! File: 4948C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:11:55:34 coverpage: title_1: SATURN RING DYNAMICS - CYC2HIGH sci_cat: SOLAR SYSTEM proposal_for: GTO/HSP cont_id: 1081 pi_fname: ROBERT pi_mi: C. pi_lname: BLESS pi_inst: WISCONSIN, UNIVERSITY OF pi_country: USA pi_phone: 608-262-1715 keywords_1: SATURN'S RINGS, OCCULTATIONS, RING DYNAMICS hours_pri: 3.01 num_pri: 1 hsp: Y time_crit: Y ! end of coverpage abstract: line_1: Understanding the dynamics of the rings is essential line_2: to our eventual understanding of their origin. Did line_3: they form recently or along with Saturn itself? We line_4: propose a series of stellar occultation observations line_5: in order to continue the dynamical investigation of line_6: Saturn's rings, at high spatial resolution, begun by line_7: the Voyager spacecraft. Revision History: Updated line_8: for cycle 2 submission, 4/24/92, asb.; cycle 2 line_9: updates, ASB 1/24/93; ! ! 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 use the ST orbit parameters and catalogs line_2: of the objects of interest to identify those line_3: occultations of sufficient signal-to-noise ratio to line_4: achieve the goals outlined in Section 2. Each line_5: observation will require (i) external "darks", taken line_6: on the dark earth as a standard calibration source, line_7: (ii) a set of two sequential onboard acquisitions, line_8: (iii) a scan of about 30-40 arcseconds along the line_9: track that the object will follow relative to line_10: Saturn's rings; and (iv) a time series run on the line_11: object with whatever filter-aperture combination line_12: that is chosen for the observation. For some line_13: occultations to be observed in the far uv, prior line_14: multi-filter photometry of the object will be line_15: necessary in order to determine the most appropriate line_16: filter to use for the occultation. The default line_17: filter set is F750W/F320N. For now, we shall assume line_18: that the calibration and observation time will line_19: average about 3 hours per occultation observed. line_20: About ten occultations would be required to achieve ! question: 4 section: 1 line_1: We can achieve a much better signal-to-noise ratio line_2: for Saturn ring occultations than would be possible line_3: from the ground because of (i) the absence of line_4: scintillation noise, which has strong components at line_5: frequencies corresponding to the occultation line_6: timescales, and (ii) our ability to reject line_7: background light from the rings themselves by line_8: employing small focal plane apertures. ! question: 5 section: 1 line_1: Acquisition of the star near Saturn may prove to be line_2: difficult. ! question: 6 section: 1 line_1: A prior scan over 30-40 arcseconds 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: VAX 11-750 belonging to the planetary astronomy line_3: group. ! question: 8 section: 1 line_1: SV test HSP09A must be completed before these observations line_2: are made because the exact observation sequence may need line_3: to be modified depending on the results of the SV test. ! question: 10 section: 1 line_1: Data reduction and analysis will be supported on computer line_2: facilities at MIT. ! question: 13 section: 1 line_1: Observations of a series of stellar occultations by line_2: Saturn's rings with the HSP (or perhaps FOS) can line_3: provide precise orbits of ringlets, other sharp line_4: features, waves, and other phenomena in the Saturn line_5: system at high spatial resolution. From these data line_6: further understanding of the present dynamical state line_7: of the ring system can be gained. This understanding line_8: should improve our knowledge of the past history and line_9: conditions of formation of the rings. ! !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 phone: 608-262-1715 ! 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: 14 name_1: GSC5801-00416 descr_1: STAR TO BE OCCULTED BY SATURN. descr_2: CLOSE APPROACH AT 7-DEC-93:19:13 pos_1: PLATE-ID = 00WO, pos_2: RA = 21H 51M 32.049S +/- 0.06", pos_3: DEC = -14D 30' 47.28" +/- 0.06", equinox: J2000 acqpr_1: BKG comment_1: SOLAR ELONG 69D fluxnum_1: 1 fluxval_1: B = 10.7 +/- 0.5 ! targnum: 15 name_1: 00416-OFFSET name_2: GSC5801-00480 descr_1: OFFSET TARGET FOR GSC5801-00416 pos_1: PLATE-ID = 00WO, pos_2: RA = 21H 51M 34.818S +/- 0.03", pos_3: DEC = -14D 30' 58.49" +/- 0.06", equinox: J2000 fluxnum_1: 1 fluxval_1: B = 14.6 +/- 0.1 ! ! end of fixed targets solar_system_targets: targnum: 18 name_1: 00416-BACKGROUND descr_1: OFFSET SATURN lev1_1: STD = SATURN lev2_1: TYPE = POS_ANGLE, lev2_2: RAD = 13.94, lev2_3: ANG = 20.5, 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: 12.010 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, req_1: SEQ 12.01 - 12.07; req_2: GROUP 12.01 - 12.09 WITHIN 9H; req_3: CYCLE 2/12.01 - 12.32; ! linenum: 12.030 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, ! linenum: 12.070 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, ! linenum: 12.090 sequence_1: USE sequence_2: ONBRD-ACQ targname: 00416-OFFSET time_per_exp: X60 req_1: ONBOARD ACQ FOR 12.10; req_2: SEQ 12.09 - 12.10 NO GAP; req_3: PCS MODE F / 12.09 - 12.10; comment_1: USE FINE LOCK ONLY. IF BRIGHT comment_2: ENOUGH GUIDE STARS CANNOT BE comment_3: FOUND, CANCEL OBSERVATION. ! linenum: 12.100 sequence_1: USE sequence_2: RING-OCC targname: GSC5801-00416 time_per_exp: X60 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, req_1: AT 7-DEC-93:20:16 +/- 1M; req_2: CRIT OBS; comment_1: END EXPOSURE AT 7-DEC-93:21:15. comment_2: OCCULTATION IS A NOMINAL MISS. comment_3: TIMES WILL BE UPDATED (OR comment_4: OBSERVATION WILL BE CANCELLED) comment_5: 1.5 TO 4 MONTHS BEFORE OBSERVATION. comment_6: CONTACT: AMANDA S. BOSH, MIT ! linenum: 12.260 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, req_1: SEQ 12.26 - 12.32; req_2: GROUP 12.10 - 12.32 WITHIN 9H; ! linenum: 12.280 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, ! linenum: 12.320 sequence_1: USE sequence_2: BACK-SCAN targname: 00416-BACKGROUND time_per_exp: X467 param_1: SAMPLE-TIME = 0.01, param_2: DATA-FORMAT = ALL, param_3: PMT-ANALOG = 1000, param_4: VIS-ANALOG = 100, ! ! end of exposure logsheet scan_data: line_list: 12.01, 12.07, 12.26, 12.32 fgs_scan: cont_dwell: C dwell_pnts: 0 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 28.0000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0750 first_line_pa: 249.4000 scan_frame: CEL len_offset: 0. wid_offset: 0 ! line_list: 12.03, 12.28 fgs_scan: cont_dwell: C dwell_pnts: 0 dwell_secs: 0.00 scan_width: 2.0000 scan_length: 28.0000 sides_angle: 90.0000 number_lines: 5 scan_rate: 0.0750 first_line_pa: 249.4000 scan_frame: CEL len_offset: 0. wid_offset: 1.0 ! ! end of scan data