! File: 4950C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:12:01:16 coverpage: title_1: DYNAMICS OF PLANETARY UPPER ATMOSPHERES - CYC2HIGH sci_cat: SOLAR SYSTEM proposal_for: GTO/HSP cont_id: 4257 pi_fname: ROBERT pi_mi: C. pi_lname: BLESS pi_inst: WISCONSIN, UNIVERSITY OF pi_country: USA pi_phone: 608-262-1715 keywords_1: PLANETARY ATMOSPHERES, JOVIAN PLANETS, MARS, UPPER keywords_2: OCCULTATIONS, TEMPERATURE PROFILES hours_pri: 4.80 num_pri: 1 hsp: Y realtime: N time_crit: Y ! end of coverpage abstract: line_1: Observations of planetary upper atmospheres through line_2: stellar occultations are of interest because they line_3: provide information about the radiative and line_4: dynamical processes at work in these rarefied line_5: regions (number density range: 10super13 - 10super15 line_6: cmsuper-3), which could be otherwise measured only line_7: through direct atmospheric probe launched from a line_8: spacecraft. One of the problems with interpretation line_9: of the temperature profiles obtained from line_10: ground-based occultation observations has been that line_11: the numerical inversion of the data is highly line_12: sensitive to photometric errors--especially in line_13: obtaining the mean temperature of the atmosphere. line_14: The much greater stability of photometry that is line_15: possible with the ST will allow us to obtain more line_16: accurate temperature profiles and permit a line_17: comparison of the atmospheric structures of the line_18: Jovian planets with much greater precision than has line_19: been possible in the past. We propose a series of line_20: three occultation observations for each Jovian ! ! end of abstract general_form_proposers: lname: ROBINSON fname: EDWARD mi: L. inst: TEXAS, UNIVERSITY OF country: USA ! lname: BLESS fname: ROBERT mi: C. inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: VAN CITTERS fname: G. mi: W. inst: NATIONAL SCIENCE FOUNDATION country: USA ! lname: DOLAN fname: JOSEPH mi: F. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: WHITE fname: RICHARD mi: L. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: ELLIOT fname: JAMES mi: L. inst: MASSACHUSETTS INSTITUTE OF TECHNOLOGY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to identify those occultations of sufficient line_2: signal-to-noise ratio to achieve the goals outlined line_3: in Section 2. Each observation proceeds as follows: line_4: 1) Obtain a WFPC image to determine the exact line_5: occultation parameters. 2) Acquire occultation line_6: candidate using onboard acquisition mode. 3) Scan line_7: along the track that the star will follow relative line_8: to the planet (along the planetary limb) in order to line_9: determine the planetary contribution to the line_10: background. 4) Start a continuous series of 10ms line_11: integrations enought before the predicted immersion line_12: time that scattered light will not affect the line_13: acquisition. The occultation observation will line_14: require simple tracking on the star before line_15: atmosphere immersion, complex tracking on the line_16: stellar image as it moves along the planetary limb, line_17: and simple tracking after atmosphere emersion. This line_18: sequence of integrations must be continuous. 6) line_19: Scan along the track that the star will follow line_20: relative to the planet. 7) Monitor dark current on ! question: 4 section: 1 line_1: We can achieve a much better signal-to-noise ratio line_2: for the temperature profiles than has been possible line_3: from the ground for the following reasons: (i) the line_4: greatly improved photometric stability of ST line_5: photometry, which will substantially reduce the line_6: errors in the numerical inversion of the data that line_7: is necessary to obtain the temperature profiles; line_8: (ii) our ability to reject background light from the line_9: planetary limb by employing small focal plane line_10: apertures; and (iii) the absence of scintillation line_11: noise, which has strong components at frequencies line_12: comparable to the occultation timescale. ! question: 6 section: 1 line_1: A prior scan over 10 arc-seconds is needed to map line_2: the scattered light field, which is needed for the line_3: data reduction. ! question: 7 section: 1 line_1: Data will be reduced and analyzed at MIT with the line_2: DEC 5000 belonging to the planetary astronomy line_3: group. ! question: 10 section: 1 line_1: Data reduction and analysis will be supported on line_2: computer facilities at MIT. ! question: 13 section: 1 line_1: Observations of the upper atmospheres of Mars and line_2: the Jovian planets with HSP through stellar line_3: occultations will provide infromation about the line_4: radiative and dynamical processes in this region. line_5: The temperature profiles obtained will allow testing line_6: of the various transfer models for each planet. ! !end of general form text general_form_address: lname: BLESS fname: ROBERT mi: C. category: PI inst: UNIVERSITY OF WISCONSIN addr_1: