! $Id: 5424,v 6.1 1995/02/27 16:12:30 pepsa Exp $ coverpage: title_1: HIGH RESOLUTION OBSERVATIONS OF THE JOVIAN UV AURORA: CYCLE4 MEDIUM sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GO longterm: 1 cont_id: 4580 pi_fname: JANE pi_mi: L. pi_lname: FOX pi_inst: SUNY STONY BROOK pi_country: U.S. pi_phone: (516) 632-8317 hours_pri: 5.00 num_pri: 1 hrs: Y off_fname: KATHERINE off_lname: MACCORMACK off_title: ASSO FR SPNSRD PROG off_inst: 2988 off_addr_1: RESEARCH FOUNDATION OF THE STATE UNIVERSITY OF NEW YORK off_addr_2: AT STONY BROOK off_city: STONY BROOK off_state: NY off_zip: 11794 off_country: USA off_phone: (516) 632-9690 ! end of coverpage abstract: line_1: The goals of this proposal are to determine both the kinetic line_2: temperatures in the Jovian auroral region and 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 methane homopause, line_8: the rotational and kinetic temperatures are expected to be equilibrated. line_9: From the amount of methane absorption in the spectral range of 1250-1300 A line_10: the altitude range from which the auroral H2 emission originates will line_11: be estimated. IR observations of H3+ and hydrocarbon molecules line_12: indicate substantially higher temperatures in the auroral region line_13: than in the equatorial or midlatitude thermosphere of Jupiter. The line_14: temperature and altitude measurements proposed here, when coupled with line_15: modeling, will provide information about thermospheric heating due to line_16: precipitating particles and cooling processes at the altitudes of the line_17: uv aurora. The temperatures obtained here will be complementary to those line_18: obtained from the infrared measurements, since they pertain to a line_19: different altitude region. ! ! end of abstract general_form_proposers: lname: FOX fname: JANE mi: L. inst: 2988 country: USA ! lname: CALDWELL fname: JOHN mi: J. inst: 4678 country: CANADA ! lname: KIM fname: YONGHA inst: 2620 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observations are divided into two groups of seven and five HST line_2: orbits to observe the auroral oval with the gratings G160M and G140L, line_3: respectively, as described in part 2 above. The seven HST orbits of G160M line_4: observations will track the westernmost part of the auroral oval. Each orbit line_5: will have a pair of spectra of 15M each by using the G160M grating with two line_6: different spectral ranges. If side 1 of the GHRS is available for cycle 4, line_7: the remaining five HST orbits of observation will be spent producing 3 line_8: pairs of spectra of 5 minutes each for each orbit (6 spectra per orbit) by line_9: using the G140L grating with two different spectral ranges and three line_10: latitudes. Each spectrum of the 5-orbit sequence will be at the central line_11: meridian. ! question: 4 section: 1 line_1: The proposed observations are below 2000 A. The rotational lines in H2 Lyman line_2: bands cannot be resolved in IUE spectra of the Jovian auroral UV emission line_3: due to the low spectral resolution and low sensitivity. line_4: A nominal exposure time has been computed from the published IUE Jovian line_5: aurora UV emission spectra and from parameters in the HST GHRS handbook. line_6: To be conservative, nominal fluxes at 1595 A and 1280 A of 0.05 and line_7: 0.04 ph/cm2/s/A, respectively are chosen, which are only one quarter line_8: of the flux that the maximum auroral emission seen by IUE would produce line_9: at a resolution of 0.3 A. line_10: The fluxes for Jovian aurora at 1595 A and 1280 A are 6.2e-13 and 6.5e-13 line_11: erg/cm2/s/A; the G160M sensitivities (LSA, post-COSTAR) are 4.66e11 and line_12: 6.0e11, respectively; line_13: 15 minutes have been budgeted to obtain one spectrum; line_14: The number of counts per bin will be 900*4.66e11*6.2e-13 = 260 at 1595 A, line_15: and 900*6.0e11*6.5e-13 = 351 at 1280 A, and the S/N = 16 and 19, line_16: respectively. line_17: For the case of observation with the grating G140L, line_18: nominal fluxes at 1595 A and 1280 A of line_19: 0.02 and 0.017 ph/cm2/s/A are chosen, which are again only one quarter of line_20: the flux that the maximum auroral emission seen by IUE would produce at a line_21: resolution of 0.6 A. line_22: The fluxes for Jovian aurora at 1595 A and 1280 A are 2.5e-13 and 2.6e-13 line_23: erg/cm2/s/A; the G140L sensitivities (LSA, post-COSTAR) are 5.34e12 and ! question: 4 section: 2 line_1: 1.30e13, respectively; 5 minutes have been budgeted to obtain one spectrum; line_2: The number of counts per bin will be 300*5.34e12*2.5e-13 = 400 at 1595 A and line_3: 300*1.3e13*2.6e-13 = 1014 at 1280 A, and the S/N = 20 and 32, respectively. ! question: 5 section: 1 line_1: It would help to schedule the proposed planetary observations near the line_2: orbital"stationary points", where the total motion is on the order of 1 line_3: arc min per day or less to eliminate the need for multiple guide star line_4: acquisitions. On-board target acquisition of a Galilean satellite will be line_5: performed, and small offsets from the satellite position to the desired line_6: northern auroral oval area (latitude = 60-75 degree) will be made. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: A proposal for high resolution observation of Jovian aurora by PI Fox, Co-I line_2: Caldwell and Co-I Y. Kim has been accepted with medium priority for cycle 3. line_3: Execution is scheduled a few weeks after the Cycle 4 proposal deadline. line_4: Co-I Caldwell is a GTO with the Observatory Scientist team. In line_5: addition to his original forty hours of GTO, he was awarded another 25 hours line_6: of AUG time in 1991, at the time of the Cycle 2 competition. The entire AUG line_7: award was devoted to recovering capability lost when the GHRS side 1 became line_8: inoperative. Specifically, spatially resolved spectroscopy of Jupiter and line_9: Saturn below 200 nm wavelength, to be done with G200M instead of G140L, was line_10: recognized by the Cycle 2 TAC as being worthy of support. The scientific line_11: goal of that work is not to observe the aurora, but rather to determine the line_12: abundances of trace gases in giant planet atmospheres. From this AUG line_13: award, a spectrum of the equator or Jupiter was obtained in June, 1992. line_14: Additional spectra of Saturn were also obtained in December, 1992. The data line_15: clearly demonstrate the high quality of HST FOS and GHRS spectra, revealing line_16: absorption features of C2H2 on both planets and NH3 on Jupiter. However, line_17: they also clearly reveal the difficulty encountered with GHRS G200M line_18: observations below 1700A for planetary spectra, as noted above. Other GTO line_19: data in hand include FOS UV spectra of Uranus and Neptune. There was a line_20: failed Titan spectral observation, now rescheduled. A DD proposal (PI J. line_21: Westphal) to image the 1990 Saturn equatorial storm has been successful. line_22: An ERO program to image Titan (17 seconds total exposure time) was line_23: successful. The ERO program demonstated that the seasonal ! question: 9 section: 2 line_1: north-south brightness asymmetry on Titan noted by Voyager in 1981 had line_2: reversed a decade earlier. line_3: b. Results from previous related programs: Caldwell's GTO program 1286 is line_4: specifically devoted to imaging the aurora on Jupiter. Initial observations line_5: were made at the time of the Ulysses Jupiter encounter, and these were line_6: extremely successful, and were published in Science. The line_7: first observations were essentially a brief and experimental snapshot of the line_8: north pole. There had been considerable concern that the "red leak" problem line_9: would be overwhelming. With the demonstration that the technique really line_10: works, a follow-up program doing a comprehensive observing GTO program, line_11: covering seven consecutive HST orbits, has been submitted by Caldwell for line_12: execution in summer, 1993. line_13: The main scientific results are that the auroral oval has been successfully line_14: imaged and the size of the oval indicates that the magnetospheric particles line_15: which excite the aurora are on field lines much farther out from Jupiter than line_16: Io (with the implication that if Io is the source, there is significant line_17: evolution of the particle trajectories before they impact Jupiter). Further, line_18: there is a strong suggestion of a "time-of-Jupiter-day" effect in auroral line_19: brightness, with the brightest part of the oval at any specific time being line_20: fixed in local afternoon, and with the possibility that the effect is line_21: modulated by Jupiter's rotational phase. The auroral imaging, both proposed line_22: and actual, will assist with the target acquisition strategies of the line_23: present proposal. ! 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. line_4: Services of Co-I Caldwell will be provided by York University. Caldwell line_5: will be assisted by one full-time post doctoral associate and two graduate line_6: students. The group has a SUN 4/690 server plus work stations, dedicated line_7: to HST data analysis. No additional funds are required at York to support line_8: this work. ! !end of general form text general_form_address: lname: FOX fname: JANE mi: L. category: PI inst: 2988 addr_1: Marine Sciences Research Center addr_2: State University of New York at Stony Brook city: Stony Brook state: NY zip: 11794 country: USA phone: 516-632-8317 telex: 516-632-8820 ! lname: category: CON ! ! 