! $Id: 5217,v 48.1 1994/07/27 15:58:36 pepsa Exp $ coverpage: title_1: JUPITER'S AURORA AND AIRGLOW sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GTO/WF2 pi_title: DR. pi_fname: JOHN pi_lname: TRAUGER pi_inst: 2370 pi_country: USA pi_phone: 818-354-9594 keywords_1: JUPITER hours_pri: 4.75 num_pri: 2 wf_pc: Y time_crit: Y pi_position: PROJECT SCIENTIST off_fname: JOHN off_mi: T. off_lname: TRAUGER off_title: DR. off_inst: JET PROPULSION LABORATORY off_addr_1: 4800 OAK GROVE DRIVE off_addr_2: MAIL STOP 179-225 off_city: PASADENA off_state: CA off_zip: 91109 off_country: USA off_phone: 818-354-9594 ! end of coverpage abstract: line_1: This cycle 4 proposal is for far-UV imaging of Jupiter's north line_2: auroral emissions in the H Ly alpha (1216 A) and H2 Lyman and line_3: Werner bands (900-1650 A). We estimate that WFPC2 with line_4: the Na metal filter will have 4-5 times higher efficiency line_5: and a much larger dynamic range than the present FOC images of line_6: Jupiter's aurora. Auroral images with a limiting sensitivity line_7: a few kR are important to reveal the full structure of the line_8: FUV auroral emission region. The longitudinal and short-term line_10: temporal dependences of the brightest sector of the north aurora line_11: will also be observed. These observations will be performed as line_12: the Galileo spacecraft approaches Jupiter, with a record of the line_13: solar wind properties near Jupiter for comparison with the WFPC2 line_14: observed auroral brightness and L-shell footprint for identification line_15: of the excitation processes. These observations constitute the line_16: first phase on this WFPC2 GTO program on Jupiter's upper atmosphere. ! ! end of abstract general_form_proposers: lname: TRAUGER fname: JOHN title: DR. mi: T. inst: 2370 country: USA esa: N ! lname: CLARKE fname: JOHN title: PROF. mi: T. inst: 2660 country: USA esa: N ! lname: BURROWS fname: CHRIS inst: STSCI country: USA ! lname: CRISP fname: DAVID inst: JPL country: USA ! lname: HOESSEL fname: JOHN inst: UNIV. OF WISCONSIN country: USA ! lname: GALLAGHER fname: JAY inst: UNIV. OF WISCONSIN country: USA ! lname: GRIFFITHS fname: RICHARD inst: JOHNS HOPKINS UNIV country: USA ! lname: HESTER fname: JEFF inst: ARIZONA STATE UNIV. country: USA ! lname: HOLTZMAN fname: JOHN inst: LOWELL OBSERVATORY country: USA ! lname: MOULD fname: JEREMY inst: CALTECH country: USA ! lname: WESTPHAL fname: JAMES inst: CALTECH country: USA ! ! end of general_form_proposers block general_form_text: ! question: 3 section: 1 line_1: One series of WF images covering 3 HST orbits (1/3 Jovian rotation) line_2: optimized for the brightest sector of the north aurora (near CML line_3: 180 deg) will be taken first, alternating the filter combinations: line_4: F160BW (detecting both H2 and H Ly a emissions), F160BW+F130LP (to line_5: separate the H Ly a component), and F160BW+F165LP (to separate the line_6: long-wavelength scattered light from Jupiter). Two short, red line_7: images with F673N using the same guide stars will register the limb line_8: position. To detect bright emissions, ~7-14 min exposures will be line_9: adequate. Exposures longer than 10 mins will be blurred E/W by line_10: Jupiter's rotation (~10 hr period), and the aurora may be varying line_11: on time scales as short as tens of seconds (by analogy to Earth). line_12: The above set of exposures will resolve the longitudinal and short line_13: term temporal dependences of the brightest emissions, dependent on line_14: the excitation processes. A second set of two long exposures with line_15: F160BW and F160BW+F130LP, followed by