!   $Id: 5414,v 10.1 1994/09/13 19:10:46 pepsa Exp $

coverpage:

  title_1:         DAYGLOW EMISSION LINE PROFILES FROM THE OUTER PLANETS
    title_2:       CYCLE4-MED
    sci_cat:       SOLAR SYSTEM
    sci_subcat:    GIANT PLANETS
    proposal_for:  GO
    pi_fname:      JOHN
    pi_mi:         T.
    pi_lname:      CLARKE
    pi_inst:       UNIVERSITY OF MICHIGAN
    pi_country:    USA
    pi_phone:      313-747-3540
    hours_pri:     7.70
    num_pri:       6
    hrs:           Y
    realtime:      Y
    time_crit:     Y
    off_fname:     NEIL
    off_lname:     GERL
    off_title:     PROJECT REP., DRDA
    off_inst:      2660
    off_addr_1:    475 E. JEFFERSON
    off_city:      ANN ARBOR
    off_state:     MI
    off_zip:       48109
    off_country:   USA
    off_phone:     313-763-6438
! end of coverpage

abstract:

    line_1:        Recent IUE observations of the H Ly alpha emission line profile
    line_2:        from Jupiter's dayglow and aurora reveal a substantial line broadening,
    line_3:        implying that the observed high brightness is due to resonant
    line_4:        scattering of solar emission with a broad line rather than charged
    line_5:        particle excitation.  This may reflect highly energetic processes
    line_6:        producing a 5-10 km/sec suprathermal population of H atoms in Jupiter's
    line_7:        upper atmosphere, which in turn may be related to the unresolved question
    line_8:        of the high exospheric temperatures of 400-1200 K detected on all 4 giant
    line_9:        planets during the Voyager encounters.  It is clear that if the bright H
    line_10:       Ly alpha emissions from the outer planets are due mainly to resonant
    line_11:       scattering of solar and interplanetary emissions, as observed
    line_12:       on Jupiter and Saturn from long term correlations with the solar
    line_13:       Ly alpha flux, then the lines from all 4 planets must be broad to
    line_14:       explain the observed high albedos.  The H Ly alpha lineshapes provide
    line_15:       a discriminant between the processes of resonant scattering and
    line_16:       charged particle excitation.  We propose to obtain high signal to noise
    line_17:       H Ly alpha line profile measurements from Saturn, Uranus, and Neptune
    line_18:       to resolve the questions about the excitation processes for the bright
    line_19:       airglow emissions.
    line_20:       ALL SATURN OBSERVATIONS HAVE BEEN MOVED TO A NEW PROPOSAL.

!
! end of abstract

general_form_proposers:

  lname:           CLARKE
    fname:         JOHN
    mi:            T.
    inst:          2660
    country:       USA

!

  lname:           BEN JAFFEL
    fname:         LOTFI
    inst:          5436
    country:       FRANCE
    esa:           Y

!

  lname:           GLADSTONE
    fname:         RANDALL
    inst:          3440
    country:       USA

!

  lname:           PRANGE
    fname:         RENEE
    inst:          5448
    country:       FRANCE
    esa:           Y

!

  lname:           VIDAL-MADJAR
    fname:         ALFRED
    inst:          5436
    country:       FRANCE
    esa:           Y

!

  lname:           WAITE
    fname:         HUNTER
    inst:          3440
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        We request 6 dark orbit spectra, with two spectra each for Saturn and
    line_2:        Uranus and one for Neptune.  The Saturn observations  will consist of center
    line_3:        to limb scans with the GHRS LSA (echelle A at 1215.7 A), with scans E/W and
    line_4:        N/S from the planet center to the limb.  The scan across the north pole will
    line_5:        be important to reveal any line broadening associated with the polar aurora,
    line_6:        as has been observed on Jupiter, and the E/W scan will show the changing line
    line_7:        shape with the increased slant column near the limb.  The 2 arc sec LSA is
    line_8:        somewhat smaller than Uranus (3.8 arc sec diameter) and Neptune (2.4
    line_9:        arc sec diameter), although it is filled by both planets, and planet-
    line_10:       center spectra will be taken of each.  In addition, one spectrum will be
    line_11:       obtained near the limb of Uranus where the magnetic pole is presently
    line_12:       rotating in and out of the field of view from the Earth.  Since the
    line_13:       rotational ephemeris for Uranus is insufficiently accurate to determine
    line_14:       the longitude system today, we will have to take our chances on the
    line_15:       location of any auroral emission near the pole.  Since the emissions from
    line_16:       Neptune are closer to the background brightness, planet and sky background
    line_17:       spectra will be taken.  Saturn can be acquired by blind offset from guide
    line_18:       stars, and GHRS autonomous acquisitions of satellites will be used for
    line_19:       offsets to Uranus and Neptune.

