! File: 4580C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:18:30:12 coverpage: title_1: HIGH RESOLUTION OBSERVATIONS OF THE JOVIAN UV AURORA -- CYCLE 3 MED sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GO pi_fname: JANE pi_mi: L. pi_lname: FOX pi_inst: SUNY STONY BROOK pi_country: U.S. hours_pri: 6.00 num_pri: 1 hrs: Y funds_length: 12 off_fname: KATHERINE off_mi: L. off_lname: MACCORMACK off_title: ASSOC FR SPONSRD PRG off_inst: 2988 off_addr_1: RESEARCH FOUNDATION OF SUNY AT STONY BROOK off_city: STONY BROOK off_state: NY off_zip: 11794 off_country: USA off_phone: 516-632-6960 ! end of coverpage abstract: line_1: This proposal has the specific goal of determining the kinetic line_2: temperatures in the Jovian auroral region in the altitude range where line_3: the precipitating particles deposit their energy and from which emission line_4: in the H2 Lyman and Werner bands originates. Due to the low spectral line_5: resolution and low sensitivity of the IUE, rotational temperatures of H2 line_6: cannot be determined from IUE spectra of the Jovian ultraviolet aurora. line_7: At the altitudes of the uv aurora, near or below the homopause, line_8: the rotational and kinetic temperatures are expected to be equilibrated. line_9: IR observations of H3+ and hydrocarbon molecules (methane, acetylene, line_10: etc) indicate substantially higher temperatures in the auroral region line_11: than in the equatorial or midlatitude thermosphere of Jupiter. The line_12: temperature measurements proposed here, when coupled with modeling, will line_13: provide information about thermospheric heating due to precipitating line_14: particles and cooling processes at the altitudes of the uv aurora. The line_15: temperatures obtained here will be complementary to those obtained line_16: from the infrared measurements, since they pertain to a different line_17: altitude region. ! ! end of abstract general_form_proposers: lname: FOX fname: JANE title: PI mi: L. inst: SUNY STONY BROOK country: USA esa: N ! lname: CALDWELL fname: JOHN mi: J. inst: YORK UNIVERSITY country: CANADA ! lname: KIM fname: YONGHA inst: UNIVERSITY OF MARYLAND country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Jovian ultraviolet auroral emissions were first detected by the Voyager line_2: spacecraft in 1979 (Broadfoot et al, 1979) and have been observed by the IUE line_3: telescope on a regular basis over the last decade (Livengood and Moos, line_4: 1990; Prange and Elkhamsi, 1991). One of the most useful signatures of the line_5: Jovian uv aurora is the H2 Lyman and Werner band emissions (800-1650 A). IUE line_6: observations of these H2 emissions have only been carried out in the low line_7: spectral resolution mode (about 10 A); low sensitivity has precluded the IUE line_8: telescope from making higher spectral resolution observations. In these IUE line_9: spectra, it was not possible to distinguish individual rotational lines in line_10: the H2 Lyman and Werner bands, which are typically 1-2 A apart. At the high line_11: resolution of GHRS of the HST, the rotational lines will be easily resolved. line_12: This will allow a direct determination of the rotational temperature of line_13: molecular hydrogen in the auroral region. IR observations of H3+ and hydro- line_14: carbon molecules indicate substantially higher temperatures in the auroral line_15: regions than in the mid-latitude upper atmosphere of Jupiter (Drossart et al., line_16: 1989; Caldwell et al., 1988; Kostiuk et al., 1987). Theoretical models of the line_17: observed H3+ IR emission lines in the auroral regions also require high line_18: temperatures (Kim et al, 1992). The temperatures in the altitude region line_19: where the energy of the precipitating particles is deposited could be anywhere line_20: from 300 K, if the auroral atmosphere is rapidly mixed with the cooler line_21: non-auroral atmosphere, to several thousand degrees, if the mixing is very line_22: slow (Waite et al, 1983). These measurements will thus also provide information line_23: about Jovian upper atmosphere dynamics, and about the energy spectrum of the ! question: 2 section: 2 line_1: precipitating particles, which is also crucial for heating. It should be noted line_2: here that the altitude region from which the H3+ emissions originate and the line_3: region from which the IR hydrocarbon emissions originate are different from line_4: that of the uv aurora. Thus the rotational temperatures derived from this study line_5: will be complementary to the temperatures indicated by the IR spectra obtained line_6: from ground-based measurements, and together with the H3+ derived temperatures, line_7: will yield a fairly complete picture of temperatures in the auroral line_8: thermosphere. line_9: Since the shortest wavelength channel of GHRS (1150-1450 A) is not currently line_10: available, the best spectral range for determining a rotational temperature is line_11: the 1586-1620 