! File: 2544C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:07:53:20 coverpage: title_1: NIGHTTIME MEASUREMENTS OF NITRIC OXIDE sci_cat: SOLAR SYSTEM sci_subcat: INNER PLANETS proposal_for: GO pi_title: DR pi_fname: CASSANDRA pi_mi: G. pi_lname: FESEN pi_inst: DARTMOUTH COLLEGE pi_country: USA pi_phone: 603-646-2230 keywords_1: OCCULTATION, NITRIC OXIDE hours_pri: 0.53 num_pri: 6 hrs: Y funds_amount: 105371 funds_length: 12 funds_date: JAN-91 off_fname: JOHN off_mi: F. off_lname: KAVANAUGH off_title: DIRECTOR off_inst: DARTMOUTH COLLEGE off_addr_1: GRANTS AND CONTRACTS off_addr_2: BOX 7 off_city: HANOVER off_state: NH off_zip: 03755 off_country: USA off_phone: 603-646-3007 ! end of coverpage abstract: line_1: We propose to make the first nighttime measurements of nitric oxide (NO) in the line_2: earth's lower thermosphere and mesosphere. Nitric oxide is an important line_3: constituent of the earth's upper atmosphere but has been poorly observed. The line_4: GHRS on the HST provides an extremely simple and efficient way to measure UV line_5: absorption bands of NO using B and/or O target stars acquired by the GHRS for line_6: other GO/GTO investigations. Several minutes before the target is occulted by line_7: the earth, we request a change of grating to obtain NO altitude profiles. The line_8: only time requested for this project is the last few minutes before earth line_9: occultation, a period when the instrument would normally be idle. line_11: Atmospheric models have demonstrated that NO in the 80-120 km region is quite line_12: sensitive to vertical transport, especially at night. The transport is line_13: typically parametrized by the eddy diffusion coefficient which is poorly known. line_14: The unique HST measurements would test and refine our knowledge of the earth's line_15: upper atmospheric diffusion processes. ! ! end of abstract general_form_proposers: lname: BARTH fname: CHARLES title: PROF. mi: A inst: COLORADO, UNIVERSITY OF country: USA ! lname: ROBLE fname: RAYMOND title: DR. mi: G inst: NCAR country: USA ! lname: BRANDT fname: JOHN title: DR. mi: C inst: COLORADO, UNIVERSITY OF country: USA ! lname: FESEN fname: ROBERT title: DR. mi: A inst: DARTMOUTH COLLEGE country: USA ! lname: FESEN fname: CASSANDRA title: DR. mi: G. inst: DARTMOUTH COLLEGE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The HST GHRS will be used to make measurements of the line_2: absorption by the nitric oxide (1,0) delta band, roughly line_3: centered near 1829.41 A. The G200M grating will be line_4: used to provide spectral coverage of the wavelength region line_5: from approximately 1810 A to 1850 A. These measurements line_6: will be obtained by observing B and/or O stars as line_7: they are occulted by the dark limb of the earth. The large line_8: aperture grating will be used to maximize the ability to line_9: track and observe the star. Rapid readout mode is required. line_10: This project differs from most GO programs in that specific line_11: targets are NOT requested. Instead, we will use stars line_12: already acquired by other investigators in order to probe line_13: the earth's thermospheric nitric oxide concentration during line_14: the nighttime. Approximately 4 minutes before the target line_15: star passes behind the dark earth, we request that the GHRS line_16: instrument configuration be changed to that compatible with line_17: our project. The instrument field of view is expected to line_18: pass through the 75-200 km region in approximately 68 line_19: seconds. We will take 0.9-second integrations to provide line_20: 2-km altitude resolution. ! question: 3 section: 2 line_1: In detail, the proposed sequence for observations is: line_2: 1) select a target: B or O target stars brighter than 5th line_3: magnitude observed with the GHRS by an independent project; line_4: 2) observe the target as specified by the GO or GTO. If line_5: the occulting earth is in darkness, stop the observations line_6: when the stellar zenith angle is approximately 95 degrees; line_7: this is estimated to be about 3.2 minutes before occultation; line_8: 3) change the instrument configuration: grating, G200M; line_9: aperture, 2" x 2"; data mode, rapid