! File: 2435C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:06:25:28 coverpage: title_1: SPECTROPHOTOMETRY OF PHOBOS AND DEIMOS sci_cat: SOLAR SYSTEM sci_subcat: SATELLITES proposal_for: GO pi_title: DR. pi_fname: B. pi_lname: ZELLNER pi_inst: COMPUTER SCIENCES CORPORATION pi_country: USA pi_phone: 31-338-4729 keywords_1: PHOBOS, DEIMOS, PLANETARY SATELLITES, ASTEROIDS hours_pri: 1.00 num_pri: 3 fos: X pi_position: STAFF SCIENTIST off_fname: EDDYE off_mi: P. off_lname: GILL off_title: CONTRACTS ADMIN. off_inst: COMPUTER SCIENCES CORPORATION off_addr_1: 8728 COLESVILLE ROAD off_city: SILVER SPRING off_state: MD off_zip: 20910 off_country: USA off_phone: 301-650-3123 ! end of coverpage abstract: line_1: The satellites of Mars have been studied by the Mariner 9 and Viking missions, line_2: and will be minutely examined by the Phobos mission. The satellites are small, line_3: dark, and irregularly shaped, and are thought to resemble C-type mainbelt line_4: asteroids and some carbonaceous chondrites. Being the only such objects line_5: inspected by rendezvous spacecraft, they provide benchmarks for comparison of line_6: disk-integrated data with disk-resolved features, and thus are important in line_7: interpretation of astronomical data for many solar system objects. Also line_8: Phobos and Deimos have substantially different surface features, and promise line_9: substantial interpretive benefit by their variety. line_11: However groundbased observations that would allow direct comparisons with the line_12: asteroids are very difficult to obtain, and the connection with meteorites is line_13: uncertain because of limitations with reflectance data obtained from rendezvous line_14: spacecraft. Thus we propose spectrophometry of both satellites with HST. ! ! end of abstract general_form_proposers: lname: WELLS fname: EDDIE title: DR. mi: N. inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: THOMAS fname: P. title: DR. inst: CORNELL UNIVERSITY country: USA ! lname: VEVERKA fname: J. title: DR. inst: CORNELL UNIVERSITY country: USA ! lname: BELL fname: J. title: DR. inst: HAWAII, UNIVERSITY OF country: USA ! lname: THOLEN fname: DAVID title: DR. inst: HAWAII, UNIVERSITY OF country: USA ! lname: ZELLNER fname: B. title: P.I. inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: CALDWELL fname: JOHN title: DR. inst: YORK UNIVERSITY country: CANADA ! lname: GRADIE fname: JONATHAN title: DR. inst: HAWAII, UNIVERSITY OF country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: 2. Scientific Justification: line_3: The satellites of Mars are small, dark, and irregularly shaped, and line_4: are thought to resemble some carbonaceous chondrites and also C-type line_5: asteroids in the main asteroid belt. They have been studied closely line_6: by the Mariner 9 and Viking missions, and will be examined in minute line_7: detail by the remaining Soviet Phobos spacecraft. Thus they have the line_8: potential to provide vital benchmarks for understanding compositions line_9: and surface processes on small dark objects throughout the solar line_10: system. line_12: However the connections with carbonaceous chondrites and especially line_13: with mainbelt asteroids need to be put on a firmer basis. Only line_14: reflectance spectra from HST can provide the link between surface line_15: features observed by rendezvous spacecraft, disk-integrated properties line_16: observed for hundreds of asteroidal and cometary objects, and line_17: laboratory studies of meteorities. line_19: C-type asteroids are most common in the central and outer parts of the line_20: main belt and among the outer satellites of Jupiter. They are usually line_21: assumed to consist of primitive, carbon-bearing materials which line_22: accreted at low temperatures under wet, oxidizing conditions, and line_23: probably serve as source bodies for some of the carbonaceous ! question: 2 section: 2 line_1: chondrites that fall on the earth. It is surprising to find such line_2: compositions in the vicinity of Mars. The inner asteroid belt is line_3: characterized by the E and S types, which are thought to be line_4: higher-temperature condensates from dry, reducing