! Proposal 6692, submission 1
! PI: Lotfi Ben Jaffel
! Received Fri Feb 16 05:09:04 EST 1996
! From: lotfi@iap.fr
! Subject: 6692.prop
! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template
! $Id: 6692,v 8.1 1996/06/17 14:43:29 pepsa Exp $
! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template
! $Id: 6692,v 8.1 1996/06/17 14:43:29 pepsa Exp $
!
! Refer to the HST Phase II Proposal Instructions to fill this out
!
! Anything after a "!" is ignored, and may be deleted
!
! All keywords with multiple entries are comma delimited except the
! Visit_Requirements and Special_Requirements keywords which can be
! delimited with carriage returns or semi-colons, but not commas
!
! For help call your Program Coordinator: Manning
! Phone: 410-338-4456 , E-mail: manning@stsci.edu
!
! This partially completed template was generated from a Phase I proposal.
! Name of Phase I Proposal: archive-0772.ben_jaffel.prop
! Date generated: Fri Dec 22 16:55:11 EST 1995
!
Proposal_Information ! Section 4
Title: The abundance and distribution of deuterium on Saturn
Proposal_Category: GO
Scientific_Category: SOLAR SYSTEM
Cycle: 6
Investigators
PI_name: Lotfi Ben Jaffel
PI_Institution: Institut d'Astrophysique de Paris
CoI_Name: Darrell Strobel
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
CoI_Name: Randall Gladstone
CoI_Institution: Southwest Research Institute
Contact: ! Y or N (designate at most one contact)
CoI_Name: Alfred Vidal-Madjar
CoI_Institution: Institut d'Astrophysique de Paris
Contact: ! Y or N (designate at most one contact)
CoI_Name: Paul Feldman
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
CoI_Name: Warren Moos
CoI_Institution: Johns Hopkins University
Contact: ! Y or N (designate at most one contact)
CoI_Name: Claude Emerich
CoI_Institution: Institut d'Astrophysique Spatiale
Contact: ! Y or N (designate at most one contact)
CoI_Name: John Clarke
CoI_Institution: University of Michigan
Contact: ! Y or N (designate at most one contact)
Abstract: ! Free format text (please update)
We propose to obtain high resolution profiles of the D Lyman
alpha line emitted by the limb of the upper atmosphere Saturn,
using the GHRS Echelle A and the LSA. Our
technique consists in a radial drift of the LSA slit across
the limb of the planet. This is much like the very efficient
occultation technique although we record reflected instead of
transmitted light. As the deuterium emission is optically
thin, the analysis of the resulting profiles will provide,
through our photochemistry models and radiative transfer
calculations, the possibility for the first time to retrieve
the deuterium scale height and abundance at least in four locations
of the upper atmosphere of Saturn. Scale heights at different
locations derived from the D Ly-alpha emission, and the analysis of the
H Ly-alpha profile, obtained with each limb observation, will accurately
provide the H total column density. A precise estimate of the
D/H ratio will therefore be inferred. Recently, we
successfully applied the technique to observe the limb of
Jupiter with the medium resolution grating G160M. The inferred
D/H ratio ~ 6+/- 1 * 10^-5 seems to support the measurements
made through HD/H2 rather than CH3D/CH4. The uncertainty on
this value could be reduced if high resolution observations
with Echelle A are conducted. This should confirm the newly
derived ratio and check the D/H ratio for Saturn.
Ultimately, this will help to refine the scenario on the
formation and the evolution our Solar System 4.5 billions
years ago.
Questions ! Free format text (please update)
Observing_Description:
1. A new technique of observation, On the basis of
the available estimates of the H total content and the D/H
ratio, one can readily show that the D Ly-alpha line is
optically thin and that the Saturn planetary disk
averaged D Ly-alpha emissions cannot exceed few tens Rayleigh.