DEPARTMENT OF ASTRONOMY city: MADISON state: WI zip: 53706 country: USA ! lname: ELLIOT fname: JAMES mi: L. category: CON inst: MASSACHUSETTS INSTITUTE OF TECHNOLOGY addr_1: BLDG. 54-422 city: CAMBRIDGE state: MA zip: 02139 country: USA phone: 617-253-6308 telex: 921473 MIT CAM ! ! end of general_form_address records fixed_targets: targnum: 17 name_1: U111 name_2: GSC6311-00105 descr_1: STAR TO BE OCCULTED BY URANUS. descr_2: CLOSE APPROACH AT 14-APR-93:09:34 pos_1: PLATE-ID = 0104, pos_2: RA = 19H 36M 18.944S +/- 0.03", pos_3: DEC = -22D 02' 54.42" +/- 0.04", equinox: J2000 acqpr_1: BKG comment_1: SOLAR ELONG 92D fluxnum_1: 1 fluxval_1: V = 12.6 +/- 0.5 ! targnum: 18 name_1: U111-OFFSET name_2: STAR-1936-2203 descr_1: OFFSET TARGET FOR U111 pos_1: RA = 19H 36M 13.458S +/- 0.05", pos_2: DEC = -22D 02' 34.05" +/- 0.04", equinox: J2000 fluxnum_1: 1 fluxval_1: V = 15.6 +/- 0.1 ! ! end of fixed targets solar_system_targets: targnum: 21 name_1: URANUS-CENTER descr_1: PLANET URANUS lev1_1: STD = URANUS, ACQ = 0.1 comment_1: ACQUISITION TARGET FOR comment_2: BACKGROUND SCANS fluxnum_1: 1 fluxval_1: V = 5.5 +/- 0.5 ! targnum: 24 name_1: U111-BACKGROUND descr_1: OFFSET URANUS lev1_1: STD = URANUS lev2_1: TYPE = POS_ANGLE, lev2_2: RAD = 23.15, lev2_3: ANG = 82.5, lev2_4: REF = NORTH comment_1: FOR USE IN A SCAN OF comment_2: BACKGROUND LEVELS ALONG comment_3: THE PATH OF THE OCCULTED STAR ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 4.000 sequence_1: DEFINE sequence_2: ONBRD-ACQ targname: # config: HSP/VIS opmode: ACQ num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 ! linenum: 6.000 sequence_1: DEFINE sequence_2: BACK-SCAN targname: # config: HSP/PMT/VIS opmode: SPLIT aperture: 1.0 sp_element: F750W/F320N num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: # req_1: SPATIAL SCAN; ! linenum: 7.000 sequence_1: DEFINE sequence_2: RING-OCC targname: # config: HSP/PMT/VIS opmode: SPLIT aperture: 1.0 sp_element: F750W/F320N num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: # ! linenum: 7.500 sequence_1: DEFINE sequence_2: RING-OCC targname: ^ config: S/C opmode: DATA aperture: NONE num_exp: 1 time_per_exp: ^ priority: 1 param_1: FORMAT=FN, req_1: PAR WITH 7.0; comment_1: CAPTURE FGS TLM DURING OCCULTATION. ! linenum: 40.000 sequence_1: USE sequence_2: ONBRD-ACQ targname: URANUS-CENTER time_per_exp: X4 req_1: ONBOARD ACQ FOR 40.01 - 40.05; req_2: SEQ 40.00 - 40.01 NO GAP; ! linenum: 40.010 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, req_1: SEQ 40.01 - 40.05; req_2: GROUP 40.01 - 40.09 WITHIN 9H; req_3: CYCLE 2/40.00 - 40.30; ! linenum: 40.020 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.030 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.040 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.050 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.090 sequence_1: USE sequence_2: ONBRD-ACQ targname: U111-OFFSET time_per_exp: X300 req_1: ONBOARD ACQ FOR 40.10 - 40.30; req_2: SEQ 40.09 - 40.10 NO GAP; req_3: PCS MODE F / 40.09 - 40.10 comment_1: USE FINE LOCK FOR OBSERVATION IF comment_2: BRIGHT ENOUGH GUIDE STARS CAN BE comment_3: FOUND. IF NOT, COARSE TRACK IS comment_4: ACCEPTABLE. ! linenum: 40.100 sequence_1: USE sequence_2: RING-OCC targname: U111 time_per_exp: X150 param_1: SAMPLE-TIME = 0.1, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, req_1: AT 14-APR-93:07:11 +/- 1M; req_2: CRIT OBS; comment_1: END EXPOSURE AT 14-APR-93:12:10. comment_2: IF FPO-FIX AVAILABLE, USE comment_3: SAMPLE-TIME=0.01. ! linenum: 40.250 sequence_1: USE sequence_2: ONBRD-ACQ targname: URANUS-CENTER time_per_exp: X4 req_1: ONBOARD ACQ FOR 40.26 - 40.30; req_2: SEQ 40.25 - 40.30 NO GAP; ! linenum: 40.260 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, req_1: SEQ 40.26 - 40.30; req_2: GROUP 40.10 - 40.30 WITHIN 9H; ! linenum: 40.270 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.280 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.290 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! linenum: 40.300 sequence_1: USE sequence_2: BACK-SCAN targname: U111-BACKGROUND time_per_exp: X133 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 10000, param_4: VIS-ANALOG = 1000, ! ! end of exposure logsheet scan_data: line_list: 40.01, 40.03, 40.05, 40.26, 40.28, 40.30 fgs_scan: cont_dwell: C dwell_pnts: 0 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 32.5000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0750 first_line_pa: 263.6000 scan_frame: CEL len_offset: 0. wid_offset: 0. ! line_list: 40.02, 40.27 fgs_scan: cont_dwell: C dwell_pnts: 0 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 32.5000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0750 first_line_pa: 263.6000 scan_frame: CEL len_offset: 0. wid_offset: 0.5 ! line_list: 40.04, 40.29 fgs_scan: cont_dwell: C dwell_pnts: 0 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 32.5000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0750 first_line_pa: 263.6000 scan_frame: CEL len_offset: 0. wid_offset: -0.5 ! ! end of scan data