! File: 5021C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:15:49:52 coverpage: title_1: HST OBSERVATIONS OF COMET SHOEMAKER-LEVY (1993E) sci_cat: SOLAR SYSTEM sci_subcat: COMETS proposal_for: GO pi_fname: HAROLD pi_mi: A. pi_lname: WEAVER pi_inst: STSCI pi_country: USA hours_pri: 3.00 num_pri: 1 wf_pc: Y fos: Y realtime: Y time_crit: Y funds_length: 12 off_fname: HERVEY off_mi: S. off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: 3470 off_addr_1: SPACE TELESCOPE SCIENCE INSTITUTE off_addr_2: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA ! end of coverpage abstract: line_1: Comet Shoemaker-Levy (1993e) is a comet that has recently broken line_2: up into many fragments, apparently somewhere in the vicinity line_3: of Jupiter. Ground-based observations reveal a string of sub-nuclei line_4: spaced over a distance of about one arcminute. HST observations line_5: of this object with the PC should reveal a fascinating spatial line_6: morphology that is more detailed than any images obtained from line_7: ground-based telescopes. In addition, FOS exposures searching line_9: for the UV band of OH should provide a sensitive indicator of any line_10: ice sublimation that has occurred since the comet's break-up. ! ! end of abstract general_form_proposers: lname: WEAVER fname: HAROLD title: PI mi: A. inst: STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The program consists of two separate visits to the comet with line_2: three orbits required for each visit. The nominal separation line_3: of each visit should be about two to six weeks. line_4: The two visits are identical with regard to the observing line_5: sequence. Thus, I will explain here only the details associated line_6: with the first visit. line_8: The first orbit will have a GS ACQ followed by a real-time line_9: pointing offset command, followed by three short PC line_10: images through the F555W filter. line_12: The second orbit will have a GS REACQ followed by two long line_13: PC images through the F555W filter. line_15: The third orbit will have a GS ACQ followed by a real-time line_16: pointing offset command, followed by a long FOS RED IMAGE line_17: exposure with the G270H grating. line_18: We would like to have the option to use an unscheduled SIP line_19: after the ACQ IMAGE to refine the pointing. ! question: 3 section: 2 line_1: Since the predicted target ephemeris six weeks prior to the line_2: HST observations may be offset by up to two arcmin from the line_3: comet's actual position, we will require a realtime uplink line_4: to correct the pointing prior to the first PC image. line_5: The pointing correction will be determined from ground line_6: based astrometry taken about one or two weeks prior to line_7: the HST observations. ! question: 3 section: 3 line_1: Each visit will thus look like: line_2: Start of 1st visib. period: full GS acq. line_3: RT (pointed) uplink line_4: 100s F555W PC image line_5: 400s PC image (downlinked) line_6: Start of 2nd visib. period: GS reacq. line_7: 800s PC image line_8: 800s PC image line_9: Start of 3rd visib. period: full GS acq. line_10: RT (pointed) uplink line_11: 11m FOS/RD G270H spectrum line_12: 11m FOS/RD G270H spectrum line_13: Three orbit sequence repeated once. ! question: 4 section: 1 line_1: HST observations of Comet Shoemaker-Levy (1993e) should provide line_2: better detail on the break-up of this object than is available line_3: from any other source. ! question: 4 section: 2 line_1: ! question: 4 section: 3 line_1: ! question: 5 section: 1 line_1: Since the ephemeris for Comet Shoemaker-Levy (1993e) is so uncertain, line_2: a real-time pointing correction must be uplinked prior to the line_3: first PC image. line_4: Reliable ephemeris data will be obtained from ground-based line_5: observations taken approximately one week prior to the line_6: HST observations. Since the ground-based data will be obtained line_7: during lunar dark time, the HST observations should be scheduled line_8: near the end of the month. Thus, the first HST observing window line_9: opens during the lastweek of June and extends into the first week of line_10: July. The second window will be from the middle of July until the line_11: comet enters the solar exclusion zone in the beginning of August. ! question: 7 section: 1 line_1: The images and spectra will be reduced and analyzed using the line_2: PI's workstation at the STScI. Deconvolution of the images will line_3: will be performed using theoretical PSF's. ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: ID no. 3064: HST Observations of Comet Levy (1990c) line_2: (A'Hearn, Arpigny, and Feldman are Co-Is), an imaging-only line_3: program that is only peripherally related to the line_4: current program. line_6: ID no. 2481: HST Observations of Periodic Comets (A'Hearn, Arpigny, line_7: and Feldman are Co-Is), only peripherally related to this program. line_9: ID no. 2483: The Volatile Composition of New Comets (A'Hearn, Arpigny, line_10: and Feldman are Co-Is), only peripherally related to this program. line_12: ID no. 2442: Cometary Parent Molecules, P.D. Feldman, PI (A'Hearn line_13: and Weaver are Co-Is), only peripherally related to this program. line_15: Cycle 2 program: line_16: ID no. 3707: HST Observations of Periodic Comets (A'Hearn, Arpigny, line_17: and Feldman are Co-Is), only peripherally related to this program. ! question: 9 section: 2 line_1: ID no. 3064: Two sets of WFC images of comet Levy were obtained 6.5 line_2: hours apart on 27 September 1990 in order to investigate its temporal line_3: variability. An arc of large grains was observed propagating line_4: sunward with a projected velocity of 0.16 km/sec. line_6: ID no. 2481: P/Hartley 2 was successfully observed in late 9/91 line_7: These observations produced the first detection of CO Cameron bands in line_8: comets. This emission is essentially a unique tracer of the CO2 line_9: abundance in comets. Additionally we obtained a beautiful spectrum line_10: of the comet covering the entire spectral range 1200-6800 A, from line_11: which we are compiling (still in progress) an inventory of volatiles line_12: in that comet. line_14: ID no. 2483: Comet Shoemaker-Levy (1991a1) was successfully observed line_15: in July 1992. Unfortunately, the comet was not as bright as we had line_16: hoped, but we obtained data of comparable (slightly higher) quality line_17: to that already in hand from P/Hartley 2. We definitely detected line_18: the CO Cameron bands again, but it is much too early to say anything line_19: more at this time. line_21: ID no. 2442: Comet Shoemaker-Levy (1991a1) was successfully observed line_22: in July 1992, but it is too early to say anything more at this time. ! question: 9 section: 3 line_1: ID no. 3064: Inner Coma Imaging of Comet Levy (1990c) with the Hubble line_2: Space Telescope, H. A. Weaver, M. F. A'Hearn, P. D. Feldman, line_3: C. Arpigny, W. A. Baum, J. C. Brandt, R. M. Light and line_4: J. A. Westphal,Icarus}, v. 97, p. 85, 1992. line_6: ID no. 2481: Probing the Nature of Comets with HST, H. A. Weaver line_7: and P. D. Feldman, in "Science with the Hubble Space Telescope", line_8: ESA-NASA CP, in press. line_10: Presentations on both the above programs have been made at several line_11: scientific meetings, including the annual DPS meetings in 1990 line_12: (for 3064), 1991 (for 2481), and 1992 (2481 and 2483). A paper line_13: on our detection of CO Cameron band emission in P/Hartley 2 line_14: will be submitted to a refereed journal shortly. ! question: 10 section: 1 line_1: The STScI has excellent data-analysis capabilities and also maintains line_2: a pool of Science Data Analysts (SDAs) that are available to its staff. line_3: However, SDA support for our program can only be assured if we are line_4: allocated money to cover the SDA's salary. line_6: The other institutions co-sponsoring this program also have excellent line_7: data analysis facilities and access to graduate students and research line_8: assistants. However, funds must be