!

  question:        4
    section:       1
    line_1:        As described above, we are also pursuing this program with IUE observa-
    line_2:        tions of Jupiter, Saturn, and Uranus: Neptune is too faint for IUE at high
    line_3:        resolution.  The observations are limited by much lower sensitivity, and
    line_4:        roughly a factor of two lower spectral resolution, of IUE compared with the
    line_5:        GHRS echelle A and LSA.  The existing IUE data with the SWP camera and small
    line_6:        aperture at high dispersion are shown by Clarke et al. (1991).  Longer
    line_7:        exposures are possible with IUE, but Jupiter's rotation of 36 degrees/hour
    line_8:        limits observations of specific longitude regions to 2-3 hours.  The GHRS
    line_9:        spectral capabilities will allow us to obtain high quality H Ly alpha
    line_10:       line profiles of regions on Saturn, and determine the full line shapes
    line_11:       (including the important wings).  With the 2 arc sec GHRS LSA we will also
    line_12:       obtain sub-solar + auroral latitude spectra of Uranus with good sensitivity
    line_13:       in the wings, and we expect to get a basic line width measurement of the
    line_14:       fainter emission from Neptune.  From our experience with IUE spectra at low
    line_15:       signal to noise, we have determined that the H Ly alpha profile of Jupiter
    line_16:       is very broad, and the high Ly alpha albedos of Saturn and Uranus require
    line_17:       similarly broad lines if the dominant emission process is RS of solar and
    line_18:       IPM Ly alpha.  Neptune is the one case where the emission is sufficiently
    line_19:       faint that the line may be narrow, and we wish to make this observation for
    line_20:       comparison with the other 3 planets.

!

  question:        5
    section:       1
    line_1:        We need to minimize the sky background subtraction, which involves
    line_2:        minimizing the geocoronal background Ly alpha emission by observing
    line_3:        near opposition.  We also need some minimum Doppler shift between
    line_4:        the planetary and geocoronal emissions from observing near roughly
    line_5:        30-60 degrees from the anti-solar point, so that the combined Earth and HST
    line_6:        orbital motions of 38 km/sec have large components along the line of sight
    line_7:        during the dark portion of the HST orbit when the background is minimal.
    line_8:        This will allow us to separate spectrally the geoc. and planetary emissions.
    line_9:        PLEASE NOTE: several parameters in the exposure list will need to be
    line_10:       adjusted depending on the dates of observations, for Saturn and Uranus.
    line_11:       PLEASE CONTACT THE PI WHEN THE WEEK OF OBSERVING IS SET to check this.
    line_12:       The observation requires that the grating tilt should be kept same
    line_13:       for the WAVE calibration as one of the scientific exposures in each group,
    line_14:       for the targets, Saturn, Uranus, and Neptune. This means NO SPYBAL
    line_15:       OPERATIONS SHOULD TAKE PLACE IN BETWEEN THE SCIENTIFIC EXPOSURES AND THE 
    line_16:       WAVE CALIBRATION.  


!

  question:        6
    section:       1
    line_1:        None.

!


!

  question:        8
    section:       1
    line_1:        None.

!

  question:        9
    section:       1
    line_1:        There are a total of 21 programs in cycles 1-3, resulting in
    line_2:        (to date) nine publications.  Several more publications are in
    line_3:        the process of being submitted and/or reviewed.