We propose a new technique of observation with the
side one echelle to derive the deuterium abundance and scale
height at least at four locations in the upper atmosphere of
the planet. For instance, let's consider, from
a theoretical point of view, the situation where the LSA is
100\% filled by the bright limb as depicted in Fig. 2.a. We
also consider an atmospheric model where the deuterium
constituent extends between the CH4 absorbing
level (located say at R_0) and an upper level (located say at
Rmax). Ignoring for the moment the H Ly-alpha emission, one
should obtain for the Ech-A resolution, a D Ly-alpha line
profile as depicted in Fig. 2.b. Here appears the strength of
GHRS. Because the line is optically thin, for each position
of the slit across the limb, there is a direct correspondence
between each 0.22" spatial region in the dispersion direction
and each of the eight diodes on which the LSA projects. The
result is that the spatial limb variation is directly
converted into clear and simple spectral variation from the
blue to the red wing of the line (see Fig. 2.b,c). Indeed,
the line being optically thin, it is not difficult to show
that the D Ly-alpha line intensity can be approximatively
written as follows:, I_D = sum\limits_i=1^8 J_i* w_i where
w_i=(n_0.H_0+n_1.H_1)/(2.cos(Psi_i)) with i=1,5,
w_6=2*(n_0.H_0)/(2.cos(Psi_6)) (the path is double for that
position), w_7=2*(n_1.H_1)/(2.cos(Psi_7)),
w_8=2*(n_2.H_1)/(2.cos(Psi_8)), with Psi_1 to Psi_8 the
observing angles, and where n_0, n_1, and n_2 are the
deuterium number densities at respectively R_0, R_1, and R_2.
J_1 to J_8 are each of the eight 0.22" region contribution to
the total signal. For a seek of clarity, we consider the
simple case where only the D scale height H_0 for the layer
embedded between R_0 and R_1 is different from H_1 the D
scale height for the region above R_1. Comparison between
theoretical models and observation will surely provide at
least the three quantities D_0 = (n_0.H_0+n_1.H_1),
D_1=n_1.H_1, and D_2=n_2.H_1 corresponding respectively to
the deuterium total column density, column density between
R_1 and R_2, and between R_2 and Rmax. Considering an
exponential variation for the D number density, it is
straightforward to show that:, H_0 = (R_1-R_0)/ln( (D_0 -
D_1)/D_1), H_1 = (R_2-R_1)/ln( D_2/D_1), n_0 = (D_0 -
D_1)/H_0, n_1 = D_1/H_1, and n_2 = D_2/H_1., Observing
with LSA and Echelle A will provide for a thin line a signal
extending over 8 diodes which may help to derive at least 4
parameters of the model. When using Ech-A, the isotopic D-H
spectral separation (~ 80 km/s) is large enough to avoid
contamination from the planet's H Ly-alpha line and the Earth
geocorona. For Jupiter, the H Ly-alpha intensity at mid-
latitude from recent GHRS data is ~ 8 kR (Clarke et al., ApJ
Lett., 430, L76 1994), and the Earth geocoronal emission is
~ 2-3 kR during dark time. We expect a 2.5 kR D Ly-alpha line
due to the limb brightening. Observing the approaching limb
will enhance even more the D Ly-alpha emission as the
incident solar D Ly-alpha photons are blue-shifted placing
the deuterium resonance close to the solar Ly-alpha blue
emission peak. This will enhance by nearly a factor 2 the
planet's D Ly-alpha line. Using the limited resolving
power of the HRS/G160M grating, the technique showed to be
very efficient even observing the dark approaching limb of
Jupiter as shown in Fig.3. The case of Saturn is somewhat more
complicated due to the absorption by the interplanetary
medium that separates the planet from Earth. During cycle 6,
we will have solar activity not too far from minimum
conditions, so that, after correction for the IPM absorption,
the Saturn H Ly-alpha emission will not exceed 1 to 2 kR
(integrated over the entire disk). Recent observations we
made, using IUE (Prange et al., IUE program 1991) and the
GHRS (Clarke et al., program ID 2556), revealed a 1.5 kR to 2
kR brightness. Near 1996 observational conditions, the
interplanetary medium will absorb in the red wing of the H Ly
-alpha line very far from the D Ly-alpha resonance wavelength
(the H-D lines separation is 80 km/s). It follows that the D
Ly-alpha line will not be disturbed by the IPM. Considering a
ratio D/H = 1.7* 10^-5 (Noll and Larson, 1991), we derive for
Saturn a sunlit limb emission at D Ly-alpha of 500 to 700
Rayleighs which corresponds to a disk integrated intensity of
50 to 70 R.,
2. Technical description of the observations,
We propose to point the approaching limb as a reference
target as depicted in Fig. 2a. To accurately locate the Ly-
alpha planet's limb, we use the procedure proposed by the STI
Moving Target Programs team for extended targets. We thus
propose to use the Onboard HRS acquisition to locate the
Saturnian satellite Rhea, shift to Saturn, and get the planetary
limb. This will lead to a total error on the limb location of
0.1 arc-sec. These estimates have been derived by K. Noll based on
already completed programs. The problem with the last
acquisition technique is that the planetary Ly-alpha limb is
not accurately defined. To handle this difficulty, we use a
well known atmospheric level (the 1 bar level, and estimate
the distance between the two planetary limbs through our radiative
transfer calculation. From our analysis, we derived that this
distance is known with an error of +/- 150 km. This corresponds
0.03 arc-sec for Saturn. Given the ~ 2
arc-sec LSA width, we are sure to get the planet's Ly-alpha
limb within the LSA field of view with an error smaller than
0.12 arc-sec. The whole technique previously presented
has been successfully used for cycle 3 observation of Jupiter
and there are no inherent obstacles (Ben Jaffel et al.,
1994). We therefore require 9 dark orbits, 7
for the LSA position across the expected planetary limb, and
the last 2 orbits for sky background. The approaching limb is
selected.