A range, where strong rotational lines in the v'= 3 to v'' = 10, line_12: v'= 4 to v'' = 11, v'= 5 to v''=12, and v'= 6 to v''=13 Lyman bands appear. line_13: Figure 1 shows synthetic spectra of Jovian aurora emission in this spectral line_14: range for two assumed temperatures at 0.3 A resolution. The photon flux here line_15: was computed assuming half the maximum flux of the Jovian uv auroral line_16: emission observed by IUE (eg. Livengood and Moos, 1990, Livengood et al, 1992). line_17: Since auroral activity varies over both time and space, in order to determine line_18: the magnitude of this variability, we need to observe the auroral oval over line_19: one full period of Jupiter's rotation (10 hours). We have chosen here to line_20: concentrate on the northern auroral oval to demonstrate the feasibility of line_21: the investigation, because better images of it have been achieved previously line_22: by the HST/FOC than for the south. Its spatial characteristics are therefore line_23: better known. Furthermore, auroral observations at other wavelengths have ! question: 2 section: 3 line_1: shown the northern aurora to be less variable with time than the southern one. line_2: We will study the northern and southern oval. First, we will devote six line_3: HST orbits to observing the westernmost point on the oval when line_4: CML is 120 and 180. FOC imaging has shown this to be the brightest point. line_5: Three HST orbits will be used to observe southern oval. The ground based IR line_6: observations have shown acive aurora in the southern oval. Then, we will line_7: longitude 180 deg of the northern oval for one HST orbit when line_8: longitude 180 deg is seen in mornig side and noon of the Jupiter. This line_9: longitude has been observed to be brightest for thermal emissions due to line_10: hydrocarbons, but FOC imaging shows it to be less bright than other parts of line_11: the oval. Note that an IUE study with very low spatial resolution by line_12: Livengood et al (1992) has claimed that this longitude range is bright in the line_13: uv, so this sequence of observations will be a good test of the apparent line_14: discrepancy between the IUE result and the new FOC images by Caldwell et al line_15: (1992). line_16: Our observations will provide alternative quantitative information on the uv line_17: brightness of the auroral oval and will provide unique measurements of line_18: temperature variation along the oval at that altitude. ! question: 3 section: 1 line_1: It may help to schedule the proposed planetary observations near the orbital line_2: "stationary points", where the total motion is of order 1 arc min per day or line_3: less to eliminate the need for multiple guide star acquisitions. On-board line_4: target acquisition of a Galilean satellite will be performed, and small line_5: offsets from the satellite position to the desired north auroral oval area line_6: (latitude = 60-75 degree) will be made. line_7: There will be ten HST orbits of observations, with each orbit having two line_8: spearate spectra of 14M each. The orbits will come in four groups, two, two, line_9: four, two, respectively, to observe different parts of the auroral oval, as line_10: described in part 2 above. ! question: 4 section: 1 line_1: The proposed observations are below 2000 A. The rotational lines in H2 Lyman line_2: bands have never been resolved in IUE spectra of Jovian auroral UV emission line_3: due to the low spectral resolution and low sensitivity. ! question: 4 section: 2 line_1: A nominal exposure time has been computed from the published IUE Jovian line_2: aurora UV emission spectra and from parameters in the HST GHRS handbook. To be line_3: conservative, a nominal flux at a rotational line P(3)(v'=3,v''=10) 1595 A of line_4: 0.02 ph/cm2/s/A is chosen, which is only one tenth of the flux that the line_5: maximum auroral emission seen by IUE would produce at a resolution of 0.3 A. line_6: The flux for Jovian aurora at 1595 A is 2.5e-13 erg/cm2/s/A; line_7: the G160M sensitivity (LSA) is 4.75e11; line_8: total 28 minutes have been budgeted to obtain one spectrum; line_10: If the data are binned to 0.3 A, the number of counts per bin will be line_11: 530, and the S/N = 23. The 0.3 A resolution will line_12: resolve the (v'=3,v''=10), and (v'=4, v''=11) Lyman bands of H2. ! question: 5 section: 1 line_1: When COSTAR is installed into the HST in late 1993, the uv throughput of the line_2: GHRS will be decreased by the additional two reflections of the COSTAR optics. line_3: Because the aurora is diffuse, the improved spatial resolution resulting from line_4: COSTAR will not produce significantly better spectra. It is therefore line_5: advantageous to schedule this proposal before the HST Repair Mission. line_6: Taking into account that Jupiter will enter the solar exclusion region in the line_7: fall of 1993, it would be advantageous schedule this proposal in late summer, line_8: 