environments, or line_5: products of igneous differentiation. line_7: However the connection between Martian satellites and C-type asteroids line_8: depends on little hard evidence. Groundbased physical observations of line_9: the Martian satellites are notoriously difficult (see below), and are line_10: limited to UBV colors of uncertain precision. The satellites are not line_11: as dark as most C asteroids, and no existing observations are adequate line_12: to distinguish among the spectroscopic sub-classes of the C type, or line_13: the superficially similar D and P types, which are well known in the line_14: main belt. line_16: Some rare igneous meteorites are now generally believed to have come line_17: from Mars, and it is even possible (though unproven) that we have line_18: samples of Phobos and Deimos in our meteorite collections. Relative line_19: UV reflectance spectra of Phobos were measured by the Viking line_20: spacecraft, and Pang et al. (1982) reported weak absorption bands at line_21: 2550, 2900, and 3300 A that matched bands in a laboratory spectrum of line_22: the C3V meteorite Allende. The apparent match with a C3V meteorite is line_23: puzzling, since the density of Phobos (1.9 gm/cm2) is much too low. ! question: 2 section: 3 line_1: Is it possible that surface processes have altered C1 or C2 material line_2: to C3 material, and if so, does the same process happen among mainbelt line_3: asteroids? line_5: A rendezvous spacecraft is myopic, however, and is not necessarily the line_6: best way to do precision reflectance spectrophotometry in the line_7: ultraviolet. The Viking data were spectrally sparse, mostly made at line_8: large phase angles with attendant problems of phase reddening, and not line_9: directly comparable with any observations of asteroids. If the line_10: remaining Phobos spacecraft is successful, it will approach one line_11: satellite closely and measure the elemental and perhaps the line_12: mineralogical composition of its surface. However it has minimal line_13: capabilities for measuring spectral reflectivity in visible light, and line_14: none shortward of 3000A. line_16: Also, Phobos and Deimos exhibit strikingly different surface features. line_17: Phobos is rough, is crisscrossed with grooves, and has only minor line_18: albedo features. Deimos is smooth, has no grooves, and has dramatic line_19: albedo features in material moving downslope. Thus any similarity or line_20: difference in their spectra may have great significance in the line_21: interpretation of spectra of asteroids and comets. line_23: Thus we propose spectrophotometric observations of both satellites of ! question: 2 section: 4 line_1: Mars with HST, during the late-1990 opposition of Mars. The FOS can line_2: cover the entire wavelength range of interest, including the region of line_3: the "Pang" bands, in a single exposure for each object. The exposures line_4: are driven by the need for adequate photon count in the ultraviolet, line_5: and the visible portion of the spectrum comes essentially "free". line_6: Both hemispheres of each objects should be observed. line_8: Comparisons with other objects are an important part of this program, line_9: and we will use techniques and calibration observations identical to line_10: those proposed in a much larger program by Chapman et al. for line_11: observations of mainbelt asteroids, outer satellites of Jupiter, and line_12: inactive comets. The results will be interpreted (1) by direct line_13: comparison with the similar HST observations of other small line_14: solar-system bodies by Chapman et al., and (2) with reference to a line_15: large body of available laboratory reflectance spectrophotometry of line_16: primitive meteorites, lunar materials, and artificial and terrestrial line_17: materials. line_19: Thus we will be able to relate the Martian satellites closely to other line_20: solar system bodies, and to meteorites that fall on the earth, in ways line_21: that will not be possible even via the Phobos mission. ! question: 3 section: 1 line_1: 3. Provide a short description of the proposed observations. line_3: We propose to do two FOS exposures