The ORIENTATION of the Telescope for planetary
targets is bimodal. Before opposition the orientation of the
U3 axis from the North is approximatively 270 degrees, and
after opposition it is approximatively 90 degrees. Based on
this, the position angle of the spin axis of Saturn, and
the orientation of the GHRS aperture, it is possible to
determine what position on the disk perimeter to point at to
align the aperture Y axis parallel to the planetary limb. Therefore,
our observation will not really constrain the spacecraft operation,
but will use the default orientation instead. However, to ensure any
departure from the nominal angle used to determine the planetary
limb, we include an ORIENT constraint, though it corresponds to the
expected orientation of the spacecraft.
3. Time exposures calculation
1 kR at 1216 Angstrom within a 2"* 0.25" solid angle (one of our
spatial-spectral bin) roughly corresponds to 1.53* 10^-14 ergs/cm^2-sec.
We expect the D Ly-alpha line to be ~ 0.04 Angstrom large which
gives a peak level of 3.83* 10^-13 ergs/cm^2-sec-Angstrom.
For Echelle A and LSA the sensitivity at 1216 Angstrom is ~
0.87* 10^11 (counts/sec-diode)/(erg/cm^2-sec-Angstrom). It
follows that for 1 kR we expect a peak rate of roughly 0.031
counts/sec-diode. For a 60 min integration time, we derived a
signal to noise S/N > 10 per kR per spectral bin i.e. S/N >
28 per kR for the LSA.
Real_Time_Justification:
We desire to obtain the maximum doppler shift between the
planetary and geocoronal emissions, and if possible to minimize
the geocoronal background Ly-alpha emission. This is accomplished
using the Earth motion, and observing Saturn no later than
July 31, 1996. Also, from our
experience using the HST/GHRS during the last years, we stress out
the importance to measure the sky-background signal in the same
conditions of observation (same range of the targets zenith angles
and sun zenith angles) than the planet. This means that the
sky-background and the planet's observations should be simultaneous
and starting with the same position of HST on its orbit.
Calibration_Justification: ! from Real_Time_Justification
As we request to acquire the limb of Saturn from the acquisition
of its satellite Rhea, we request a WAVE exposure at the beginning of
the observation of Saturn. The WAVE should be recorded on the same
position of the carrousel as when starting the planetary observation.
It is intended to monitor wavelength drifts. We ask a WAVE for each
exposure. Indeed, given the particular geometry of observation, we
cannot use the H Ly-alpha center line as a reference. Moreover,
Doppler shifts induced by thermospheric wind may occur and we would
like to avoid the confusing situation where a wavelength drift may
be interpreted as a real Doppler shift. As we request our own wave
calibration, no SPYBAL is necessary.
Additional_Comments: The success of this program is completely based on
the following conditions :
- At the time of observation, the Y axis of LSA should be parallel to
the approaching limb of the planet. The latitude of the
only region that satisfy that condition is equal to :
LATITUDE = 225D - (HST/Roll angle)
with a corresponding radius RAD = 59438 + 3929*(COS(LAT))**2
- The doppler shift between Saturn and Earth lines should be maximum
in order to not affect the weak H and D lyman-alpha lines of
Saturn. This is accomplished by observing Saturn before July 31 1996.
Solar_System_Targets ! Section 5.2
Target_Number:1
Target_Name:Rhea-Acquisition
Description:Satellite Rhea
Level_1:STD=Saturn
Level_2:STD=Rhea ! Satellite of Level_1
Window:SEP OF Rhea Saturn FROM Earth LT 60"
SEP OF Rhea Saturn FROM Earth GT 30"
SEP OF RHEA TETHYS FROM EARTH GT 10"
SEP OF RHEA DIONE FROM EARTH GT 10"
SEP OF RHEA MIMAS FROM EARTH GT 10"
SEP OF RHEA TITAN FROM EARTH GT 10"
SEP OF RHEA ENCELADUS FROM EARTH GT 10"
Flux:V=9.7
B-V=0.78 ! Include at least V and B-V
Comments:HRS ACQUISITION OF RHEA FOR PEAKUP ON SATELLITE CENTER.
