! File: 4600C.PROP
! Database: PEPDB
! Date: 22-FEB-1994:19:14:17
coverpage:
title_1: FUV SPECTROSCOPY OF IO'S SO2 ATMOSPHERE AND SURFACE -- CYCLE 3 HIGH
sci_cat: SOLAR SYSTEM
proposal_for: GO
pi_title: DR.
pi_fname: JOHN
pi_mi: T.
pi_lname: CLARKE
pi_inst: UNIVERSITY OF MICHIGAN
pi_country: USA
pi_phone: 313-747-3540
keywords_1: PLANETARY SATELLITE, PLASMA TORUS
hours_pri: 7.75
num_pri: 1
fos: Y
time_crit: Y
funds_length: 12
funds_date: JUN-93
off_fname: NEIL
off_mi: D.
off_lname: GERL
off_title: PROJECT REP., DRDA
off_inst: UNIVERSITY OF MICHIGAN
off_addr_1: 475 E. JEFFERSON
off_city: ANN ARBOR
off_state: MI
off_zip: 48109
off_country: USA
! end of coverpage
abstract:
line_1: Cycle 1 HST observations of Io have provided new insights into the
line_2: nature of Io's surface albedo, the distribution of the SO2 atmosphere,
line_3: and the extent and excitation of the FUV airglow emissions. FOC images
line_4: show an anti-correlation between the brightness at 4000 A and 2800 A,
line_5: due to either surface SO2 frost or SO2 gas absorption above the frost
line_6: at the shorter wavelength. FOS spectra of the albedo spectrum at high
line_7: signal to noise clearly show SO2 gas absorption bands near 1900-2000 A
line_8: and evidence up to 1000 times spatial variation in the SO2 gas column
line_9: from the 2300 A spectrum. The FOS and GHRS airglow spectra have for the
line_10: first time resolved the extent of the FUV emission lines (1.7 Io radii
line_11: in diameter), and found that these lines decrease by a factor of 4-5
line_12: within 15 minutes of Io's passing into eclipse. This suggests that in
line_13: shadow either the SO2 atmosphere condenses onto the surface or the
line_14: ionosphere recombines rapidly: the difference between these two
line_15: possibilities is very significant. In cycle 3 we propose to scan across
line_16: Io with a small FOS aperture to obtain spatially resolved spectra of the
line_17: known bright and dark regions to discriminate between gas absorption and
line_18: surface albedo changes. We will also obtain FUV spectra of Io emerging
line_19: from eclipse to determine the time scale on which the FUV airglow
line_20: emission lines recover their intensity on return into sunlight.
!
! end of abstract
general_form_proposers:
lname: CLARKE
fname: JOHN
title: PI
mi: T.
inst: 2660
country: USA
!
lname: MCGRATH
fname: MELISSA
inst: 3470
country: USA
!
lname: AJELLO
fname: JOE
inst: 2370
country: USA
!
lname: SCHNEIDER
fname: NICK
inst: 1760
country: USA
!
lname: BALLESTER
fname: GILDA
inst: 2660
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 2
section: 1
line_1:
!
question: 3
section: 1
line_1: We propose to obtain spectra of specific regions on Io with
line_2: FOS G190H and G270H using the 0.25 arc sec aperture with offsets
line_3: from the acquired center of Io. These will be obtained near
line_4: times of Io western elongation, when the apparent
line_5: motion is small and corresponding to the existing FOC images at
line_6: 2800 A. We will center the aperture on known bright and dark
line_7: regions from the FOC images, and also perform a single spatial
line_8: scan N/S across the disk of Io to look for unexpected spectral
line_9: changes. We will also take a FOS G130H spectral time series of Io
line_10: emerging from eclipse behind Jupiter, with Io centered in the
line_11: 4.3 arc sec aperture: this will complete the series of eclipse
line_12: observations begun in cycles 1 and 2.