provided by this program in order line_9: for the Co-Is to utilize these resources. ! !end of general form text general_form_address: lname: Weaver fname: Harold mi: A title: Dr. category: PI inst: 3470 addr_1: 3700 San Martin Drive city: Baltimore state: MD zip: 21218 country: USA phone: 410-516-8619 ! lname: Weaver fname: Harold mi: A. title: Dr. category: PI inst: STScI addr_1: 3700 San Martin Drive addr_2: Baltimore, MD 21218 addr_3: USA city: Baltimore state: MD zip: 21218 country: USA phone: 410-516-8619 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: 1993E descr_1: COMET SHOEMAKER-LEVY 1993E lev1_1: TYPE = COMET, lev1_2: Q = 5.0019435, E = 0.0460109, lev1_3: O = 336.38966, W = 313.31572, lev1_4: I = 1.76533, lev1_5: T = 24-JUN-1996:13:40:47, lev1_6: EQUINOX = J2000, lev1_7: EPOCH = 13-MAY-1993, ACQ = 0.25 comment_1: OPTIMUM OBSERVING TIME IS DURING comment_2: THE LAST WEEK IN MAY THROUGH THE comment_3: FIRST WEEK IN JUNE AND DURING THE comment_4: THE LAST WEEK IN JUNE THROUGH THE comment_5: FIRST WEEK IN JULY. OBS. WILL GO comment_6: IN SMS 93179 AND 93200, HOWEVER. comment_7: THE ELEMENTS ABOVE ARE FROM comment_8: NAKANO VIA MARSDEN ON 23 APRIL. fluxnum_1: 1 fluxval_1: SURF(V) = 13 +/- 1 fluxnum_2: 2 fluxval_2: SIZE = 1 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: IMAGE targname: 1993E config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 1 S priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=NO comment_1: A PC IMAGE IS OBTAINED ! linenum: 3.000 sequence_1: DEFINE sequence_2: GRATING targname: 1993E config: FOS/RD opmode: IMAGE aperture: 4.3 sp_element: G270H num_exp: # time_per_exp: 1 M s_to_n: 5 s_to_n_time: 1 H priority: 1 param_1: Y-SIZE = 5 param_2: Y-SPACE = 128 param_3: COMB = YES param_4: SUB-STEP = 4 comment_1: EXP TO SEARCH FOR OH EMISSION ! linenum: 5.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X100 req_1: SEQ 5-10 NO GAP; req_2: CRIT OBS / 5-16; req_3: CYCLE 2 / 5-16; req_4: REQ UPLINK; req_5: SEQ 5-7 NON-INT; comment_1: PC IMAGE OF COMET. ! linenum: 7.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X400 comment_1: PC IMAGE OF COMET. comment_2: ANALYSIS OF IMAGE WILL comment_3: BE USED TO FIX FOS comment_4: POINTING. ! linenum: 8.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X700 req_1: SEQ 8-9 NON-INT; comment_1: DEEP PC IMAGE OF COMET. comment_2: TWO LONG, EQUAL DURATION comment_3: EXPOSURES ARE REQUESTED IN comment_4: LINES 8 AND 9. comment_5: EXP TIMES SHOULD BE CHOSEN comment_6: TO FILL THE ORBIT. ! linenum: 9.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X700 comment_1: PC IMAGE OF COMET. ! linenum: 10.000 sequence_1: USE sequence_2: GRATING num_exp: 2 time_per_exp: X8 req_1: REQ UPLINK; comment_1: LONG FOS EXP. comment_2: EXP TIME SHOULD BE CHOSEN comment_3: TO FILL THE ORBIT. ! linenum: 11.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X400 req_1: SEQ 11-15 NO GAP; req_2: AFTER 5 BY 21D +/- 7D; req_3: REQ UPLINK; req_4: SEQ 11-13 NON-INT; comment_1: PC IMAGE OF COMET. comment_2: THIS IMAGE SHOULD BE TAKEN comment_3: ABOUT ONE MONTH AFTER THE comment_4: FIRST SET OF IMAGES. NOTE comment_5: THAT THE TARGET ENTERS THE comment_6: SEZ IN EARLY AUGUST 1993. ! linenum: 13.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X400 comment_1: PC IMAGE OF COMET. comment_2: ANALYSIS OF IMAGE WILL comment_3: BE USED TO FIX FOS comment_4: POINTING. ! linenum: 14.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X700 req_1: SEQ 14-15 NON-INT; comment_1: DEEP PC IMAGE OF COMET. comment_2: TWO LONG, EQUAL DURATION comment_3: EXPOSURES ARE REQUESTED IN comment_4: LINES 14 AND 15. comment_5: EXP TIMES SHOULD BE CHOSEN comment_6: TO FILL THE ORBIT. ! linenum: 15.000 sequence_1: USE sequence_2: IMAGE time_per_exp: X700 comment_1: PC IMAGE OF COMET. ! linenum: 16.000 sequence_1: USE sequence_2: GRATING num_exp: 2 time_per_exp: X8 req_1: REQ UPLINK; comment_1: LONG FOS EXP. comment_2: EXP TIME SHOULD BE CHOSEN comment_3: TO FILL THE ORBIT. ! ! end of exposure logsheet ! No scan data records found