two shorter exposures with line_16: F160BW+F165LP and F673N, will be made of the north aurora active line_17: sector to resolve the full structure of the H and H2 emissions. line_18: These images may also show the equatorial airglow and Ly a 'bulge', line_19: and also limb brightening from optically thin H2 band emissions and line_20: from dayglow Ly a emission (due to scattering in the wings of the line_21: solar line by the increased slant column at the limb). The F160BW line_22: images will show the extent of the polar hood absorption and any line_23: structure possibly related to enhanced auroral photochemistry. ! question: 4 section: 1 line_1: The far-UV emissions of Jupiter's aurora and airglow can only be line_2: recorded from a space-based platform due to atmospheric absorption. line_3: The UV emissions are important because they are directly excited by line_4: the precipitating energetic particles. While IR emissions imaged line_5: from the ground are important tracers of the ionospheric line_6: temperature (H3+) and thermal/abundance effects in the neutral line_7: atmosphere (CnHm), these may not reflect the direct excitation of line_8: the atmosphere. In addition, only the HST is capable of providing line_9: 0.1 arc sec resolution to image the UV emissions with high spatial line_10: resolution. line_11: The exposure strategy is outlined above. The UV images are timed line_12: for maximum sensitivity with a minimal amount of blurring E/W due line_13: to Jupiter's rotation. The longer exposures are timed for maximum line_14: sensitivity with a longitude-averaged view of the limb emissions. line_15: The F673N images are to register the position of the limb. line_16: The auroral emission image sequence is repeated due to the known line_17: auroral emission image sequence is repeated due to the known line_18: variability in Jupiter's aurora: each sequence is to determine the line_19: emission variability with Jovian rotation. In cycle 5, two line_20: sequences will determine longer-term variations. ! question: 5 section: 1 line_1: The size of Jupiter is reduced significantly away from opposition, line_2: by about 4" within two months, and 8" within 3 months: The +/- 2 line_3: month window away from opposition is therefore desireable. line_4: These observations may be scheduled close in time (i.e. within a line_5: couple of orbits) with images of the Io torus emission (separate line_6: GTO proposal). line_7: We will try to arrange ground-based imaging of the H3+ and line_8: CnHm thermal emissions from Jupiter simultaneously (i.e. over the line_9: same Jovian rotation) with the WFPC2 images of the aurora. line_10: This will be important to determine the relation between the line_11: different emission processes, and we are particularly interested line_12: in establishing the relation between the spatial distribution of line_13: the directly-excited UV emissions and of the ionospheric H3+ line_14: emissions. We would also like to have simultaneous IUE observations line_15: in a sequence of spectra similar to the 14 year data base that line_16: exists from IUE. One of the important questions today is to line_17: understand how the FOC bright spots relate to the 180 deg. line_18: brightening at Jupiter's north pole observed repeatedly with IUE. ! question: 6 section: 1 line_1: Scheduling during dark time is required. We are imaging FUV line_2: emissions from H (Lyman alpha) and H2 (Lyman and Werner bands), line_3: some very weak emissions, and therefore require minimum line_4: contamination from geocoronal Ly a emission, to obtain the best line_5: possible S/N. line_6: The