!
question: 4
section: 1
line_1: The line emissions excited by the impact of magnetospheric plasma
line_2: at Io are radiated chiefly in the FUV, and require a space-based
line_3: instrument with high sensitivity and angular resolution to be detected.
line_4: Ground-based instruments today have great difficulty in detecting
line_5: atmospheric line emissions from Io. Emissions from the extended
line_6: atmosphere of Io are just detectable with the IUE, but higher
line_7: sensitivity and angular resolution are required to determine the
line_8: source region and spatial distribution. Only the HST is fast enough
line_9: to detect changes in emission brightness through the eclipse events.
line_10: The capability of the FOS for measuring the 1600-3300 A albedo of Io
line_11: has been demonstrated in cycle 1 in 2 separate programs, whereas IUE
line_12: spectra are much too noisy below roughly 2400 A due to the decreasing
line_13: flux. Even with the HST spherical aberration, the central 0.15 arc sec
line_14: peak is sufficient to sample regions on the 1 arc sec Io disk with the
line_15: 0.25 arc sec aperture and compare the spectra of different regions of
line_16: known overall reflectivity from the FOC images. Only the angular
line_17: resolution and large aperture of HST can provide the high signal
line_18: spatially resolved spectra proposed here. After the insertion of
line_19: COSTAR the point spread function should be greatly improved, however
line_20: there will be a loss of sensitivity at the shorter wavelengths from
line_21: the added mirrors. We prefer to do what we can now in the UV, and
line_22: after COSTAR we may propose additional observations at longer
line_23: wavelengths.
!
question: 5
section: 1
line_1: The FOS G190H and G270H spectra are to be scheduled near
line_2: western elongation of Io. Io must be acquired and its center
line_3: determined to within roughly 0.10 arc sec: an offset will then be
line_4: made to position the FOS 0.25 arc sec aperture on the desired region(s)
line_5: of Io. The FOS G130H observation of Io must be centered (+/- 15 min.)
line_6: on the time of eclipse re-appearance, and must occur at the time of
line_7: year when the orbital longitude of Jupiter is 250 to 300 degrees.
line_8: These constraints can be relaxed somewhat if necessary to allow
line_9: scheduling.
!
question: 6
section: 1
line_1: None.
!
question: 7
section: 1
line_1: The UV spectra of Io will be reduced using standard routines as
line_2: in cycle 1: both JC and MM have reduced their cycle 1 data using IDL
line_3: on Sun workstations, and both have complete software packages for
line_4: the reduction and analysis of HST data. We have developed a
line_5: synthetic model program in IDL which predicts the albedo spectrum
line_6: of Io for assumed surface amounts of SO2 frost and a given column
line_7: of SO2 gas (see section 2). We are presently adapting the Ballester
line_8: et al (1990) IUE models for our cycle 1 HST FOS spectra which
line_9: accounts in more detail for spatial surface and atmospheric
line_10: structure. We are also in the process of a quantitative model of
line_11: the grating scatter in FOS for the 3 high dispersion gratings: we
line_12: expect these results to be concluded within the next 6 months. In
line_13: other words, we are ready to reduce, model, and interpret the new
line_14: albedo data. J. Ajello and collaborators are performing laboratory
line_15: studies of electron excitation of SO2 gas, measuring the electron
line_16: impact induced fluorescence spectrum of SO2 in the UV (400-2000 A)
line_17: at 2.5 A resolution. For the strongest features we have measured
line_18: excitation functions from 0-400 eV for modeling the excitation rates
line_19: at Io. This group also has a proposal in to measure the SO2 gas
line_20: photoabsorption cross sections over 1600-3300 A as a function of
line_21: pressure and temperature to address outstanding questions about line
line_22: saturation effects in the low density/low temperature lower
line_23: atmosphere of Io.
!
question: 8
section: 1
line_1: None.
!
question: 9
section: 1
line_1: 1. GO 2602 - "The Excitation of the Atmospheres of Planetary Satellites", J.
line_2: Clarke PI, J. Ajello and N. Schneider Co-I's - directly related.
line_3: 2. GO 2603 - "Parallel Observations of H Ly alpha Emission from the Local ISM",
line_4: J. Clarke PI - unrelated.
line_5: 3. GO 2393 - "D/H Ratio of Venus and Mars from Lyman alpha Emission", J. Clarke
line_6: Co-I - unrelated.
line_7: 4. GO 2625 - "Excitation Processes for the Outer Planet UV Emissions", M.
line_8: McGrath and J. Clarke Co-I's - unrelated.
line_9: 5. GO 2627 - "Io's Atmosphere and its Interaction with the Plasma Torus",
line_10: Co-I's: M. McGrath, G. Ballester - directly related.
line_11: 6. GO 3511 - "H Ly alpha Dayglow Emission Line Profiles from the Outer Planets",
line_12: J. Clarke PI - unrelated.
