Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5348 Report Date: 18-Jul-95:17:12 Version: ********** Check-in Date: ********** 1.Proposal Title: SPECTROSCOPIC OBSERVATIONS OF JUPITER'S AURORA: CYCLE4 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID SOLAR SYSTEM GO Sub Category GIANT PLANETS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Laurence M Trafton 3550 US 5124711476 ------------------------------------------------------------------------------------ 7. Abstract We propose to compare FUV spectra of bright, quasi-permanent regions of Jupiter's northern aurora using the GHRS with G160M+LSA to search directly for heavy ions in the precipitating particle flux and to determine the effects of strongly precipitating flux on the atmospheric structure. Specifically, we will search for selected emission lines from oxygen and sulfur in various ionization states. The primary objectives of this study are twofold: 1) to investigate the relative roles of ions and electrons as the primary precipitating particles in the Jovian aurora and their energy/flux distribution. This is a prerequisite for understanding the mechanisms which generate these auroral emissions. 2) to examine the effect of intense particle precipitation on the Jovian upper atmosphere. Of particular interest is the extent to which the auroral homopause is elevated as a result of the local enhancement of the eddy diffusion coefficient. This will be determined from the H2 "color ratio" and the ro-vib H2 temperature, which, with modeling, characterizes the hydrocarbon content of the atmospheric layers contributing most to the observed H2 emissions, the pressure level of penetration, and the energy of the precipitating particles. The spectra will complement FOC images previously obtained and permit a symbiotic analysis of both spectra and images. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 3.26 par: 0 10. Num targs pri: 2 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS ------------------------------------------------------------------------------------ 12. Special sched req: Time Critical obs. ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5348 PI: Laurence M Trafton Proposal Title: SPECTROSCOPIC OBSERVATIONS OF JUPITER'S AURORA: CYCLE4 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Laurence Trafton 3550 USA J. Hunter Waite 3440 USA Jean-Claude Gerard 4330 Belgium X Laurence M. Trafton Page 3 ------------------------------------------------------------------------------------ 3. Description of proposed observations. a. The spectra will be acquired with the GHRS using an onboard Galilean- satellite assisted acquisition followed by an offset to the northern aurora near the morning limb. This will be done for each of three phased Jupiter rotations ~ repeating the longitude segments covered during two consecutive visibility periods of the first Jupiter rotation. The timing will be such as to put the central meridian longitude (CML) near 143 deg at the start of the first exposure near the beginning of the first visiblilty period each visit in order that the 31 min exposure fit within the visibility period. All exposures are ~31 min long and should fit within a single visibility period in order to sample the proper longitude ranges. All spectra will be taken with G160M in the ACCUM mode with the LSA (2" x 2") yielding a resolution ~0.61 A or better depending on the extent to which the auroral emission fills the aperture. Jupiter's rotation will not be tracked; spectra will be obtained as bright portions of the aurora pass continuously across the LSA. The primary purpose of targeting bright emission regions is to maximize the number of photons detected in order to facilitate the detection of heavy ions and to study a region of the atmosphere strongly disturbed by auroral precipitation; tracking of hot spots is not required. The first HST orbit will acquire a 31min spectrum of the H2 Werner band emission from 1252-1288A approximately covering the CML range 143-165 deg, and search for SII emission at 1256A. The 2nd orbit will repeat this for the afternoon northern aurora over CML 185-230deg. The pointing will remain fixed as Jupiter rotates. For each visit, the target is the