exposures cannot be interrupted because of Jupiter's fast line_7: rotation (10 hours) and temporal variations, and the exposures line_9: series have been planned accordingly. ! ! question: 8 section: 1 line_1: NONE ! question: 9 section: 1 line_1: We estimate that WFPC2 with the Na metal filter will have line_2: 4-5 times higher efficiency and a much larger dynamic line_3: range than the present FOC images of Jupiter's aurora. ! question: 10 section: 1 line_1: Unix workstations are available with IDL and the WFPC2 system line_2: SPICA software packages. ! question: 13 section: 1 line_1: This proposal constitutes the first step in our program to image line_2: Jupiter's FUV emissions arising from phenomena in the upper line_3: atmosphere/ionosphere of this planet. There are many unknowns line_4: about the characteristics of this atmospheric region and about the line_5: processes related to the magnetospheric and solar input, resulting line_6: in particular morphologies for the auroral and airglow emissions line_7: (eg, discrete vs diffuse aurora, the H Ly a bulge). The first line_8: steps are to concentrate on the brightest emissions from the north line_9: pole aurora, to fully identify the magnetospheric excitation line_10: processes at the time of the observations by accurately line_11: defining its variable structure down to its weaker emissions. line_12: Images for the weaker emissions may also show the equatorial line_13: airglow, the extent of the Ly a 'bulge'. We may also detect limb line_14: brightening from the optically thin H2 band emissions, and also line_15: from the dayglow Ly a emission due to scattering in the wings of line_16: the solar line by the increased slant column at the limb. From line_17: the cycle 4 data, a follow-up strategy will be identified for our line_18: future GTO observations, that will extend to the south aurora, of line_19: different characteristics than the north aurora, and of the poorly line_20: understood dayglow processes. ! !end of general form text general_form_address: lname: TRAUGER fname: JOHN mi: T. title: DR. category: PI inst: 2370 addr_1: MS 179-225 addr_2: 4800 Oak Grove Drive city: Pasadena state: CA zip: 91109 country: USA phone: 818-354-9594 ! lname: CLARKE fname: JOHN mi: T. title: DR. inst: 2660 phone: 313-747-3540 ! lname: BALLESTER fname: GILDA mi: E. title: DR. inst: 2660 phone: 313-747-3670 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: JUPITER-N-160 descr_1: PLANET JUPITER lev1_1: STD = JUPITER wind_1: CML OF JUPITER FROM EARTH BETWEEN wind_2: 60 25, wind_3: OLG OF JUPITER BETWEEN 300 60, wind_4: SEP OF IO JUPITER FROM EARTH GT 30", wind_5: SEP OF EUROPA JUPITER FROM EARTH wind_6: GT 30", SEP OF GANYMEDE JUPITER FROM wind_7: EARTH GT 30", SEP OF CALLISTO JUPITER wind_8: FROM EARTH GT 30" comment_1: JUPITER NORTH AURORA SERIES OF comment_2: EXPOSURES WITH WFC WITH 4 FILTER comment_3: COMBINATIONS TO BE MADE IN SEQUENTIAL comment_4: ORBITS CENTERED AT TIME WHEN SYSTEM III comment_5: CML IS 180 +/- 30 DEGREES. comment_6: WINDOWS CAN BE EXPANDED SOMEWHAT IF comment_7: NEEDED FOR SCHEDULING. comment_8: SCHEDULE DURING DARK TIME. fluxnum_1: 1 fluxval_1: V = -2.5 +/- 0.5 fluxnum_2: 2 fluxval_2: F-LINE(1400)=3+/-10E-14,W-LINE(1400)=420 fluxnum_3: 3 fluxval_3: F-CONT(1800) = 5 +/- 5 E-14 fluxnum_4: 4 fluxval_4: SIZE = 3.5 +/- 3.0 fluxnum_5: 5 fluxval_5: F-CONT(5500) = 2.8 +/- 1 E-11 fluxnum_6: 6 fluxval_6: SIZE = 1.1 ! targnum: 2 name_1: JUPITER-N-AUR1 descr_1: PLANET JUPITER lev1_1: STD = JUPITER wind_1: CML OF JUPITER FROM EARTH BETWEEN wind_2: 80 350, wind_3: OLG OF JUPITER BETWEEN 300 60, wind_4: SEP OF IO JUPITER