1993. That would also help with the preference to schedule it near a Jovian line_9: stationary point, to minimize Jupiter's apparent motion and therefore to line_10: minimize the number of new guide star acquisitions required. ! question: 6 section: 1 line_1: None ! question: 7 section: 1 line_1: A simple approach will be followed first to determine rotational temperatures line_2: of H2 by computing ratios of intensities of rotational lines with low J numbers line_3: to high J numbers (for example P(1) to P(5) in v'=5, v''=12, see figure 1). line_4: The temperature obtained from this approach represents an average temperature line_5: over the altitude region where the emissions orginate. line_6: Electron transport calculations will be carried out for the observed locations line_7: of Jovian aurora to simulate auroral particle precipitation. This was done for line_8: parametric studies of Jovian aurora by the P.I. and one of the Co-I.'s (Y. Kim) line_9: in the past (Kim and Fox, 1992). Synthetic spectra will be made to fit the line_10: observed spectra by assuming various rotational temperatures and using the line_11: emission profiles computed from a model which employs an electron line_12: transport code developed by H. S. Porter. ! question: 8 section: 1 line_1: None ! question: 9 section: 1 line_1: Co-I Caldwell is a GTO with the Observatory Scientist team. In line_2: addition to his original forty hours of GTO, he was awarded another 25 hours line_3: of AUG time in 1991, at the time of the Cycle 2 competition. The entire AUG line_4: award was devoted to recovering capability lost when the GHRS side 1 became line_5: inoperative. Specifically, spatially resolved spectroscopy of Jupiter and line_6: Saturn below 200 nm wavelength, to be done with G200M instead of G140L, was line_7: recognized by the Cycle 2 TAC as being worthy of support. The scientific goal line_8: of that work is not to observe the aurora, but rather to determine the line_9: abundances of trace gases in giant planet atmospheres. From this AUG line_10: award, a spectrum of the equator or Jupiter has been obtained in June, 1992. line_11: Analysis is underway. Other GTO data in hand include UV spectra of Uranus. line_12: Neptune spectra are expected in August. There was a failed Titan spectral line_13: observation. A DD proposal (PI J. Westphal) to image the 1990 Saturn line_14: equatorial storm has been successful (see below). An ERO program to image line_15: Titan (17 seconds total exposure time) was successful (see below). Caldwell line_16: is also a Co-I on a GO proposal (PI B. Zellner) to observe the satellites of line_17: Mars, with data expected in January, 1993. line_18: This is the first HST proposal by PI Fox and by Co-I Y. Kim ! question: 9 section: 2 line_1: Results from previous related programs: Caldwell's GTO program 1286 is line_2: specifically devoted to imaging the aurora on Jupiter. Initial observations line_3: were made at the time of the Ulysses Jupiter encounter, and these were line_4: extremely successful, with a publication now in press with SCIENCE. The first line_5: observations were essentially a brief and experimental snapshot of the north line_6: pole. There had been considerable concern that the "red leak" problem would line_7: be overwhelming. With the demonstration that the technique really works, a line_8: follow-up program doing a comprehensive observing GTO program, covering seven line_9: consecutive HST orbits, has been submitted by Caldwell for scheduling in line_10: April, 1993. There will also be an experimental snapshot program on the south line_11: pole in November, 1992. line_12: The main scienitific results are that the auroral oval has been successfully line_13: imaged and the size of the oval indicates that the magnetospheric particles line_14: which excite the aurora are on field lines much farther out from Jupiter than line_15: Io (with the implication that if Io is the source, there is significant line_16: evolution of the particle trajectories before they impact Jupiter). Further, line_17: there is a strong suggestion of a "time-of-Jupiter-day" effect in auroral line_18: brightness, with the brightest part of the oval at any specific time being line_19: fixed in local afternoon, and with the possibility that the effect is line_20: modulated by Jupiter's rotational phase. The auroral imaging, both proposed line_21: and actual, will assist with the target acquisition strategies of the present line_22: proposal. ! question: 9 section: 3 line_1: (1) "Titan: Evidence for Seasonal Change - A Comparison of Hubble line_2: Space Telescope and Voyager Images", J. Caldwell et al., Icarus 96, 1-9, 1992. line_3: (2) "Hubble Space Telescope Imaging of the North Polar Aurora On line_4: Jupiter", J. Caldwell, B. Turgeon, H.