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_1: SEP OF IO JUPITER FROM EARTH LT 60" 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-S1A 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: 3 name_1: JUPITER-S1B 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 355 35 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML= 15 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-S2A descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 25, lev2_2: LAT = -65, RAD = 67531, 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: 5 name_1: JUPITER-S2B descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 25, lev2_2: LAT = -65, RAD = 67531, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 55 95 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: SOUTH AURORA OVAL WHEN CML=75 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-N1A descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 165, lev2_2: LAT = 58, RAD = 67979, 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-N1B descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 165, lev2_2: LAT = 58, RAD = 67979, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 115 155 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=135 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-N2A descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 150, lev2_2: LAT = 58, RAD = 67979, 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-N2B descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 150, lev2_2: LAT = 58, RAD = 67979, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 175 215 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=195 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-N3A descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 175, lev2_2: LAT = 60, RAD = 67842, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 110 150 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML= 130 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-N3B descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 175, lev2_2: LAT = 60, RAD = 67842, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 125 165 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=145 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-N4A descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 155, lev2_2: LAT = 58, RAD = 67979, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 170 210 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML= 190 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-N4B descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, lev2_1: TYPE = CARTO, LONG = 155, lev2_2: LAT = 58, RAD = 67979, wind_1: CML OF JUPITER FROM wind_2: EARTH BETWEEN 185 225 comment_1: GHRS LSA WITH G160M ON JUPITER comment_2: NORTH AURORA OVAL WHEN CML=205 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 4 / 1-16; req_2: ONBOARD ACQ FOR 2 - 10; req_3: SEQ 1 - 10 NO GAP ; comment_1: 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 - 10 ! linenum: 3.000 targname: JUPITER-S1A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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 - 10 WILL BE PROVIDED WHEN comment_5: YONGHA KIM(301-405-1546) comment_6: REMEMBER OFFSET SLOT 1 ! linenum: 4.000 targname: JUPITER-S1B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 1 ! linenum: 5.000 targname: JUPITER-S2A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 2 ! linenum: 6.000 targname: JUPITER-S2B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 2 ! linenum: 7.000 targname: JUPITER-N1A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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 7 - 8 NON-INT; comment_1: REMEMBER OFFSET SLOT 3 ! linenum: 8.000 targname: JUPITER-N1B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 3 ! linenum: 9.000 targname: JUPITER-N2A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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: REMEMBER OFFSET SLOT 4 ! linenum: 10.000 targname: JUPITER-N2B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 4 ! linenum: 11.000 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 12 - 16; req_2: SEQ 11 - 16 NO GAP ; comment_1: STEP-TIME = 0.4S ! linenum: 12.000 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 13 - 16 ! linenum: 13.000 targname: JUPITER-N3A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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 13 - 14 NON-INT; comment_1: LSA SHOULD BE FILLED WITH comment_2: JUPITER DISK 100 PERCENT. comment_3: MORE ACURATE POSITION FOR comment_4: 13 - 16 WILL BE PROVIDED comment_5: YONGHA KIM(301-405-1546) comment_6: REMEMBER OFFSET SLOT 5 ! linenum: 14.000 targname: JUPITER-N3B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 5 ! linenum: 15.000 targname: JUPITER-N4A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1603 num_exp: 1 time_per_exp: 761.6S 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: REMEMBER OFFSET SLOT 6 ! linenum: 16.000 targname: JUPITER-N4B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1275 num_exp: 1 time_per_exp: 761.6S 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 comment_1: REMEMBER OFFSET SLOT 6 ! ! end of exposure logsheet ! No scan data records found