FROM EARTH GT 30", wind_5: SEP OF EUROPA JUPITER FROM EARTH wind_6: GT 30", SEP OF GANYMEDE JUPITER FROM wind_7: EARTH GT 30", SEP OF CALLISTO JUPITER wind_8: FROM EARTH GT 30" comment_1: LONG WFC EXPOSURE OF JUPITER'S NORTH comment_2: AURORA IN ITS WEAKEST H2 EMISSIONS, comment_3: PLUS A VISIBLE AND A BACKGROUND FUV comment_4: EXPOSURE, TO BE MADE IN SEQUENTIAL comment_5: ORBITS CENTERED AT TIME WHEN SYSTEM comment_6: III CML IS 180 +/- 30 DEGREES. comment_7: WINDOWS CAN BE EXPANDED SOMEWHAT IF comment_8: NEEDED FOR SCHEDULING. comment_9: SCHEDULE DURING DARK TIME. fluxnum_1: 1 fluxval_1: V = -2.5 +/- 0.5 fluxnum_2: 2 fluxval_2: F-LINE(1400)=3+/-10E-14,W-LINE(1400)=420 fluxnum_3: 3 fluxval_3: F-CONT(1800) = 5 +/- 5 E-14 fluxnum_4: 4 fluxval_4: SIZE = 3.5 +/- 3.0 fluxnum_5: 5 fluxval_5: F-CONT(5500) = 2.8 +/- 1 E-11 fluxnum_6: 6 fluxval_6: SIZE = 1.1 ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.01 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F673N num_exp: 1 time_per_exp: 1.0 S s_to_n: 120 fluxnum_1: 5 fluxnum_2: 6 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; req_2: SEQ 1.01 - 1.02 NO GAP; ! req_3: DARK TIME / 1.03 - 1.08; ! req_4: PCS MODE F; req_5: GUID TOL 0.2"/1.01-1.10, 2.1-2.5; req_6: POS TARG -13.3,+10.7 comment_1: RED IMAGE OF JUPITER WITH SAME GUIDE comment_2: STARS AS IN LINENUM 1.02-1.10 TO comment_3: IDENTIFY LIMB OF PLANET. ! linenum: 1.02 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F165LP num_exp: 1 time_per_exp: 500.0 S s_to_n: 8 fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO param_3: CR-TOLERANCE=0.1 req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: IMAGE OF JUPITER'S BACKGROUND UV comment_2: SCATTERED LIGHT TO SUBTRACT FROM FUV comment_3: IMAGES OF AURORA. TWO CONSECUTIVE comment_4: IMAGES FOR CR-SPLIT AND SUMMATION. ! linenum: 1.03 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F130LP num_exp: 1 time_per_exp: 500.0 S s_to_n: 7 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; req_2: SEQ 1.03-1.10 NO GAP; req_3: AFTER 1.01 BY 90M +/- 10M; req_4: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORA comment_2: SEPARATING THE H LY A FROM THE H2 comment_3: EMISSIONS. comment_4: TAKE IMAGE DURING SAME DARK HST ORBIT comment_5: AS LINENUM = 1.04. ! linenum: 1.04 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW num_exp: 2 time_per_exp: 600.0 S s_to_n: 10 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORAL H comment_2: AND H2 EMISSIONS. TAKE IMAGES 1.03 AND comment_3: 1.04 DURING SAME DARK HST ORBIT TO comment_4: AVOID BLURRING FROM PLANET ROTATION. comment_5: ORBIT SHOULD IMMEDIATELY FOLLOW comment_6: LINENUM = 1.01 & 1.02 ! linenum: 1.05 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F130LP num_exp: 1 time_per_exp: 500.0 S s_to_n: 7 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORA comment_2: SEPARATING THE H LY A FROM THE H2 comment_3: EMISSIONS. comment_4: TAKE IMAGE DURING SAME DARK HST ORBIT comment_5: AS LINENUM = 1.06. ! linenum: 1.06 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW num_exp: 2 time_per_exp: 600.0 S s_to_n: 10 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORAL H comment_2: AND H2 EMISSIONS. TAKE IMAGES 1.05 AND comment_3: 1.06 DURING SAME DARK HST ORBIT TO comment_4: AVOID BLURRING FROM PLANET ROTATION. comment_5: ORBIT SHOULD IMMEDIATELY FOLLOW comment_6: LINENUM = 1.03 & 1.04 ! linenum: 1.07 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F130LP num_exp: 1 time_per_exp: 500.0 S s_to_n: 7 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORA comment_2: SEPARATING THE H LY A FROM THE H2 comment_3: EMISSIONS. comment_4: TAKE IMAGE