morning aurora during the first orbit and the afternoon aurora during the second orbit. The two orbits in each visit should be back-to-back (NO GAP) to cover the desired auroral region using the same guide stars. The two orbits span the northern "active sector" near 180 deg where FOC images of the FUV emission (Dols et al., 1992; Gerard et al., 1992; and Waite, 1992) show enhanced emission near the auroral limb. The above procedure is repeated for a second Jupiter rotation, including a new onboard, satellite- assisted acquisition 10 hrs (one Jupiter rotation) after the start of the first sequence but at different wavelengths in order to measure the H2 "color ratio" and explore for additional heavy ion emission lines. These observations should immediately follow those of the first rotation of Jupiter to minimize the extent of any temporal changes in the aurora. After one orbit for the onboard acquisition, the exposure will start near CML 159 deg instead of 143 deg, a phase slip of about 16 deg, which is OK. The first orbit of this second Jupiter rotation will cover the "Lyman band" seqment from 1575-1605A, spanning roughly the same longitudes as scanned by the Werner band spectrum during the first Jupiter rotation. For the second orbit, a heavy ion wavelength, OIII at 1664A, will be observed. This observing sequence will be repeated for a third Jupiter rotation and visit, except that only heavy ions will be observed. This visit need not immediately follow the second rotation. The CML ranges must approximate those of the first visit's two rot- ions in order to observe the same bright auroral regions. Some error in Jupiter's phase is allowed to account for the incommensurate HST orbit and Jupiter period; the idea is to repeat for each Jupiter rotation the desired longitude segments. The same guide stars should be used throughout a given visit, including the satellite-assisted acquisition. Page 4 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. a. Only HST can observe Jupiter's FUV auroral features with the spatial resolution and sensitivity required for this study. Previous HST spectra of the northern aurora have missed the brighter emissions owing to blind pointing; and observations planned in Cycle 3 do not have the same constraint on the CML window as proposed here, nor do they measure the H2 "color ratio". In any event, "near- simultaneous" spectra are required for our comparative study. Extensive IUE observations of the Jovian aurora have been done but they were taken through a large aperture which provided little spatial resolution of auroral phenomena. Projection effects highly weight the longitudinal variations observed. Moreover, IUE's relatively low sensitivity has sharply limited the achievable S/N. b. Justify the amount of exposure time Our proposed program makes very efficient use of spacecraft time by combining the search for heavy ions in the primary precipitating magnetospheric flux with the comparative study of the northern and southern H2 aurorae. Since the "active sectors" of the two aurorae differ by ~150 deg, it is possible to interleave observations from opposite hemispheres, filling the gaps with heavy ion observations. Because the same guide stars can be used over a Jupiter rotation (10 hrs), the two target regions can be observed with only one satellite-assisted acquisition for each of the three Jupiter rotations needed to cover our program. Observing the diurnally-enhanced morning emission means that Jupiter's rotation need not be tracked, so fewer constraints are placed on the scheduling. We assume spectral exposures of 31 min per visibility period (this may be adjusted, if needed), and two consecutive visibility periods per Jupiter rotation. At a given wavelength, the H2 exposures will total to 31 min. The heavy ion exposures will sum to 155 min. The spectra will be taken at the locations of quasi- stationary emission discovered from the FOC images (Gerard et al., 1992; Waite, 1992). These emission zones have intensities for the H2 band in excess of 200 kR . With COSTAR installed, a 200 kR band intensity would give an average S/N =7 per diode with the GHRS+G160M +LSA over a 31 min exposure (This would correspond to an average count rate