line_13: 7. GO 3616 - "Upper Atmospheres of Uranus and Neptune", M. McGrath PI, J. Clarke
line_14: Co-I - unrelated.
line_15: 8. GO 3617 - "The UV Emissions of Titan", M. McGrath PI, unrelated.
line_16: 9. GO 3618 - "Excitation Processes for the Outer Planet UV Emissions" - Cycle
line_17: 2 Continuation - M. McGrath PI - unrelated.
line_18: 10. GO 3862 - "The Excitation of the Atmospheres of Planetary Satellites", J.
line_19: Clarke PI, - J. Ajello and N. Schneider Co-I's - directly related.
!
question: 10
section: 1
line_1: Complete computing facilities are in place and available within
line_2: the Space Physics Research Lab. at the University of Michigan for use
line_3: on this project. Two Sparcstations, including a Sun IPX procured with
line_4: cycle 1 GO funding, and a VAX 8600 are available and connected via a
line_5: local area network, in addition to the Michigan network MERIT, SPAN,
line_6: and Internet. All Co-I's also have complete computing facilities at
line_7: their institutions for use on this project. In addition, the laboratory
line_8: work of J. Ajello and collaborators is proceeding with input from the
line_9: HST data and with independent funding.
!
!end of general form text
general_form_address:
lname: CLARKE
fname: JOHN
mi: T.
title: PROF.
category: PI
inst: UNIVERSITY OF MICHIGAN
addr_1: AOSS DEPT.
city: ANN ARBOR
state: MI
zip: 481092143
country: USA
!
! end of general_form_address records
! No fixed target records found
solar_system_targets:
targnum: 1
name_1: IO-ACQ-SPOTS
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
wind_1: OLG OF IO BETWEEN 215-235,
wind_2: OLG OF JUPITER BETWEEN 300 60
comment_1: IO ACQUISITION IN 4.3 ARC SEC
comment_2: APERTURE: TAKE A SET OF 11 SPECTRA
comment_3: AT DIFFERENT Y-DEFLECTIONS TO
comment_4: DETERMINE CENTERING IN X AND Y
comment_5: (FROM OBSERVED WAVELENGTH) THEN
comment_6: UPLINK HST POINTING CORRECTION.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
!
targnum: 2
name_1: IO-W-BRIGHT
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
lev3_1: TYPE = CARTO,
lev3_2: LONG = 222.0,
lev3_3: LAT = +5.0
wind_1: SEP OF EUROPA IO FROM EARTH GT 10",
wind_2: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_3: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_4: OLG OF IO BETWEEN 230 265,
wind_5: OLG OF JUPITER BETWEEN 300 60
comment_1: OBSERVE BRIGHT REGION ON IO WHEN
comment_2: IO IS FROM ABOUT -30 TO -5 DEGREES
comment_3: FROM WESTERN ELONGATION, WHEN JUPITER
comment_4: IS WITHIN 60 DEGREES OF OPPOSITION.
comment_5: PLEASE NOTE THAT THE WINDOWS CAN BE
comment_6: EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
fluxnum_4: 4
fluxval_4: SURF-CONT(1900) = 1.5 +/- 1 E-15
!
targnum: 3
name_1: IO-W-PELE
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
lev3_1: TYPE = CARTO,
lev3_2: LONG = 257.0,
lev3_3: LAT = -19.0
wind_1: SEP OF EUROPA IO FROM EARTH GT 10",
wind_2: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_3: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_4: OLG OF IO BETWEEN 240 280,
wind_5: OLG OF JUPITER BETWEEN 300 60
comment_1: OBSERVE PELE VOLCANO ON IO WHEN
comment_2: IO IS FROM ABOUT -30 TO +10 DEGREES
comment_3: FROM WESTERN ELONGATION, WHEN JUPITER
comment_4: IS WITHIN 60 DEGREES OF OPPOSITION.
comment_5: PLEASE NOTE THAT THE WINDOWS CAN BE
comment_6: EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
fluxnum_4: 4
fluxval_4: SURF-CONT(1900) = 1.5 +/- 1 E-15
!