DURING SAME DARK HST ORBIT comment_5: AS LINENUM = 1.08. ! linenum: 1.08 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW num_exp: 2 time_per_exp: 600.0 S s_to_n: 10 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT= NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: FUV IMAGE OF JUPITER'S NORTH AURORAL comment_2: H AND H2 EMISSIONS. TAKE IMAGES 1.07 comment_3: AND 1.08 DURING SAME DARK HST ORBIT comment_4: TO AVOID BLURRING FROM JUPITER'S comment_5: ROTATION. ! linenum: 1.09 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F165LP num_exp: 1 time_per_exp: 500.0 S s_to_n: 8 fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: IMAGE OF JUPITER'S BACKGROUND UV comment_2: SCATTERED LIGHT TO SUBTRACT FROM comment_3: PREVIOUS FUV IMAGES OF AURORA. ! linenum: 1.10 targname: JUPITER-N-160 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F673N num_exp: 1 time_per_exp: 1.0 S s_to_n: 120 fluxnum_1: 5 fluxnum_2: 6 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: RED IMAGE OF JUPITER WITH SAME GUIDE comment_2: STARS AS IN LINENUM 1.02-1.09 TO comment_3: IDENTIFY LIMB OF PLANET. ! linenum: 2.100 targname: JUPITER-N-AUR1 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F673N num_exp: 1 time_per_exp: 0.23 S s_to_n: 120 fluxnum_1: 5 fluxnum_2: 6 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO param_3: SUM = 2X2 req_1: CYCLE 4; req_2: SEQ 2.1 - 2.5 NO GAP; ! req_3: DARK TIME / 2.3 - 2.4; ! req_4: PCS MODE F; req_5: GUID TOL 0.2"/2.1-2.5; req_6: POS TARG -13.3, +10.7 comment_1: RED IMAGE OF JUPITER WITH SAME GUIDE comment_2: STARS AS IN LINENUM 2.2-2.5 TO comment_3: IDENTIFY LIMB OF PLANET. ! linenum: 2.200 targname: JUPITER-N-AUR1 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F165LP num_exp: 2 time_per_exp: 350.0 S s_to_n: 15 fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO param_3: CR-TOLERANCE=0.1 param_4: SUM = 2X2 req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: IMAGE OF JUPITER'S BACKGROUND UV comment_2: SCATTERED LIGHT TO SUBTRACT FROM FUV comment_3: IMAGES OF AURORA. TWO CONSECUTIVE comment_4: IMAGES FOR CR-SPLIT AND SUMMATION. ! linenum: 2.300 targname: JUPITER-N-AUR1 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW num_exp: 1 time_per_exp: 1500.0 S s_to_n: 10 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT= NO param_3: CR-TOLERANCE=0.1 param_4: SUM = 2X2 req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: LONG FUV IMAGES OF JUPITER'S NORTH comment_2: AURORA SEPARATING THE H LY A FROM THE comment_3: H2 EMISSIONS. comment_4: TAKE IMAGE DURING HST ORBIT comment_5: FOLLOWING ORBIT OF LINENUM = 2.2. ! linenum: 2.400 targname: JUPITER-N-AUR1 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F160BW, F130LP num_exp: 1 time_per_exp: 1500.0 S s_to_n: 10 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO param_3: CR-TOLERANCE=0.1 param_4: SUM = 2X2 req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -13.3, +10.7 comment_1: LONG FUV IMAGES OF JUPITER'S NORTH comment_2: AURORA SEPARATING THE H LY A FROM THE comment_3: H2 EMISSIONS. comment_4: TAKE IMAGES DURING HST ORBIT comment_5: FOLLOWING ORBIT OF LINENUM = 2.3. ! linenum: 2.500 targname: JUPITER-N-AUR1 config: WFPC2 opmode: IMAGE aperture: WF4-FIX sp_element: F673N num_exp: 1 time_per_exp: 0.23 S s_to_n: 120 fluxnum_1: 5 fluxnum_2: 6 priority: 1 param_1: ATD-GAIN = 7 param_2: CR-SPLIT=NO param_3: SUM = 2X2 req_1: CYCLE 4; ! req_2: PCS MODE F; req_3: POS TARG -14.7, +17.1 comment_1: RED IMAGE OF JUPITER WITH SAME GUIDE comment_2: STARS AS IN LINENUM 2.2-2.4 TO comment_3: IDENTIFY LIMB OF PLANET. ! ! end of exposure logsheet ! No scan data records found