of 0.03 Hz/diode). For the Lyman H2 bands, the peak flux seen by IUE was 0.03 ph cm-2 s-1 -1. If this were spread out over the upper part of IUE's large aperture (about 6"x2"), a 31 min exposure with GHRS+G160M+LSA would give S/N ratios of 10 per diode, or 21 binned over 4 diodes. The Werner bands have about one third this strength. Summing the observations or binning the spectra would improve the S/N ratio. Concerning the detection of S and O ions, a 1hr exposure in this configuration would detect a 75 R line with S/N =8.4. This corresponds to S/N= 8.1 for a 64 min exposure; or 6.1 for a 31 min exposure. Use of the medium resolution grating, as opposed to the low resolution of the FOS, allows better wavelength resolution from neighboring H2 emission lines for the wavelength groups overlapping the H2 emission, thus improving the chances of detection. Page 5 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. The aurorae in a given hemisphere are bright only during certain phases of Jupiter's rotation, different for each hemisphere. Efficient coverage of the north auroral zone requires beginning the observation sequence at a particular Jovian rotational phase (cf. GF question 3). This phase must be preserved for subsequent visits, which look at the same longitude ranges but at different wavelengths. This is so that the flux at different wave- lengths refer to the same auroral region and so may be compared and conclusions drawn. The first two orbits of each visit need to be consecutive in order that the proper auroral longitudes be spanned and to make efficient use of the visit. The first two rotations of Jupiter (i.e., the first two visits) should be observed consecutively to avoid the buildup of systematic effects arising from the time variability of Jupiter's aurorae. The Guide Stars must remain unchanged throughout a given visit, including the OA, to assure pointing accuracy. Any suitable Galilean satellite may be used for the OA, not just Io as assumed in the Exposure Log. The GS's should not be changed in offsetting to the Jovian aurorae. Dark Time is requested for Line 12 for the OI 1304 A line to minimize blending with the geocoronal OI emission. If only partial Dark Time is available during the visibility period, then break the exposure up into the dark and light portions, respectively. If Dark Time cannot be scheduled, see the PI for an alternate heavy-ion emission-line wavelength. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. none. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. Initial data reduction will be accomplished by the PI Trafton at the STScI using the STSDAS with a more detailed followup at the University of Texas using the GHRS Team software, CALHRS. The data reduction will include blemish removal, background subtraction, flat fielding, wavelength scaling, and conversion to flux units, using updated calibration files. The oxygen and sulfur spectra will be examined individually, compared via ratioing, and coadded to build up the S/N ratio for detecting these ions in emission. The facilities of the Southwest Research Institute, the University of Texas at Austin, and the Institut d' Astrophysique, Universite de Liege, Belgium will be employed for modeling, analyzing, and interpreting the data. Our objectives are as follows: * Attempt to detect or set upper limits on emission from oxygen and sulfur ions. * Measure the "color ratio" between the Werner and Lyman bands of H2. * Measure the ro-vib temperature of H2 emission for a bright emission. * Deduce the relative importance of ions vs electrons as primary precipitating particles. * Determine the pressure level of penetration and the energy of the precipitating particles. * Constrain the flux and spectral index of the primary precipitating particles. * Determine the elevation of the homopause over the normal level. * Constrain the strength of turbulent mixing in the auroral zones. * Search for other emission species as clues to ionic chemistry in auroral zone. PI L. Trafton will be responsible for executing the observing program, reducing the observations, participating in the modeling and analysis, and managing the program. Co-I H. Waite will do the required modeling of the auroral processes in Jupiter's atmosphere. Co-I J. C. Gerard will focus mainly on the modeling of synthetic H2 spectra and fitting them to the observations. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. Co-I Gerard is the PI on an Cycle 3 FOC proposal to observe the northern auroral intensity distribution. The results from these observations will help to refine the longitude range of the proposed observations. Page 6 ------------------------------------------------------------------------------------ 9. Description of previous HST work. a. List the HST program numbers, titles, and present authors involved in each. Trafton: 1202 Lyman-alpha and H2 Survey; None for Jupiter. 1203 Jovian Auroral Ly-alpha Profile; No 1204: Io Proton Aurora? No 1205/3214: SO2 on Io; No 1206 Sulfur Near Io; No 1290: Uranus and Neptune below 3000 ; No 2569: UV Rotational Light Curves for Pluto, and Charon's UV Spectrum; No 2957 High Resolution UV Spectroscopy of Triton; No 2560: Integrated Dynamical and Spectroscopic Observations of Jupiter and Saturn; No 3803: Pluto's FUV Spectrum: CO Abundance and FUV Survey, No 4001 H2 Survey of Jupiter's Northern Aurora During Ulysses Flyby; Yes 4005: HST UV Imaging of Jupiter to Support the Interpretation of Ulysses X-ray Measurements; Yes b Spectra of Jupiter's northern aurora were taken during the flyby of the Ulysses spacecraft (P4001) and reveal a ro-vib temperature of 550 K near latitude +65 deg and longitude 180 deg. c. "First results from the GHRS: Resolved velocity and density structure in the beta pictoris circumstellar gas", A. Boggess, F. C. Bruhweiler, C. A. Grady, D. C. Ebbets, Y. Kondo, L. M. Trafton, J. C. Brandt, and S. R. Heap, Astrophys. J. (Letters), 377, L49, 1991. "Several Early Results from HST Planetary Observations" -L. Trafton, ESO Conference and Workshop Proceedings No. 44, pp 487 -492, "Far ultraviolet imaging of the Jovian aurora with the Hubble Space Telescope", V. Dols, J. C. Gerard, F. Paresce, R. Prange, and A. Vidal- Madjar, Geophys. Res. Lett. 19, 1803, 1992. "Morphology and time variation of the Jovian far ultraviolet imaged with the HST", J. C. Gerard, V. Dols, F. Paresce, and R. Prange, JGR Planets, submitted 1992. "Solar system observations with HST", in Proceedings of the International Space Year Conference, Munich, F. Paresce and J. C. Gerard, in press 1993. "Jupiter's northern auroral emission during the flyby of Ulysses on 8 Feb 1992", ApJ, in press 1994. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Facilities of the University of Texas Computation Center and Advanced Graphics Laboratory are available to support this project, as well as a Sun 2 Sparcstation and peripherals. A pool of astronomy graduate students is potentially available from which to draw research assistants. Ground based observations of Jovian aurora at 2 5m are periodically made from McDonald Observatory for related studies. The Southwest Research Institute will support this project by providing Co-I H. Waite with the computing facilities, time, and codes required for modeling the auroral processes in Jupiter's atmosphere. The University of Liege will support all of Co-I J. C. Gerard's activities under this proposal, which focus on the modeling of synthetic H2 spectra. ------------------------------------------------------------------------------------ 11. Address Information Name: Laurence Trafton Category: PI Institution: 3550 Address: ASTRONOMY DEPARTMENT UNIVERSITY OF TEXAS AT AUSTIN City: AUSTIN State: TX Zip Code: 78712 Country: USA Telephone: 512 471 1476 Telex (or e-mail): lmt@astro.as.utexas.edu ------------------------------------------------------------------------------------ TARGET LIST b)Solar System Targets ID = 5348 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ TARGET NUMBER: 1 | TARGET NAME: IO ------------------------------------------------------------------------------------------------------------------------------------ TARGET DESCRIPTION: SATELLITE IO ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 1 | TARGET POSITION LEVEL 2 | STD=JUPITER | STD = IO | ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 3 | WINDOWS | | SEP OF EUROPA IO FROM EARTH GT 12", | SEP OF GANYMEDE IO FROM EARTH GT 12", | SEP