LSA IS REQUIRED. FIRST STEP OF THE TECHNIQUE TO ACCURATELY
ACQUIRE THE LIMB OF SATURN DESCRIBED IN TARGNUM 2,3
Target_Number:2
Target_Name:SATURN-LIMB
Description:FEATURE SATURN
Level_1:STD=SATURN
Level_2:TYPE = TORUS, LONG = 270,
LAT = -22, RAD = 64534.,
POLE_LAT = 90
Flux:SURF(V)=7.0
SURF-LINE(1216) = 2 +/- 1 E-13
W-LINE(1216) = 0.04 +/- 0.02
Comments:THE APPROACHING LIMB IS REQUIRED.
IF, AT THE DATE OF OBSERVATION, THE HST ROLL ANGLE CHANGES,
PLEASE CHANGE THE LATITUDE AND THE RADIUS AS FOLLOWS :
LAT = 225 D - ROLL ; RAD (KM) = 59438 + 5929*(COS(LAT))**2
IN ORDER TO ALWAYS HAVE THE Y AXIS OF LSA // TO THE LIMB
Target_Number:3
Target_Name:SKY-BACKGROUND
Description:OFFSET SATURN
Level_1:STD=SATURN
Level_2:TYPE = TORUS, LONG = 270,
LAT = -22, RAD = 12000000.,
POLE_LAT = 90
Flux:SURF-LINE(1216) = 10 +/- 5 E-13
W-LINE(1216) = 0.1 +/- 0.02
Comments:SKY BACKGROUND ROUGHLY 3 ARCMIN OFF SATURN.
PLEASE SCHEDULE IMMEDIATELY AFTER SATURN OBSERVATION
IN ORDER TO AVOID SOLAR FLUX VARIATION AT 1216 A.
THE SKY OBSERVATION SHOULD START WITH HST IN THE SAME
POSITION ON ITS ORBIT AS FOR THE PLANETARY OBSERVATION.
! This is a template for a single visit containing a single exposure
! Repeat exposure and visit blocks as needed
Visits ! Section 6
Visit_Number:1
Visit_Requirements:GUIDing TOLerance 0.13" ! Section 7.1
ORIENTation 246D TO 248D
BETWEEN 1-JUL-96 AND 31-JUL-96
SEQ 1-2 WITHIN 48H
Visit_Comments:THE ORIENT REQUIREMENT ABOVE IS NOT A CONSTRAINT.
WE NEED TO CONSTRAIN THE LATITUDE FOR WHICH THE
Y AXIS OF THE LSA IS PARALLEL TO THE PLANETARY APPROACHING
LIMB. THIS LATITUDE IS DEFINED BY : LAT = 225D - ROLL
AND RAD (KM) = 58438 + 5929*(COS(LAT))**2
WE RECOMMAND TO USE THE DEFAULT ROLL BUT TO MODIFY
THE PLANETARY LAT ACCORDING TO THE FORMULAS PROVIDED ABOVE;
Visit should be completed in SEVEN consecutive orbits.
Exposure_Number:10 ! Section 6.5
Target_Name:RHEA-ACQUISITION
Config:HRS
Opmode:ACQ
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:BRIGHT=RETURN,LOCATE=EXTENDED
Number_of_Iterations:1
Time_Per_Exposure:18S
Special_Requirements:ONBOARD ACQ FOR 20 ! Section 7.2
Comments:STEP-TIME=2.0 sec
Exposure_Number:20 ! Section 6.5
Target_Name:RHEA-ACQUISITION
Config:HRS
Opmode:ACQ/PEAKUP
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:EXTENDED=YES
Number_of_Iterations:1
Time_Per_Exposure:204S
Special_Requirements:ONBOARD ACQ FOR 25-81
Comments:step-time= 2.0 sec
Exposure_Number:25 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:IMAGE
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:precision=high
Number_of_Iterations:1
Time_Per_Exposure:51.2S
Special_Requirements:SEQ 20-26 NON-INT
comments:STEP-TIME=0.2
Exposure_Number:26 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:G160M
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR
Number_of_Iterations:1
Time_Per_Exposure:326.4S
Special_Requirements:
comments:
Exposure_Number:30 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 30-33 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 31.
Exposure_Number:31 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 30.
Exposure_Number:32 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:
Comments:WAVE CALIBRATION FOR EXPOSURE 33.
Exposure_Number:33 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:652.8S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 32.
Exposure_Number:40 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 40-43 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 41.