-M. Hua, Science, in press, 1992. line_5: (3) "Hubble Space Telescope Observations of the 1990 Equatorial line_6: Disturbance on Saturn: Images, Albedos, and Limb Darkening", J. Westphal et line_7: al., Icarus, submitted, 1992. line_8: A paper on the Saturn north polar hexagon and its companion "little white line_9: spot", based on the same images as paper (3) above is in the final stages of line_10: preparation for journal submission by Caldwell et al. ! question: 10 section: 1 line_1: Services of the PI during the academic year will be provided by SUNY-Stony line_2: Brook. Use of the atmospheric sciences computation facility, currently line_3: a VAX 6310, will also be available without charge. ! !end of general form text general_form_address: lname: Fox fname: Jane mi: L. category: PI inst: SUNY Stony Brook addr_1: Inst. for Terrestrial and Planetary Atmospheres addr_2: State University of New York at Stony Brook city: Stony Brook state: NY zip: 11794 country: USA phone: 516-632-8317 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: IO-ACQ descr_1: SATELLITE IO lev1_1: STD = JUPITER, ACQ = 0.1 lev2_1: STD = IO wind_2: SEP OF IO JUPITER FROM EARTH GT 30" comment_1: HRS ACQUISITION OF IO FOR PEAKUP ON comment_2: SATELLITE CENTER. LSA IS REQUIRED. fluxnum_1: 1 fluxval_1: SURF(V) = 5.8 +/- 0.5 fluxnum_2: 2 fluxval_2: SIZE = 1.0 +/- 0.2 ! targnum: 2 name_1: JUPITER-N1A1 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 100, lev2_2: LAT = 68, RAD = 67366 wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 3 name_1: JUPITER-N1B1 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 110, lev2_2: LAT = 68, RAD = 67366, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 4 name_1: JUPITER-N2A1 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 137.5, lev2_2: LAT = 55, RAD = 68192, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 5 name_1: JUPITER-N2B1 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 147.5, lev2_2: LAT = 55, RAD = 68192, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 6 name_1: JUPITER-N1A2 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 100, lev2_2: LAT = 66, RAD = 67474, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML = 120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 7 name_1: JUPITER-N1B2 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 110, lev2_2: LAT = 66, RAD = 67474, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 8 name_1: JUPITER-N2A2 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 137.5, lev2_2: LAT = 53, RAD = 68341, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML= 180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 9 name_1: JUPITER-N2B2 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 147.5, lev2_2: LAT = 53, RAD = 68341, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 10 name_1: JUPITER-N1A3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 100, lev2_2: LAT = 70, RAD = 67266, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 11 name_1: JUPITER-N1B3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 110, lev2_2: LAT = 70, RAD = 67266, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 100 140 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=120 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 12 name_1: JUPITER-N2A3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 137.5, lev2_2: LAT = 57, RAD = 68049, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML= 180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 13 name_1: JUPITER-N2B3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 147.5, lev2_2: LAT = 57, RAD = 68049, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 160 200 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=180 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 14 name_1: JUPITER-S1 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 330, lev2_2: LAT = -68, RAD = 67366, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 340 20 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML= 0 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 15 name_1: JUPITER-S2 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 340, lev2_2: LAT = -68, RAD = 67366, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 340 20 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML= 0 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 16 name_1: JUPITER-S3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 60, lev2_2: LAT = -63, RAD = 67651, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 40 80 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML=60 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 17 name_1: JUPITER-S4 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 50, lev2_2: LAT = -63, RAD = 67651, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 40 80 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML=60 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 20 name_1: JUPITER-N3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 180, lev2_2: LAT = 55, RAD = 68192, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 130 170 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML= 