!

  question:        10
    section:       1
    line_1:        Complete computing facilities are in place and available within the Space
    line_2:        Physics Research Laboratory at the University of Michigan for use on this
    line_3:        project.  Two VAX 750's and a VAX 8600 are accessible via a local area
    line_4:        network, in addition to the Michigan network MERIT, SPAN, and Internet.
    line_5:        Three Sun Sparcstations with IDL are presently being used for IUE and
    line_6:        HST data reductions.  All Co-Investigators also have complete computer
    line_7:        facilities available at their institutions for use on this project, and
    line_8:        graduate students are available at all institutions for assistance with
    line_9:        this project.

!
!end of general form text

general_form_address:

  lname:           Clarke
    fname:         John
    mi:            T.
    category:      PI
    inst:          2660
    addr_1:        AOSS Department
    addr_2:        2455 Hayward
    city:          Ann Arbor
    state:         MI
    zip:           481092143
    country:       USA
    phone:         313-747-3540

!
! end of general_form_address records

! No fixed target records found

solar_system_targets:
!

  targnum:         3
    name_1:        TITANIA-ACQ
    descr_1:       SATELLITE TITANIA
    lev1_1:        STD = URANUS, ACQ = 0.25
    lev2_1:        STD = TITANIA
    wind_1:        OLG OF URANUS BETWEEN 300 330,
    wind_2:        SEP OF OBERON TITANIA FROM EARTH
    wind_3:        GT 10", SEP OF UMBRIEL TITANIA FROM
    wind_4:        EARTH GT 10", SEP OF ARIEL TITANIA
    wind_5:        FROM EARTH GT 10"
    comment_1:     ON-BOARD ACQUISITION OF TITANIA
    comment_2:     FOR OFFSET TO URANUS.
    fluxnum_1:     1
    fluxval_1:     V = 13.7

!

  targnum:         4
    name_1:        URANUS-CENTER
    descr_1:       PLANET URANUS
    lev1_1:        STD = URANUS, ACQ = 0.25
    wind_1:        OLG OF URANUS BETWEEN 300 330
    comment_1:     OBSERVE URANUS AT PLANET CENTER.
    comment_2:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_3:     LINE WHEN URANUS OLG = 300-330
    comment_4:     DEGREES.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 8.0
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1216) = 3. +/- 1. E-12
    fluxnum_3:     3
    fluxval_3:     W-LINE(1216) = 0.2 +/- 0.15

!

  targnum:         5
    name_1:        URANUS-AUR
    descr_1:       OFFSET URANUS
    lev1_1:        STD = URANUS, ACQ = 0.25
    lev2_1:        TYPE=POS_ANGLE, REF=NORTH,
    lev2_2:        ANG = 275., RAD=1.4
    wind_1:        OLG OF URANUS BETWEEN 300 330
    comment_1:     OBSERVE URANUS NEAR LIMB WHERE
    comment_2:     AURORAL EMISSION IS EXPECTED.
    comment_3:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_4:     LINE WHEN URANUS OLG = 300-330
    comment_5:     DEGREES. NOTE: RAD DEPENDS ON
    comment_6:     DAY OF OBSERVATION.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 8.0
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1216) = 3. +/- 1. E-12
    fluxnum_3:     3
    fluxval_3:     W-LINE(1216) = 0.2 +/- 0.15

!

  targnum:         6
    name_1:        TRITON-ACQ
    descr_1:       SATELLITE TRITON
    lev1_1:        STD = NEPTUNE, ACQ = 0.25
    lev2_1:        STD = TRITON
    wind_1:        OLG OF NEPTUNE BETWEEN 300 330
    wind_2:        OLG OF NEPTUNE BETWEEN 30 60
    comment_1:     ON-BOARD ACQUISITION OF TRITON
    comment_2:     FOR OFFSET TO NEPTUNE.
    fluxnum_1:     1
    fluxval_1:     V = 13.5

!