targnum: 4
name_1: IO-W-DARK
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
lev3_1: TYPE = CARTO,
lev3_2: LONG = 288.0,
lev3_3: LAT = -15.0
wind_1: SEP OF EUROPA IO FROM EARTH GT 10",
wind_2: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_3: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_4: OLG OF IO BETWEEN 265 295,
wind_5: OLG OF JUPITER BETWEEN 300 60
comment_1: OBSERVE DARK REGION ON IO WHEN
comment_2: IO IS FROM ABOUT -5 TO +25 DEGREES
comment_3: FROM WESTERN ELONGATION, WHEN JUPITER
comment_4: IS WITHIN 60 DEGREES OF OPPOSITION.
comment_5: PLEASE NOTE THAT THE WINDOWS CAN BE
comment_6: EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
fluxnum_4: 4
fluxval_4: SURF-CONT(1900) = 1.5 +/- 1 E-15
!
targnum: 5
name_1: IO-W-LOKI
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
lev3_1: TYPE = CARTO,
lev3_2: LONG = 304.0,
lev3_3: LAT = +20.0
wind_1: SEP OF EUROPA IO FROM EARTH GT 10",
wind_2: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_3: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_4: OLG OF IO BETWEEN 280 325,
wind_5: OLG OF JUPITER BETWEEN 300 60
comment_1: OBSERVE LOKI VOLCANO ON IO WHEN
comment_2: IO IS FROM ABOUT +10 TO +55 DEGREES
comment_3: FROM WESTERN ELONGATION, WHEN JUPITER
comment_4: IS WITHIN 60 DEGREES OF OPPOSITION.
comment_5: PLEASE NOTE THAT THE WINDOWS CAN BE
comment_6: EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
fluxnum_4: 4
fluxval_4: SURF-CONT(1900) = 1.5 +/- 1 E-15
!
targnum: 6
name_1: IO-ACQ-SCAN
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
comment_1: IO ACQUISITION IN 4.3 ARC SEC
comment_2: APERTURE: TAKE A SET OF 5 SPECTRA
comment_3: AT DIFFERENT Y-DEFLECTIONS TO
comment_4: DETERMINE CENTERING IN X AND Y
comment_5: (FROM OBSERVED WAVELENGTH) THEN
comment_6: UPLINK HST POINTING CORRECTION.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
!
targnum: 7
name_1: IO-W-SCAN
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
wind_1: SEP OF EUROPA IO FROM EARTH GT 10",
wind_2: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_3: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_4: OLG OF IO BETWEEN 250 290,
wind_5: OLG OF JUPITER BETWEEN 300 60
comment_1: OBSERVE IO WITHIN +/- 20 DEGREES
comment_2: OF WESTERN ELONGATION WHEN JUPITER
comment_3: IS WITHIN 60 DEGREES OF OPPOSITION.
comment_4: PLEASE NOTE THAT THE WINDOWS CAN
comment_5: BE EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
fluxnum_4: 4
fluxval_4: SURF-CONT(1900) = 1.5 +/- 1 E-15
!
targnum: 8
name_1: IO-ACQ-SHADOW
descr_1: OFFSET EUROPA
lev1_1: STD = JUPITER
lev2_1: STD = EUROPA
comment_1: STRATEGY IS TO ACQUIRE EUROPA
comment_2: AND THEN BLIND OFFSET TO IO, BOTH
comment_3: IN 4.3 APERTURE. TO ACQUIRE EUROPA
comment_4: WITH FOS, TAKE A SET OF 5 SPECTRA
comment_5: AT DIFFERENT Y-DEFLECTIONS TO
comment_6: DETERMINE CENTERING IN X AND Y
comment_7: (FROM OBSERVED WAVELENGTH) THEN
comment_8: UPLINK HST POINTING CORRECTION.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.3 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 0.9 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
!
targnum: 9
name_1: IO-EGRESS
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
wind_1: OLG OF JUPITER BETWEEN 250 300,
wind_2: ECL U OF IO BY JUPITER,
wind_3: SEP OF EUROPA IO FROM EARTH GT 10",
wind_4: SEP OF GANYMEDE IO FROM EARTH GT 10",
wind_5: SEP OF CALLISTO IO FROM EARTH GT 10",
wind_6: SEP OF EUROPA IO FROM EARTH LT 2'
comment_1: OBSERVE IO COMING OUT OF ECLIPSE
comment_2: BEHIND JUPITER; BEGIN FOS EXPOSURE
comment_3: 15-20 MINUTES BEFORE IO ECLIPSE
comment_4: REAPPEARANCE AND SCHEDULE
comment_5: WHEN ORBITAL LONGITUDE OF JUPITER
comment_6: IS 250 TO 300 DEGREES.