150 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! targnum: 21 name_1: JUPITER-N4 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 110, lev2_2: LAT = 0, RAD = 71398, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 130 170 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: EQUATOR WHEN CML= 150 fluxnum_1: 1 fluxval_1: SURF(V) = 5.4 fluxnum_2: 2 fluxval_2: SURF-LINE(1596) = 6.2 +/- 3.5 E-14 fluxnum_3: 3 fluxval_3: W-LINE(1596) = 0.3 +/- 0.1 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: IO-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE = 5 param_2: BRIGHT = RETURN param_3: LOCATE = EXTENDED req_1: CYCLE 3 / 1-28; req_2: ONBOARD ACQ FOR 2 - 6; req_3: SEQ 1 - 6 NO GAP ; comment_1: IF LOCATE = EXTENDED CAN BE USED, comment_2: THEN DELETE LINE 2 (DON'T comment_3: PERFORM ACQ/PEAKUP). comment_4: STEP-TIME = 0.4S ! linenum: 2.000 targname: IO-ACQ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 3 - 6 ! linenum: 3.000 targname: JUPITER-N1A1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 3 - 4 NON-INT ; comment_1: LSA SHOULD BE FILLED WITH comment_2: JUPITER DISK 100 PERCENT. comment_3: MORE ACURATE POSITION FOR comment_4: 3 - 6 WILL BE PROVIDED WHEN comment_5: CML IS KNOWN. CONTACT comment_6: YONGHA KIM(301-405-1546) ! linenum: 4.000 targname: JUPITER-N1B1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 5.000 targname: JUPITER-N2A1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 5 - 6 NON-INT; ! linenum: 6.000 targname: JUPITER-N2B1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 7.000 targname: IO-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE = 5 param_2: BRIGHT = RETURN param_3: LOCATE = EXTENDED req_1: ONBOARD ACQ FOR 8 - 12; req_2: SEQ 7 - 12 NO GAP; comment_1: IF LOCATE = EXTENDED CAN BE USED, comment_2: THEN DELETE LINE 8 (DON'T comment_3: PERFORM ACQ/PEAKUP). comment_4: STEP-TIME = 0.4S ! linenum: 8.000 targname: IO-ACQ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 9 - 12 ! linenum: 9.000 targname: JUPITER-N1A2 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 9 - 10 NON-INT; comment_1: LSA SHOULD BE FILLED WITH comment_2: JUPITER DISK 100 PERCENT. comment_3: MORE ACURATE POSITION FOR comment_4: 9 - 12 WILL BE PROVIDED WHEN comment_5: CML IS KNOWN. CONTACT comment_6: YONGHA KIM(301-405-1546) ! linenum: 10.000 targname: JUPITER-N1B2 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 11.000 targname: JUPITER-N2A2 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 11 - 12 NON-INT; ! linenum: 12.000 targname: JUPITER-N2B2 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 13.000 targname: IO-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE = 5 param_2: BRIGHT = RETURN param_3: LOCATE = EXTENDED req_1: ONBOARD ACQ FOR 14 - 22; req_2: SEQ 12 - 22 NO GAP; comment_1: IF LOCATE = EXTENDED CAN BE USED, comment_2: THEN DELETE LINE 14 (DON'T comment_3: PERFORM ACQ/PEAKUP). comment_4: STEP-TIME = 0.4S ! linenum: 14.000 targname: IO-ACQ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 15 - 22 ! linenum: 15.000 targname: JUPITER-S1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 15 - 16 NON-INT; comment_1: LSA SHOULD BE FILLED WITH comment_2: JUPITER DISK 100 PERCENT. comment_3: MORE ACURATE POSITION FOR comment_4: 15 - 22 WILL BE PROVIDED WHEN comment_5: CML IS KNOWN. CONTACT comment_6: YONGHA KIM(301-405-1546) ! linenum: 16.000 targname: JUPITER-S2 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 17.000 targname: JUPITER-S3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 17 - 18 NON-INT ! linenum: 18.000 targname: JUPITER-S4 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 19.000 targname: JUPITER-N1A3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 19 -20 NON-INT; ! linenum: 20.000 targname: JUPITER-N1B3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 21.000 targname: JUPITER-N2A3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 21 - 22 NON-INT; ! linenum: 22.000 targname: JUPITER-N2B3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! linenum: 23.000 targname: IO-ACQ config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE = 5 param_2: BRIGHT = RETURN param_3: LOCATE = EXTENDED req_1: ONBOARD ACQ FOR 24 - 28; req_2: SEQ 27 - 28 NO GAP; comment_1: IF LOCATE = EXTENDED CAN BE USED, comment_2: THEN DELETE LINE 24 (DON'T comment_3: PERFORM ACQ/PEAKUP). comment_4: STEP-TIME = 0.4S ! linenum: 24.000 targname: IO-ACQ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 27 - 28 ! linenum: 27.000 targname: JUPITER-N3 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES req_1: SEQ 27 - 28 NON-INT; ! linenum: 28.000 targname: JUPITER-N4 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 783.2S s_to_n: 10 s_to_n_time: 15M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT = 5 param_2: FP-SPLIT = FOUR param_3: COMB = FOUR param_4: DOPPLER = ON param_5: STEP-TIME = 0.2 param_6: CENSOR = YES ! ! end of exposure logsheet ! No scan data records found