readout; line_10: 4) at stellar zenith angle 101 degrees, begin observations; line_11: do 0.9 second integrations for 70 seconds. ! question: 4 section: 1 line_1: HST has the capability to make observations of nitric oxide line_2: that are unique. Nitric oxide (NO) is an important line_3: constituent of the earth's upper atmosphere but has never line_4: been measured at nighttime. Not only will the HST permit line_5: such measurements, but inferences on the local time line_6: variation of NO during the night could be made if line_7: observations of a fixed star were made during several line_8: orbits. These observations will also provide measurements line_9: of a region that has been poorly sampled in the past: the line_10: low-latitude atmosphere. line_11: Daytime observations of NO have been made for many years by line_12: rocket- and satellite-borne instruments. Satellite line_13: observations include those of the Atmosphere Explorer series line_14: (AE-C and AE-D) and the Solar Mesosphere Explorer. Emphasis line_15: was generally placed on the high-latitude regions where NO line_16: is more abundant and more variable. Satellite conditions line_17: were such that measurements were made at a fixed local time line_18: (e.g., 1500 LT for SME) or a restricted range of local times line_19: (e.g., 0600-1000 LT for AE-D). Our proposed HST line_20: observations provide a simple and straightforward way to line_21: extend this NO database from solely daytime measurements line_22: into the night. ! question: 5 section: 1 line_1: Ideally, this program would provide information on the line_2: solar cycle, seasonal, and diurnal dependence of NO. line_3: The observing time awarded in the present cycle precludes line_4: such a detailed study; the emphasis now is on demonstrating line_5: the viability of the technique. line_6: Again, observations of specific stars are not requested: line_7: we are "piggybacking" onto approved programs which observe line_8: B and/or O stars that are occulted by the dark earth. line_9: For each observation, we request approximately 17 minutes of line_10: spacecraft time and 70 seconds of exposure time. The 17 line_11: minutes of time is an estimate of instrument overhead needed line_12: to change the grating, aperture, and data acquisition modes. line_13: The 70-second exposure time is that required to obtain line_14: measurements from 200 to 75 km in 2-km intervals. Our line_15: exposure time is therefore inflexible. Our signal-to-noise line_16: ratio may then be increased by judicious averaging. The line_17: example calculations shown below indicate that the line_18: signal-to-noise ratios we anticipate given the constraints line_19: of the observations. ! question: 5 section: 2 line_1: flux at 1829 A for selected B and O stars: about 1E-9 line_2: G200M grating sensitivity at 1829 A : 1.5E12 for line_3: the large aperture (LSA) line_4: Count rate = CDS = flux x sensitivity x aperture transmission line_5: CDS is estimated to be about 1500 line_6: maximum signal-to-noise S/N is the square root of (CDS x line_7: ns x t) where ns is the number of pixels averaged together line_8: in the diode and t is the integration time. ns is line_9: greater than or equal to 1, while t is 0.9 seconds. Then line_10: the typical S/N is about 35. ! question: 6 section: 1 line_1: The proposed observations are to observe stellar occultations with the GHRS line_2: to study the earth's atmosphere. We will observe line_3: B stars that were targeted by two other GO's (#2403 and line_4: #2251). By utilizing targets already acquired and line_5: observed with GHRS, we eliminate much of the instrument line_6: overhead and slew time. By observing occulting stars, we line_7: utilize the instrument during periods when it would line_8: otherwise be idle. line_9: The acquisition and calibrations for our project requires about 17 line_10: minutes of time, plus 70 seconds for exposure time. line_11: We will require guidance in determining when to begin our line_12: observations. line_13: Five of the six targets we have specified in our exposure line_14: logsheet are being observed by 2 other GO's: the proposal line_15: id's are #2403 (2 of our targets) and #2251 (3 of our line_16: targets). These two investigations were rated as "High" line_17: priority investigations. line_18: We request that 3 or more exposures be taken of each of these targets line_19: as it is occulted. We assumed it would be most efficient line_20: if these exposures were taken on consecutive orbits. We line_21: therefore used an "AFTER" special requirement in the line_22: exposure logsheets with the time interval equal line_23: to the orbit time. ! question: 6 section: 2 line_1: We did not indicate a special requirement of "DARK TIME" line_2: on our logsheets, since we were not sure if that was line_3: a valid constraint on our observations. ! question: 7 section: 1 line_1: GHRS data will be reduced by the pipeline data reduction line_2: scheme. No extraordinary problems are anticipated in this line_3: phase. line_4: The occultation data will be analyzed using software line_5: developed by co-investigator R. Roble of NCAR for similar line_6: investigations which used the sun as the light source. line_7: Extension of the method to use different stellar sources is line_8: straightforward. line_9: The NO absorption band data will consist of measurements of line_10: intensity vs time. Spacecraft orbital information will be line_11: used to transform the data into intensities vs slant path line_12: height. The data will then be filtered and smoothed. The line_13: observed signal at 1829 A is due to NO and O2 bands. line_14: The O2 signal can be removed by using the observations near line_15: 1820 A and 1835 A where O2 alone absorbs to line_16: determine the O2 contribution and then subtract it from the line_17: signal. The residual intensity is related to the tangential line_18: column number density of the absorbing species, NO, through line_19: Beer's law. The equation relating intensity and number line_20: density is an Abel integral equation, for which various line_21: numerical schemes have been developed. The result is the line_22: number density of the absorbing species as a function of the line_23: tangent point. ! question: 7 section: 2 line_1: The nighttime number density profiles will be compared to line_2: NCAR thermospheric general circulation model which predicts line_3: the global NO densities in this atmospheric region. Numerical line_4: experiments are anticipated to determine the influence of line_5: various transport processes on the NO number densities, line_6: particularly vertical eddy diffusion. ! question: 8 section: 1 line_1: The targets required are early B or late O stars, line_2: with V less than 5, which are being observed for other line_3: investigators. line_4: If the project proves feasible, we will extend the observations line_11: to other features of interest, such as the 2150 A bands line_12: of NO and the 2800 A emission of Mg+, and the UV lines line_13: of chlorine, water vapor, ozone, etc. ! question: 9 section: 1 line_1: No ! question: 10 section: 1 line_1: The resources provided by Dartmouth include computer time line_2: and programming assistance for data reduction and analysis: line_3: software development, graphics, and post-processing will be line_4: carried out at the home institution. ! !end of general form text general_form_address: lname: FESEN fname: CASSANDRA mi: G. title: DR. category: PI inst: DARTMOUTH COLLEGE addr_1: THAYER SCHOOL OF ENGINEERING city: HANOVER state: NH zip: 03755 country: USA phone: 603-646-2230 ! ! end of general_form_address records fixed_targets: targnum: 101 name_1: HD36512 name_2: NU-ORI descr_1: STAR; TYPE=B0V; OCCULTATION pos_1: RA = 5H 31M 55.8S +/- 0.007", pos_2: DEC = -7D 18' 05" +/- 0.004" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 4.62, TYPE = B0V fluxnum_2: 2 fluxval_2: F(1830) = 1.62E-9 ! targnum: 102 name_1: HD91316 name_2: RHO-LEO descr_1: STAR; TYPE=B1IB; OCCULTATION pos_1: RA = 10H 32M 48.6S +/- 0.002", pos_2: DEC = +9D 18' 24" +/- 0.002" equinox: 2000 comment_1: THIS STAR IS TARGETED BY comment_2: GO 2251, SO IT SHOULD BE comment_3: SCHEDULED WITH THAT PROJECT. fluxnum_1: 1 fluxval_1: V = 3.85, TYPE = B1IB fluxnum_2: 2 fluxval_2: F(1830) = 1.39E-9 ! targnum: 103 name_1: HD212571 name_2: PI-AQR descr_1: STAR; TYPE=B1V; OCCULTATION pos_1: RA = 22H 25M 16.5S +/- 