Exposure_Number:41 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 40.
Exposure_Number:42 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:
Comments:WAVE CALIBRATION FOR EXPOSURE 43.
Exposure_Number:43 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:652.8S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 42.
Exposure_Number:50 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 50-53 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 51.
Exposure_Number:51 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 50.
Exposure_Number:52 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:
Comments:WAVE CALIBRATION FOR EXPOSURE 53.
Exposure_Number:53 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:652.8S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 52.
Exposure_Number:60 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 60-63 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 61.
Exposure_Number:61 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 60.
Exposure_Number:62 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:
Comments:WAVE CALIBRATION FOR EXPOSURE 63.
Exposure_Number:63 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:652.8S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 62.
Exposure_Number:70 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 70-71 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 81.
Exposure_Number:71 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:1414.4S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 70.
Exposure_Number:80 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 80-81 NON-INT
Comments:WAVE CALIBRATION FOR EXPOSURE 81.
Exposure_Number:81 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:1414.4S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 80.
Visits ! Section 6
Visit_Number:2
Visit_Requirements:GUIDing TOLerance 0.13"
ORIENTation 246D TO 248D
BETWEEN 1-JUL-96 AND 31-JUL-96
SEQ 1-2 WITHIN 48H
Visit_Comments:The main reason to have the observations within 48H
is to avoid lyman-alpha solar flux variation (particularly
the solar line shape) that could be catastrophic for the
isotopic D/H ratio.
Exposure_Number:14 ! Section 6.5
Target_Name:RHEA-ACQUISITION
Config:HRS
Opmode:ACQ
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:BRIGHT=RETURN,LOCATE=EXTENDED
Number_of_Iterations:1
Time_Per_Exposure:18S
Special_Requirements:ONBOARD ACQ FOR 15 ! Section 7.2
Comments:STEP-TIME=2.0 sec
Exposure_Number:15 ! Section 6.5
Target_Name:RHEA-ACQUISITION
Config:HRS
Opmode:ACQ/PEAKUP
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:EXTENDED=YES
Number_of_Iterations:1
Time_Per_Exposure:204S
Special_Requirements:ONBOARD ACQ FOR 16-19
Comments:step-time= 2.0 sec
Exposure_Number:16 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:IMAGE
Aperture:2.0
Sp_Element:MIRROR-N2
Wavelength:
Optional_Parameters:precision=high
Number_of_Iterations:1
Time_Per_Exposure:51.2S
Special_Requirements:SEQ 16-17 NON-INT
comments:STEP-TIME=0.2
Exposure_Number:17 ! Section 6.5
Target_Name:SATURN-LIMB
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:G160M
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD,STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR
Number_of_Iterations:1
Time_Per_Exposure:326.4S
Special_Requirements:
comments:
Exposure_Number:18 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 18-19 NON-INT
Comments:WAVE CALIBRATION FOR SKY-BACKGROUND 19.
Exposure_Number:19 ! Section 6.5
Target_Name:SKY-BACKGROUND
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD, STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 18.
Exposure_Number:20 ! Section 6.5
Target_Name:WAVE
Config:HRS
Opmode:ACCUM
Aperture:SC2
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:
Number_of_Iterations:1
Time_Per_Exposure:54.4S
Special_Requirements:SEQ 20-21 NON-INT
Comments:WAVE CALIBRATION FOR SKY-BACKGROUND 19.
Exposure_Number:21 ! Section 6.5
Target_Name:SKY-BACKGROUND
Config:HRS
Opmode:ACCUM
Aperture:2.0
Sp_Element:ECH-A
Wavelength:1216
Optional_Parameters:FP-SPLIT = STD, STEP-PATT= DEF,
DOPPLER=DEF,COMB=FOUR,SPYBAL=NO
Number_of_Iterations:1
Time_Per_Exposure:761.6S
Special_Requirements:
Comments:Please start on same position of
carrousel used for wave 18.
Data_Distribution ! Defaults indicated; change if desired
Medium: 8MM ! 8MM or 6250BPI or 1600BPI
Blocking_Factor: 10 ! 10 or 1
! Only astronomers with very old 9-
! track tape drives should consider
! a blocking factor of 1
Ship_To: PI_Address ! STSCI or PI_Address or <free-text>
! PI Address from Phase I is:
!
! 98bis Boulevard Arago
! Paris
! F-75014
!
!
Ship_Via: UPS ! UPS (2-day) or OVERNIGHT
! Overnight shipping done at PI expense
Recipient_Email: ! Needed if Ship_To: is not PI_Address
! <free-text>
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