comment_7: PLEASE NOTE THAT THE WINDOWS CAN
comment_8: BE EXPANDED IF NEEDED TO SCHEDULE.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
!
targnum: 10
name_1: IO-ACQ-IMAGE
descr_1: SATELLITE IO
lev1_1: STD = JUPITER
lev2_1: STD = IO
comment_1: ACQUISITION IMAGE OF IO IN 4.3
comment_2: FOS APERTURE FOR POST-UPLINK
comment_3: POINTING INFORMATION.
fluxnum_1: 1
fluxval_1: SURF(V) = 5.0 +/- 0.5
fluxnum_2: 2
fluxval_2: SIZE = 1.0 +/- .2
fluxnum_3: 3
fluxval_3: SURF-CONT(2700) = 2 +/- 1 E-13
!
! end of solar system targets
! No generic target records found
exposure_logsheet:
linenum: 1.000
targname: IO-ACQ-SPOTS
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 660 S
fluxnum_1: 3
priority: 1
param_1: Y-SIZE = 5,
param_2: Y-SPACE = 64,
param_3: COMB = YES,
param_4: SUB-STEP = 4
req_1: CYCLE 3 / 1-16;
req_2: SEQ 1-10 NOGAP;
req_3: INT ACQ FOR 2;
comment_1: SPECTRA OF IO FOR INTERACTIVE
comment_2: ACQUISITION: REQUIRES REAL-TIME
comment_3: UPLINK FOR S/C MOTIONS IN X AND
comment_4: Y DURING EARTH OCCULTATION.
!
linenum: 2.000
targname: IO-ACQ-SPOTS
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 4.0 S
fluxnum_1: 3
priority: 2
param_1: STEP-TIME=1.0,
param_2: SUB-STEP=1,
param_3: Y-SIZE=4,
param_4: Y-SPACE=64,
param_5: COMB=NO
comment_1: IMAGE OF 4.3 APERTURE
comment_2: FOR POST-UPLINK POINTING
comment_3: INFORMATION. NEXT,
comment_4: OFFSET TO 0.3 APERTURE
comment_5: FOR SPECTRA IN LINENUM 3.
!
linenum: 3.000
targname: IO-W-BRIGHT
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G270H
num_exp: 1
time_per_exp: 9 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF BRIGHT SPOT
comment_2: OF IO AT LONG,LAT = 222,+5.
!
linenum: 4.000
targname: IO-W-BRIGHT
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G190H
num_exp: 1
time_per_exp: 33 M
fluxnum_1: 4
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G190H SPECTRA OF BRIGHT SPOT
comment_2: OF IO AT LONG,LAT = 222,+5.
!
linenum: 5.000
targname: IO-W-PELE
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G270H
num_exp: 1
time_per_exp: 10 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF PELE VOLCANO
comment_2: OF IO AT LONG,LAT = 257,-19.
!
linenum: 6.000
targname: IO-W-PELE
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G190H
num_exp: 1
time_per_exp: 31 M
fluxnum_1: 4
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF PELE VOLCANO
comment_2: OF IO AT LONG,LAT = 257,-19.
!
linenum: 7.000
targname: IO-W-DARK
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G270H
num_exp: 1
time_per_exp: 10 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF DARK SPOT
comment_2: OF IO AT LONG,LAT = 288,-15.
!
linenum: 8.000
targname: IO-W-DARK
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G190H
num_exp: 1
time_per_exp: 38 M
fluxnum_1: 4
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF DARK SPOT
comment_2: OF IO AT LONG,LAT = 288,-15.
!
linenum: 9.000
targname: IO-W-LOKI
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G270H
num_exp: 1
time_per_exp: 10 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF LOKI VOLCANO
comment_2: OF IO AT LONG,LAT = 304,+20.
!
linenum: 10.000
targname: IO-W-LOKI
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G190H
num_exp: 1
time_per_exp: 31 M
fluxnum_1: 4
priority: 1
param_1: STEP-PATT=SINGLE
param_2: READ-TIME=60
comment_1: G270H SPECTRA OF LOKI VOLCANO
comment_2: OF IO AT LONG,LAT = 304,+20.