OF CALLISTO IO FROM EARTH GT 12", | WND1 = 10-MAR-94 TO 31-JUL-94 | ------------------------------------------------------------------------------------------------------------------------------------ REF | DATA | COMMENTS | | 1 |V = 5, TYPE = G2V | THIS TARGET IS USED FOR AN ONBOARD | | SATELLITE-ASSISTED ACQUISITON OF THE | | NORTHERN AURORAE. ANY OTHER GALILEAN | | SATELLITE MAY BE USED INSTEAD. | ------------------------------------------------------------------------------------------------------------------------------------ TARGET NUMBER: 2 | TARGET NAME: JUP-N1-AURORA ------------------------------------------------------------------------------------------------------------------------------------ TARGET DESCRIPTION: FEATURE JUPITER ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 1 | TARGET POSITION LEVEL 2 | STD = JUPITER | TYPE = TORUS, | LONG = +315, | LAT = +61.5, | RAD= 67800, | POLE_LAT=+90 | ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 3 | WINDOWS | | CML OF JUPITER FROM EARTH BETWEEN | 125 195, | WND1 = 10-APR-95 TO 31-AUG-95 | ------------------------------------------------------------------------------------------------------------------------------------ REF | DATA | COMMENTS | | 1 |V = -2.5 | OBSERVE MORNING NORTHERN AURORA. 2 |SURF(1600)=2.3E-15 | | ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST b)Solar System Targets ID = 5348 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ TARGET NUMBER: 3 | TARGET NAME: JUP-N2-AURORA ------------------------------------------------------------------------------------------------------------------------------------ TARGET DESCRIPTION: FEATURE JUPITER ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 1 | TARGET POSITION LEVEL 2 | STD = JUPITER | TYPE = TORUS, | LONG = +45, | LAT = +61.5, | RAD = 67800, | POLE_LAT=+90 | ------------------------------------------------------------------------------------------------------------------------------------ TARGET POSITION LEVEL 3 | WINDOWS | | CML OF JUPITER FROM EARTH BETWEEN | 175 245, | WND1 = 10-APR-95 TO 31-AUG-95 | ------------------------------------------------------------------------------------------------------------------------------------ REF | DATA | COMMENTS | | 1 |V = -2.5, TYPE = G2V | Observe afternoon N. aurora 2 |SURF(1600)=2.3E-15 | | ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5348 [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 IO HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 1 1 ONBOARD ACQ FOR LOCATE=EXTENDED 1.2,3,4,4.5 SEARCH-SIZE=3 CYCLE 4/1-12 SEQ 1-1.2 NON-INT SEQ 1-4.5 NO GAP GROUP 1-12 WITHIN Comments: This onboard satellite-assisted 2D acq will allow accurate acquisition of jupiter's auroral region. ANY GALILEAN SATELLITE MAY BE USED INSTEAD OF IO. USE LOCATE=EXTENDED ------------------------------------------------------------------------------------------------------------------------------------ 1.2 IO HRS IMAGE 2.0 MIRROR-N2 1 60S 1 2 Comments: TAKE MAP AFTER CENTERING ------------------------------------------------------------------------------------------------------------------------------------ 3 JUP-N1- HRS ACCUM 2.0 G160M 1252- 1 26M 2 1 GROUP 3,7 WITHIN AURORA 1288 11H Comments: DESIRE CML IN RANGE=135-175 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 3.5 JUP-N1- HRS ACCUM 2.0 G160M 1252- 1 8M 2 1 AURORA 1288 Comments: DESIRE CML IN RANGE=135-175 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 4 JUP-N2- HRS ACCUM 2.0 G160M 1252- 1 26M 2 1 AURORA 1288 Comments: DESIRE CML IN RANGE=185-230 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 4.5 JUP-N2- HRS ACCUM 2.0 G160M 1252- 1 8M 2 1 AURORA 1288 Comments: DESIRE CML IN RANGE=185-230 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 6 IO HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 1 1 ONBOARD ACQ FOR LOCATE=EXTENDED 6.2-8.5 SEARCH-SIZE=3 SEQ 6,6.2 NON-INT SEQ 6-9 NO GAP Comments: This onboard satellite-assisted acq will allow accurate acquisition of jupiter's auroral region. ANY GALILEAN SATELLITE MAY BE USED INSTEAD OF Io. USE LOCATE=EXTENDED ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5348 [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 6.2 IO HRS IMAGE 2.0 MIRROR-N2 1 60S 1 2 Comments: TAKE MAP AFTER CENTERING ------------------------------------------------------------------------------------------------------------------------------------ 7 JUP-N1- HRS ACCUM 2.0 G160M 1575- 1 26M 2 1 AURORA 1605 Comments: DESIRE CML IN RANGE=135-175 DEG PLUS 16 deg phase shift. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 7.25 JUP-N1- HRS ACCUM 2.0 G160M 1575- 1 8M 2 1 AURORA 1605 Comments: DESIRE CML IN RANGE=135-175 DEG PLUS 16 deg phase shift. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 8 JUP-N2- HRS ACCUM 2.0 G160M 1664 1 26M 2 1 AURORA Comments: DESIRE CML IN RANGE=185-230 DEG PLUS 16 deg phase shift. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 8.5 JUP-N2- HRS ACCUM 2.0 G160M 1664 1 8M 2 1 AURORA Comments: DESIRE CML IN RANGE=185-230 DEG PLUS 16 deg phase shift. OBSERVATION SHOULD FIT IN ONE ORBIT. ------------------------------------------------------------------------------------------------------------------------------------ 9 WAVE HRS ACCUM SC2 G160M 1664 1 60S 2 CALIB FOR 8.5 Comments: SCHEDULE DURING EARTH OCCULTATION OF JUPITER. ------------------------------------------------------------------------------------------------------------------------------------ 10 IO HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 1 1 ONBOARD ACQ FOR LOCATE=EXTENDED 10.2-12 SEARCH-SIZE=3 SEQ 10-10.2 NON- INT SEQ 10-11.6 NO GAP Comments: This onboard satellite-assisted acq will allow accurate acquisition of jupiter's auroral region. ANY GALILEAN SATELLITE MAY BE USED INSTEAD OF Io. USE LOCATE=EXTENDED ------------------------------------------------------------------------------------------------------------------------------------ 10.2 IO HRS IMAGE 2.0 MIRROR-N2 1 60S 1 2 Comments: TAKE MAP AFTER CENTERING ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5348 [ 11] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 11 JUP-N1- HRS ACCUM 2.0 G160M 1411 1 26M 2 1 AURORA Comments: DESIRE CML IN RANGE=135-175 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. This orbit need not be contiguous with previous one. ------------------------------------------------------------------------------------------------------------------------------------ 11.5 JUP-N1- HRS ACCUM 2.0 G160M 1411 1 8M 2 1 AURORA Comments: DESIRE CML IN RANGE=135-175 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. This orbit need not be contiguous with previous one. ------------------------------------------------------------------------------------------------------------------------------------ 11.6 WAVE HRS ACCUM SC2 G160M 1411 1 60S 2 CALIB FOR 11.5 Comments: SCHEDULE DURING EARTH OCCULTATION OF JUPITER. ------------------------------------------------------------------------------------------------------------------------------------ 12 JUP-N2- HRS ACCUM 2.0 G160M 1300 1 26M 2 1 DARK TIME AURORA Comments: DESIRE CML IN RANGE=185-230 DEG. OBSERVATION SHOULD FIT IN ONE ORBIT. IF ONLY PARTIAL DARK TIME IS AVAILABLE, BREAK EXPOSURE INTO DARK AND LIGHT PORTIONS. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5348 [ 12] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations HRS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ IMAGE ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters BRIGHT=RETURN LOCATE=EXTENDED SEARCH-SIZE=3 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 3.26 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category SOLAR SYSTEM ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category GIANT PLANETS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 1.2,3,4,4.5; CYCLE 4/1-12; SEQ 1-1.2 NON-INT; SEQ 1-4.5 NO GAP; GROUP 1-12 WITHIN 2D GROUP 3,7 WITHIN 11H; ONBOARD ACQ FOR 6.2-8.5; SEQ 6,6.2 NON-INT; SEQ 6-9 NO GAP; CALIB FOR 8.5; ONBOARD ACQ FOR 10.2-12; SEQ 10-10.2 NON-INT; SEQ 10-11.6 NO GAP; CALIB FOR 11.5; DARK TIME; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR-N2 G160M ------------------------------------------------------------------------------------------------------------------------------------ Target Names IO JUP-N1-AURORA JUP-N2-AURORA ------------------------------------------------------------------------------------------------------------------------------------