  targnum:         7
    name_1:        NEPTUNE
    descr_1:       PLANET NEPTUNE
    lev1_1:        STD = NEPTUNE, ACQ = 0.25
    wind_1:        OLG OF NEPTUNE BETWEEN 300 330
    wind_2:        OLG OF NEPTUNE BETWEEN 30 60
    comment_1:     OBSERVE NEPTUNE AT PLANET CENTER.
    comment_2:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_3:     LINE. NEPTUNE OLG = 300-330 OR 30-
    comment_4:     60 DEGREES.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 9.0
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1216) = 0.6 +/- 0.6 E-12
    fluxnum_3:     3
    fluxval_3:     W-LINE(1216) = 0.1 +/- 0.05

!

  targnum:         8
    name_1:        NEPTUNE-OFFSET-SKY
    descr_1:       OFFSET NEPTUNE
    lev1_1:        STD = NEPTUNE
    lev2_1:        TYPE=POS_ANGLE, REF=NORTH,
    lev2_2:        ANG = 0, RAD=60
    wind_1:        OLG OF NEPTUNE BETWEEN 300 330
    wind_2:        OLG OF NEPTUNE BETWEEN 30 60
    comment_1:     OBSERVE SKY BACKGROUND GEO AND IPM
    comment_2:     LY ALPHA EMISSIONS NEAR NEPTUNE.
    comment_3:     OFFSET NORTH BY 1 ARC MINUTE.
    comment_4:     ALSO GIVES SKY BACKGROUND FOR
    comment_5:     SATURN AND URANUS, SO PLEASE
    comment_6:     SCHEDULE #1-8 CLOSE IN TIME.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 8.0
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1216) = 3. +/- 2. E-12
    fluxnum_3:     3
    fluxval_3:     W-LINE(1216) = .04 +/- .02

!
! end of solar system targets

! No generic target records found

exposure_logsheet:



!

    linenum:       4.100
    targname:      TITANIA-ACQ
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  90S
    fluxnum_1:     1
    priority:      2
    param_1:       SEARCH-SIZE=3
    req_1:         ONBOARD ACQ FOR 5;
    req_2:         GROUP 4.1-6.1 NO GAP;
    req_3:         SEQ 4.1-6 NO GAP;
    req_4:         CYCLE 4 / 4.1-9;
    comment_1:     ON-BOARD ACQ OF TITANIA WITH N2.
    comment_2:     WITH GHRS N2 - THEN OFFSET TO
    comment_3:     URANUS FOR ECH-A SPECTRA.
    comment_4:     I TAKE STEP-TIME = 10 SEC
    comment_5:     FOR 2000 COUNTS/DWELL PT.

!

    linenum:       4.200
    targname:      TITANIA-ACQ
    config:        HRS
    opmode:        IMAGE
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  350S
    fluxnum_1:     1
    priority:      3
    comment_1:     IMAGE OF TITANIA IN LSA
    comment_2:     AFTER CENTERING. EXPECT
    comment_3:     250 COUNTS MAX.

!

    linenum:       5.000
    targname:      URANUS-CENTER
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-A
    wavelength:    1215.0
    num_exp:       6
    time_per_exp:  300S
    s_to_n:        10
    s_to_n_time:   300S
    fluxnum_1:     2
    priority:      1
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME = 1.0,
    param_4:       DOPPLER = ON
    req_1:         DARK TIME / 5-6
    comment_1:     OBSERVE URANUS AT PLANET CENTER.
    comment_2:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_3:     LINE WHEN URANUS OLG = 300-330
    comment_4:     DEGREES.

!

    linenum:       6.000
    targname:      URANUS-AUR
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-A
    wavelength:    1215.0
    num_exp:       6
    time_per_exp:  300S
    s_to_n:        10
    s_to_n_time:   300S
    fluxnum_1:     2
    priority:      1
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME = 1.0,
    param_4:       DOPPLER = ON
    comment_1:     OBSERVE URANUS NEAR LIMB WHERE
    comment_2:     AURORAL EMISSION IS EXPECTED.
    comment_3:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_4:     LINE WHEN URANUS OLG = 300-330
    comment_5:     DEGREES. NOTE: RAD DEPENDS ON
    comment_6:     DAY OF OBSERVATION.

