! 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