for each satellite, one for each line_4: hemisphere, and a sky background exposure for each target exposure. line_5: The sky background is expected to be quite small, and its measurement line_6: may be omitted based on OV/SV experience. We also propose one line_7: exposure of a G2V standard star for calibration to the solar spectrum line_8: (see below). All exposures would use the FOS in the Spectrophotometry line_9: (ACCUM) mode with the Red Digicon and prism and the 1 arcsecond line_10: aperture. With exposure times of 300 and 600 seconds for Phobos and line_11: Deimos, we can achieve a SNR of 10 over the spectral range of line_12: 2200-7500 Angstroms and at least 30 over the 2500-7500 A range. line_13: Multiple readout/clears of the data during the exposures will be line_14: required to permit accumulation of sufficient UV photons without line_15: saturating the long-wavelength signal. line_17: Long-wavelength light scattering in the FOS will be tested in orbit in line_18: OV/SV Proposal 1343, for which Caldwell is the PI. If on-orbit line_19: testing should indicate that scattered light will corrupt observations line_20: with the Red Digicon and prism below 2500 A, we would use instead the line_21: Blue Digicon, with a loss of spectral coverage longward of 5200A. ! question: 4 section: 1 line_1: 4. Justify the need for the capabilities of HST. line_3: Scattered light from Mars causes groundbased physical observations of line_4: Phobos and Deimos to be notoriously difficult. Photoelectric results line_5: in visible light have been obtained only by Kuiper in 1956 and Zellner line_6: in 1973, yielding only UBV colors and magnitudes of low precision. line_7: Attempts by Zellner et al. during subsequent apparitions using line_8: fixed-aperture techniques with the eight-color photometric system in line_9: the visible and near-IR have all failed to yield consistent results. line_11: During the 1988 apparition Co-Investigators Bell, Gradie, and Tholen line_12: are attempting 8-color visible spectrophotometry with a CCD detectors line_13: at Mauna Kea. At this writing it appears they may have succeeded, in line_14: which case HST spectrophotometry in the vacuum ultraviolet will become line_15: all the more valuable. The proposed HST observations in visible light line_16: will then provide a vital link between FOS spectrophotometry of line_17: asteroids and faint comets as proposed by Chapman et al., and the line_18: groundbased 8-color system in which nearly 600 asteroids have been line_19: observed. line_21: The satellites of Mars are too faint for observations with IUE, for line_22: which the limit is around visual magnitude 10 for objects seen by line_23: reflected sunlight. ! question: 5 section: 1 line_1: 5. Justify the amount of exposure time and estimated spacecraft time line_2: requested. line_4: We have requested 0.6 hours of exposure time (including the sky line_5: background exposures) and 1.5 hours of spacecraft time. There are two line_6: exposures on Phobos (300 seconds each), two sky background exposures line_7: for Phobos (60 seconds each), two exposures on Deimos (600 seconds line_8: each), two sky background exposures for Deimos (120 seconds each), and line_9: a 20-second exposure of an 8th-magnitude standard star. line_11: To estimate the flux from Phobos, the XCAL simulator at STScI was used line_12: to calculate the flux from an 11.3 mag. G2V star using data from line_13: Bruzual's atlas. Since Phobos has an albedo that decreases in the UV, line_14: a correction was applied to the stellar flux. A laboratory line_15: reflectance spectrum for a sample of the Allende meteorite was used to line_16: correct the stellar flux. line_18: Exposure times were calculated using materials from the FOS Handbook line_19: and from the July 1988 issue of the STScI Newsletter. The line_20: calculations were made for a SNR of 30 at the shortest wavelength line_21: absorption band reported by Pang et al. (2550 A), and a SNR greater line_22: than 10 for the shortest wavelength to be measured (2200 A). ! question: 5 section: 2 line_1: Deimos is 0.7 magnitude fainter than Phobos, and required exposure line_2: times are 1.9 