!
linenum: 11.000
targname: IO-ACQ-SCAN
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 300 S
fluxnum_1: 3
priority: 1
param_1: Y-SIZE = 5,
param_2: Y-SPACE = 128,
param_3: COMB = YES,
param_4: SUB-STEP = 4
req_1: SEQ 11-13 NOGAP;
req_2: INT ACQ FOR 12;
comment_1: SPECTRA OF IO FOR INTERACTIVE
comment_2: ACQUISITION: REQUIRES REAL-TIME
comment_3: UPLINK FOR S/C MOTIONS IN X AND
comment_4: Y DURING EARTH OCCULTATION.
comment_5: NEXT, OFFSET TO 0.3 APERTURE
comment_6: FOR SPECTRA IN LINENUM 12.
!
linenum: 12.000
targname: IO-W-SCAN
config: FOS/BL
opmode: RAPID
aperture: 0.3
sp_element: G270H
num_exp: 1
time_per_exp: 24 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=SINGLE
param_2: COMB = YES,
param_3: READ-TIME=60.0
req_1: SPATIAL SCAN ;
req_2: REQ UPLINK;
comment_1: VERY SLOW SPATIAL SCAN
comment_2: N/S ACROSS DISK OF IO.
comment_3: REQUIRES REVIEW BY STSCI.
!
linenum: 13.000
targname: IO-ACQ-IMAGE
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 4.0 S
fluxnum_1: 3
priority: 2
param_1: STEP-TIME=1.0,
param_2: SUB-STEP=1,
param_3: Y-SIZE=4,
param_4: Y-SPACE=64,
param_5: COMB=NO
comment_1: IMAGE OF 4.3 APERTURE
comment_2: FOR POST-UPLINK POINTING
comment_3: INFORMATION.
!
linenum: 14.000
targname: IO-ACQ-SHADOW
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 300 S
fluxnum_1: 3
priority: 1
param_1: Y-SIZE = 5,
param_2: Y-SPACE = 128,
param_3: COMB = YES,
param_4: SUB-STEP = 4
req_1: SEQ 14-16 NOGAP;
req_2: INT ACQ FOR 15;
comment_1: SPECTRA OF EUROPA FOR INT. ACQ.
comment_2: REQUIRES REAL-TIME UPLINK FOR
comment_3: S/C MOTIONS IN X AND Y DURING
comment_4: EARTH OCCULTATION. AFTER
comment_5: CENTERING ON EUROPA, OFFSET TO
comment_6: IO, WHICH IS IN SHADOW.
!
linenum: 15.000
targname: IO-EGRESS
config: FOS/BL
opmode: RAPID
aperture: 4.3
sp_element: G130H
num_exp: 1
time_per_exp: 25 M
fluxnum_1: 3
priority: 1
param_1: STEP-PATT=DEF,
param_2: READ-TIME=60.
req_1: DARK TIME;
req_2: REQ UPLINK;
comment_1: G130H SPECTRA OF IO: BEGIN
comment_2: 15-20 MINUTES BEFORE IO
comment_3: REAPPEARS IN SUNLIGHT FROM
comment_4: ECLIPSE. SCHEDULE IN DARK TIME
comment_5: DUE TO 1304 OXYGEN AIRGLOW.
!
linenum: 16.000
targname: IO-ACQ-IMAGE
config: FOS/BL
opmode: IMAGE
aperture: 4.3
sp_element: G270H
num_exp: 1
time_per_exp: 4.0 S
fluxnum_1: 3
priority: 2
param_1: STEP-TIME=1.0,
param_2: SUB-STEP=1,
param_3: Y-SIZE=4,
param_4: Y-SPACE=64,
param_5: COMB=NO
comment_1: IMAGE OF 4.3 APERTURE
comment_2: FOR POST-UPLINK POINTING
comment_3: INFORMATION, PERFORMED
comment_4: WHEN IO IS IN SUNLIGHT.
!
! end of exposure logsheet
scan_data:
line_list: 12.00
fgs_scan:
cont_dwell: C
dwell_pnts: 0
dwell_secs: 0.00
scan_width: 0.0000
scan_length: 1.2600
sides_angle: 90.0000
number_lines: 1
scan_rate: 0.0009
first_line_pa: 25.0000
scan_frame: CEL
len_offset: 0.6300
wid_offset: 0.0000
!
! end of scan data