! $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