times longer at all wavelengths. Several candidate G2V line_3: standard stars are known with V magnitudes of around 8, for which an line_4: exposure time of about 20 seconds will be sufficient. line_6: In calculating the requested spacecraft time we have assumed that the line_7: exposure sequence of satellite, sky background, second satellite, and line_8: it sky background can be counted as one visit; they can use one set of line_9: guide stars and one target acquisition. With a total exposure time of line_10: 36 minutes, 9 exposures with 1 minute overheads, and 2 satellite line_11: visits and 1 standard star visit with 15 minute overheads, the total line_12: spacecraft time would be 1.5 hours. We expect it can all be done in 3 line_13: orbits of HST. ! question: 6 section: 1 line_1: 6. Justify any special scheduling requests and any requests for line_2: special calibrations. line_4: The opposition of Mars will occur in late November 1990. To avoid line_5: complications of phase reddening in the interpretations, both line_6: satellites should be observed at solar phase angles not exceeding 15 line_7: degrees, or roughly between Nov. 10 and Dec. 15 1990. line_9: In order to observe different hemispheres of the synchronously line_10: rotating satellites, they should each be observed near east and west line_11: elongations. ! question: 7 section: 1 line_1: 7. Describe plans for data reduction and analysis. line_3: The amount of data and the expected data-reduction effort for this line_4: work are small. The output spectra only have to be co-added and the line_5: sky background subtracted in order to get uncalibrated spectra. line_7: Obtaining an instrumental solar spectrum for calculation of the line_8: spectral reflectance is another matter. The expected spectral line_9: features are weak and shallow, and the FOS with prism gives resolution line_10: varying sharply with wavelength. We expect that the standard line_11: HST-supplied calibration will be adequate only for a first-order line_12: analysis. We propose instead to rely primarily on calibration via FOS line_13: observations of solar-type stars proposed under the program line_14: "Observations of Asteroids, Inactive Comet Nuclei, and Distant line_15: Satellites of Planets" by C. Chapman et al. Solar-type stars differ line_16: in the details of their UV spectra, and several should be observed. line_17: Since the observations of Martian satellites will necessarily come line_18: early in the GO phase of HST operations, however, we have proposed line_19: here one observation of a solar-type star. line_21: Consultation among the Investigators will be needed for interpretation line_22: and publication of the results, and travel funds are budgeted line_23: appropriately. ! question: 8 section: 1 line_1: 8. Additional comments or requests. line_3: Though it is not necessary for our scientific purposes, the satellites line_4: could be observed in succession when both are on the same side of the line_5: planet. The relative positions of the satellites are predictable with line_6: high precision, and only one Mode II target acquisition plus an offset line_7: of <30 arcseconds to the other target should be necessary per line_8: elongation. Mode II acquisitions of planetary satellites will be line_9: explicitly tested in the Science Verification phases of HST, in line_10: proposals for which Co-Investigator Caldwell is Principal line_11: Investigator. line_13: We expect that target acquisition, observation of both satellites, and line_14: both observations of the sky brightness can all be done in one HST line_15: orbit. Such a scenario is currently being used to test the SCS and line_16: SPSS elements of the HST ground system, and its feasibility will be line_17: verified prior to Phase II. ! !end of general form text general_form_address: lname: ZELLNER fname: B. title: DR. category: PI inst: COMPUTER SCIENCES CORPORATION addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA ! ! end of general_form_address records fixed_targets: targnum: 5 name_1: BD+16D601-CALIB name_2: HYA VB64 name_3: SAO93936 descr_1: STAR;SOLAR ANALOG;TYPE=G0 pos_1: RA= 4H 23M 47.654S +/- 0.013S, pos_2: DEC= +16D 38' 7.34" +/- 0.2" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: 0.007100 ra_pm_unct: 0.000467 dec_pm_val: -0.0230 dec_pm_unct: 0.0090 comment_1: SOLAR-TYPE STAR FOR CALIBRATION comment_2: OF SPECTRAL REFLECTANCE OF comment_3: SATELLITES OF MARS. fluxnum_1: 1 fluxval_1: V=8.073 +/- 0.004, TYPE=G0 fluxnum_2: 2 fluxval_2: B-V=0.674 ! ! end of fixed targets solar_system_targets: targnum: 1 name_1: PHOBOS-E descr_1: SATELLITE PHOBOS lev1_1: STD=MARS lev2_1: STD=PHOBOS wind_1: SEP OF EARTH SUN FROM MARS LT 18D, wind_2: SEP OF PHOBOS MARS FROM EARTH GT 10", wind_3: OLG OF PHOBOS FROM EARTH BETWEEN 45 135 comment_1: PHOBOS NEAR EAST ELONGATION, comment_2: SOLAR PHASE ANGLE LESS THAN comment_3: PLUS OR MINUS 18 DEG. comment_4: SATELLITE AT LEAST 10 ARCSEC FROM comment_5: MARS LIMB. FLUXNUM_2 IS FOR SKY, comment_6: BRIGHTNESS IS JUST A GUESS. fluxnum_1: 1 fluxval_1: V=11.6 fluxnum_2: 2 fluxval_2: V=14.2 ! targnum: 2 name_1: PHOBOS-W descr_1: SATELLITE PHOBOS lev1_1: STD=MARS lev2_1: STD=PHOBOS wind_1: SEP OF EARTH SUN FROM MARS LT 18D, wind_2: SEP OF PHOBOS MARS FROM EARTH GT 10", wind_3: OLG OF PHOBOS FROM EARTH BETWEEN wind_4: 225 315 comment_1: PHOBOS NEAR WEST ELONGATION, comment_2: SOLAR PHASE ANGLE LESS THAN comment_3: PLUS OR MINUS 18 DEG. comment_4: SATELLITE AT LEAST 10 ARCSEC comment_5: FROM MARS LIMB. fluxnum_1: 1 fluxval_1: V=11.6 fluxnum_2: 2 fluxval_2: V=14.2 ! targnum: 3 name_1: DEIMOS-E descr_1: SATELLITE DEIMOS lev1_1: STD=MARS lev2_1: STD=DEIMOS wind_1: SEP OF EARTH SUN FROM MARS LT 18 D, wind_2: SEP OF DEIMOS MARS FROM EARTH GT 20", wind_3: OLG OF DEIMOS FROM EARTH BETWEEN 45 135 comment_1: DEIMOS NEAR EAST ELONGATION, comment_2: SOLAR PHASE ANGLE LESS THAN comment_3: PLUS OR MINUS 18 DEG. comment_4: SATELLITE AT LEAST 20 ARCSEC comment_5: FROM MARS LIMB. FLUXNUM_2 IS comment_6: FOR SKY, BRIGHTNESS IS JUST A comment_7: GUESS. fluxnum_1: 1 fluxval_1: V=12.7 fluxnum_2: 2 fluxval_2: V=16.0 ! targnum: 4 name_1: DEIMOS-W descr_1: SATELLITE DEIMOS lev1_1: STD=MARS lev2_1: STD=DEIMOS wind_1: SEP OF EARTH SUN FROM MARS LT 18D, wind_2: SEP OF DEIMOS MARS FROM EARTH GT 20", wind_3: OLG OF DEIMOS FROM EARTH BETWEEN wind_4: 225 315 comment_1: DEIMOS NEAR WEST ELONGATION, comment_2: SOLAR PHASE ANGLE LESS THAN comment_3: PLUS OR MINUS 18 DEG. comment_4: SATELLITE AT LEAST 20 ARCSEC comment_5: FROM MARS LIMB. fluxnum_1: 1 fluxval_1: V=12.7 fluxnum_2: 2 fluxval_2: V=16.0 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PHOBOS-E config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.20 S fluxnum_1: 1 priority: 1 param_1: BRIGHT=330000, param_2: FAINT=3300 req_1: ONBOARD ACQ FOR 2-4 comment_1: MODE II ACQUISITION OF PHOBOS comment_2: EAST OF MARS. ! linenum: 2.000 targname: PHOBOS-E config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 30 S fluxnum_1: 2 priority: 1 req_1: SEQ 2-4 NON-INT; req_2: POS TARG 0.7, 0.7 comment_1: FIRST SKY MEAS FOR PHOBOS-E. comment_2: DELTA-X = 0.7 ARCSEC AND comment_3: DELTA-Y = 0.7 ARCSEC FROM comment_4: CURRENT POSITION OF PHOBOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 3.000 targname: PHOBOS-E config: FOS/BL opmode: RAPID aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 518 S s_to_n: 7.0 s_to_n_time: 130 S fluxnum_1: 1 priority: 1 comment_1: MEASUREMENT OF PHOBOS comment_2: NEAR EASTERN ELONGATION. ! linenum: 4.000 targname: PHOBOS-E config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 30 S fluxnum_1: 2 priority: 1 req_1: POS TARG -0.7, -0.7 comment_1: SECOND SKY MEAS FOR PHOBOS-E. comment_2: DELTA-X = -0.7 ARCSEC AND comment_3: DELTA-Y = -0.7 ARCSEC FROM comment_4: CURRENT POSITION OF PHOBOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 5.000 targname: PHOBOS-W config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.20 S fluxnum_1: 1 priority: 3 param_1: BRIGHT=330000, param_2: FAINT=3300 req_1: ONBOARD ACQ FOR 6-8 comment_1: MODE II ACQUISION OF PHOBOS comment_2: NEAR WESTERN ELONGATION. ! linenum: 6.000 targname: PHOBOS-W config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 30 S fluxnum_1: 2 priority: 3 req_1: SEQ 6-8 NON-INT; req_2: POS TARG +0.7, +0.7 comment_1: FIRST SKY MEAS FOR PHOBOS-W. comment_2: DELTA-X = +0.7 