!

    linenum:       6.100
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    ECH-A
!    wavelength:    1215.5
    wavelength:    1215.0
    num_exp:       1
    time_per_exp:  2M
    s_to_n:        50
    s_to_n_time:   120S
    fluxnum_1:     1
    priority:      1
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME=1.0
    req_1:         CALIB FOR 6;
    req_2:         PCS MODE G
    comment_1:     WAVELENGTH CALIBRATION FOR 5-6.
    comment_2:     NO SPYBAL SHOULD OCCURE BETWEEN 
    comment_3:     LINE 6-6.1.

!

    linenum:       7.100
    targname:      TRITON-ACQ
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  90S
    fluxnum_1:     1
    priority:      2
    param_1:       SEARCH-SIZE=3
    req_1:         ONBOARD ACQ FOR 8;
    req_2:         GROUP 7.1-9 NO GAP;
    req_3:         SEQ 7.1-8 NO GAP
    comment_1:     ON-BOARD ACQ OF TRITON WITH N2.
    comment_2:     WITH GHRS N2 - THEN OFFSET TO
    comment_3:     NEPTUNE FOR ECH-A SPECTRA.
    comment_4:     I TAKE STEP-TIME = 10 SEC
    comment_5:     FOR 2000 COUNTS/DWELL PT.

!

    linenum:       7.200
    targname:      TRITON-ACQ
    config:        HRS
    opmode:        IMAGE
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  350S
    fluxnum_1:     1
    priority:      3
    comment_1:     IMAGE OF TRITON IN LSA
    comment_2:     AFTER CENTERING. EXPECT
    comment_3:     250 COUNTS MAX.

!

    linenum:       8.000
    targname:      NEPTUNE
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-A
    wavelength:    1215.0
    num_exp:       5
    time_per_exp:  600S
    s_to_n:        8
    s_to_n_time:   600S
    fluxnum_1:     2
    priority:      2
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME = 1.0,
    param_4:       DOPPLER = ON
    req_1:         DARK TIME
    comment_1:     OBSERVE NEPTUNE AT PLANET CENTER.
    comment_2:     GHRS ECH-A SPECTRUM OF H LY ALPHA
    comment_3:     LINE. NEPTUNE OLG = 300-330 OR 30-
    comment_4:     60 DEGREES.
    comment_5:     NO SPYBAL SHOULD OCCURE BETWEEN 
    comment_6:     LINE 8-8.1.

!

    linenum:       8.100
    targname:      WAVE
    config:        HRS
    opmode:        ACCUM
    aperture:      SC2
    sp_element:    ECH-A
!    wavelength:    1215.5
    wavelength:    1215.0
    num_exp:       1
    time_per_exp:  2M
    s_to_n:        50
    s_to_n_time:   120S
    fluxnum_1:     1
    priority:      1
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME=1.0
    req_1:         CALIB FOR 8;
    req_2:         PCS MODE G
    comment_1:     WAVELENGTH CALIBRATION FOR 8-9.

!

    linenum:       9.000
    targname:      NEPTUNE-OFFSET-SKY
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    ECH-A
    wavelength:    1215.0
    num_exp:       6
    time_per_exp:  300S
    s_to_n:        10
    s_to_n_time:   300S
    fluxnum_1:     2
    priority:      1
    param_1:       FP-SPLIT = STD,
    param_2:       STEP-PATT = 9,
    param_3:       STEP-TIME = 1.0,
    param_4:       DOPPLER = ON
    req_1:         DARK TIME
    comment_1:     OBSERVE SKY BACKGROUND GEO AND IPM
    comment_2:     LY ALPHA EMISSIONS NEAR NEPTUNE.
    comment_3:     OFFSET NORTH BY 1 ARC MINUTE.
    comment_4:     ALSO GIVES SKY BACKGROUND FOR
    comment_5:     SATURN AND URANUS, SO PLEASE
    comment_6:     SCHEDULE #1-9 CLOSE IN TIME.

!
! end of exposure logsheet