2:         SEQ 37-38 NO GAP

!

    linenum:       38.000
    targname:      HD44478
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2335
    num_exp:       6
    time_per_exp:  5.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 6 EXP'S.

!

    linenum:       39.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2612.5
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 40 NO SLEW;
    req_2:         SEQ 39-40 NO GAP

!

    linenum:       40.000
    targname:      HD44478
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2612.5
    num_exp:       3
    time_per_exp:  5.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 3 EXP'S.

!

    linenum:       41.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2756.6
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 42 NO SLEW;
    req_2:         SEQ 41-42 NO GAP

!

    linenum:       42.000
    targname:      HD44478
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2756.5
    num_exp:       3
    time_per_exp:  5.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 3 EXP'S.

!

    linenum:       43.000
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    G270M
    wavelength:    2850
    num_exp:       1
    time_per_exp:  30S
    priority:      1
    param_1:       STEP-PATT=3
    req_1:         CALIB FOR 44 NO SLEW;
    req_2:         SEQ 43-44 NO GAP

!

    linenum:       44.000
    targname:      HD44478
    config:        HRS
    opmode:        ACCUM
    aperture:      0.25
    sp_element:    G270M
    wavelength:    2850
    num_exp:       3
    time_per_exp:  5.0M
    s_to_n:        10
    fluxnum_1:     2
    priority:      1
    param_1:       STEP-PATT=5,
    param_2:       FP-SPLIT=NO
    comment_1:     S/N IS FOR SUM OF 5 FP-SPLIT EXP'S.

!
! end of exposure logsheet

scan_data:

    line_list:     1.0,11.0
    fgs_scan:
    cont_dwell:    D
    dwell_pnts:    3
    dwell_secs:       1.00
    scan_width:       0.0000
    scan_length:      2.8000
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0000
    first_line_pa:   0.0000
    scan_frame:    S/C
    len_offset:    1.400
    wid_offset:    0.0

!

    line_list:     1.1,11.1
    fgs_scan:
    cont_dwell:    D
    dwell_pnts:    6
    dwell_secs:       1.00
    scan_width:       0.7000
    scan_length:      3.5000
    sides_angle:    90.0000
    number_lines:  2
    scan_rate:       0.0000
    first_line_pa:  90.0000
    scan_frame:    S/C
    len_offset:    1.750
    wid_offset:    0.350

!

    line_list:     1.3,11.3
    fgs_scan:
    cont_dwell:    D
    dwell_pnts:    7
    dwell_secs:       1.00
    scan_width:       0.0000
    scan_length:      0.4000
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0000
    first_line_pa:  90.0000
    scan_frame:    S/C
    len_offset:    0.200
    wid_offset:    0.0

!
! end of scan data