ARCSEC AND comment_3: DELTA-Y = +0.7 ARCSEC FROM comment_4: CURRENT POSITION OF PHOBOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 7.000 targname: PHOBOS-W config: FOS/BL opmode: RAPID aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 518 S s_to_n: 7.0 s_to_n_time: 130 S fluxnum_1: 1 priority: 3 comment_1: MEASUREMENT OF PHOBOS comment_2: NEAR WEST ELONGATION. ! linenum: 8.000 targname: PHOBOS-W config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 30 S fluxnum_1: 2 priority: 3 req_1: POS TARG -0.7, -0.7 comment_1: SECOND SKY MEAS FOR PHOBOS-W. comment_2: DELTA-X = -0.7 ARCSEC AND comment_3: DELTA-Y = -0.7 ARCSEC FROM comment_4: CURRENT POSITION OF PHOBOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 9.000 targname: DEIMOS-E config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.30 S fluxnum_1: 1 priority: 2 param_1: BRIGHT=330000, param_2: FAINT=3300 req_1: ONBOARD ACQ FOR 10-12 comment_1: MODE II ACQUISITION OF comment_2: DEIMOS EAST OF MARS. ! linenum: 10.000 targname: DEIMOS-E config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 80 S fluxnum_1: 2 priority: 2 req_1: SEQ 10-12 NON-INT; req_2: POS TARG +0.7, +0.7 comment_1: FIRST SKY MEAS FOR DEIMOS-E. comment_2: DELTA-X = +0.7 ARCSEC AND comment_3: DELTA-Y = +0.7 ARCSEC FROM comment_4: CURRENT POSITION OF DEIMOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 11.000 targname: DEIMOS-E config: FOS/BL opmode: RAPID aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 1426 S s_to_n: 7.0 s_to_n_time: 356 S fluxnum_1: 1 priority: 2 comment_1: MEASUREMENT OF DEIMOS comment_2: NEAR EASTERN ELONGATION. ! linenum: 12.000 targname: DEIMOS-E config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 80 S fluxnum_1: 2 priority: 2 req_1: POS TARG -0.7, -0.7 comment_1: SECOND SKY MEAS FOR DEIMOS-E. comment_2: DELTA-X = -0.7 ARCSEC AND comment_3: DELTA-Y = -0.7 ARCSEC FROM comment_4: CURRENT POSITION OF DEIMOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 13.000 targname: DEIMOS-W config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.30 S fluxnum_1: 1 priority: 4 param_1: BRIGHT=330000, param_2: FAINT=3300 req_1: ONBOARD ACQ FOR 14-16 comment_1: MODE II ACQUISITION FOR comment_2: DEIMOS WEST OF MARS. ! linenum: 14.000 targname: DEIMOS-W config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 80 S fluxnum_1: 2 priority: 4 req_1: SEQ 14-16 NON-INT; req_2: POS TARG +0.7, +0.7 comment_1: FIRST SKY MEAS FOR DEIMOS-W. comment_2: DELTA-X = +0.7 ARCSEC AND comment_3: DELTA-Y = +0.7 ARCSEC FROM comment_4: CURRENT POSITION OF DEIMOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 15.000 targname: DEIMOS-W config: FOS/BL opmode: RAPID aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 1426 S s_to_n: 7.0 s_to_n_time: 356 S fluxnum_1: 1 priority: 4 comment_1: MEASUREMENT OF DEIMOS comment_2: WEST OF MARS. ! linenum: 16.000 targname: DEIMOS-W config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 80 S fluxnum_1: 2 priority: 4 req_1: POS TARG -0.7, -0.7 comment_1: SECOND SKY MEAS FOR DEIMOS-W. comment_2: DELTA-X = -0.7 ARCSEC AND comment_3: DELTA-Y = -0.7 ARCSEC FROM comment_4: CURRENT POSITION OF DEIMOS. comment_5: SATELLITE NOT IN APERTURE. comment_6: CONTINUE TRACKING SATELLITE. ! linenum: 17.000 targname: BD+16D601-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 5 param_1: SCAN-STEP=0.7 param_2: SEARCH-SIZE=4 req_1: ONBOARD ACQ FOR 18 comment_1: SOLAR-TYPE STAR FOR CALIBRATION comment_2: OF SATELLITES OF MARS; MODE II comment_3: ACQUISITION. ! linenum: 18.000 targname: BD+16D601-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 5 param_1: SCAN-STEP=0.2 param_2: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 19 comment_1: SOLAR-TYPE STAR FOR CALIBRATION comment_2: OF SATELLITES OF MARS; MODE II comment_3: ACQUISITION. ! linenum: 19.000 targname: BD+16D601-CALIB config: FOS/BL opmode: RAPID aperture: 0.5 sp_element: PRISM wavelength: 1850-5500 num_exp: 1 time_per_exp: 54 S s_to_n: 20 s_to_n_time: 7.5 S fluxnum_1: 1 priority: 5 param_1: READ-TIME=4.0 req_1: CALIB FOR 3,7,11,15 comment_1: SOLAR-TYPE STAR FOR CALIBRATION comment_2: OF SATELLITES OF MARS. ! ! end of exposure logsheet ! No scan data records found