0.002", pos_2: DEC = +1D 22' 39" +/- 0.002" equinox: 2000 comment_1: THIS STAR IS TARGETED BY comment_2: GO 2251, SO IT SHOULD BE comment_3: SCHEDULED WITH THAT PROJECT. fluxnum_1: 1 fluxval_1: V = 4.6, TYPE = B1V ! targnum: 104 name_1: HD35149 name_2: 23-ORI descr_1: STAR; TYPE=B1V; OCCULTATION pos_1: RA = 5H 22M 49.9S +/- 0.009", pos_2: DEC = +03D 32' 40" +/- 0.007" equinox: 2000 comment_1: THIS STAR IS TARGETED BY comment_2: GO 2251, SO IT SHOULD BE comment_3: SCHEDULED WITH THAT PROJECT. fluxnum_1: 1 fluxval_1: V = 5.0, TYPE = B1V ! targnum: 105 name_1: HD116658 name_2: ALPHA-VIR descr_1: STAR; TYPE=B1III; OCCULTATION pos_1: RA = 13H 25M 11.5S +/- 0.002", pos_2: DEC = -11D 09' 41" +/- 0.002" equinox: 2000 comment_1: THIS STAR IS TARGETED BY comment_2: GO 2403 AND 2536, SO IT SHOULD comment_3: BE SCHEDULED WITH THAT PROJECT. fluxnum_1: 1 fluxval_1: V = 0.98, TYPE = B1III ! targnum: 106 name_1: HD33328 name_2: LAMBDA-ERI descr_1: STAR; TYPE=B2; OCCULTATION pos_1: RA = 5H 09M 8.7S +/- 0.003", pos_2: DEC = -08D 45' 15" +/- 0.003" equinox: 2000 comment_1: THIS STAR IS TARGETED BY comment_2: GO 2403 SO IT SHOULD BE comment_3: SCHEDULED WITH THAT PROJECT. fluxnum_1: 1 fluxval_1: V = 4.27, TYPE = B2IV ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD36512 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 10 req_1: ONBOARD ACQ FOR 2-4; comment_1: SCHEDULE ALL TARGETS AS THEY ARE comment_2: OCCULTED BY EARTH'S ATMOSPHERE. comment_3: 3 SEPARATE OCCULTATIONS REQUESTED IN comment_4: 2-4 ! linenum: 2.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 10 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 3.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 10 param_1: SAMPLE-TIME=0.9 req_1: AFTER 2 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 2 AND 4 ! linenum: 4.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 10 param_1: SAMPLE-TIME=0.9 req_1: AFTER 3 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 2-3 ! linenum: 5.000 targname: HD116658 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 6-10 comment_1: 5 SEPARATE OCCULTATIONS comment_2: REQUESTED IN 6-10 ! linenum: 6.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 7.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 6 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 6 AND 8-10 ! linenum: 8.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 7 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 6-7 AND 9-10 ! linenum: 9.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 8 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 6-8 AND 10 ! linenum: 10.000 targname: HD116658 config: HRS opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 9 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 6-9 ! linenum: 11.000 targname: HD91316 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 5 req_1: ONBOARD ACQ FOR 12-15 comment_1: 4 SEPARATE OCCULTATIONS comment_2: REQUESTED IN 12-15 ! linenum: 12.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 13.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 12 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 12 AND 14-15 ! linenum: 14.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 13 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 12-13 AND 15 ! linenum: 15.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 14 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 12-14 ! linenum: 16.000 targname: HD33328 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 17-21 comment_1: 5 SEPARATE OCCULTATIONS comment_2: REQUESTED IN 17-21 ! linenum: 17.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 18.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 17 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 17 AND 19-21 ! linenum: 19.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 18 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 17-18 AND 20-21 ! linenum: 20.000 targname: HD33328 config: HRS opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 19 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 15-19 AND 21 ! linenum: 21.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 1 param_1: SAMPLE-TIME=0.9 req_1: AFTER 20 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 17-20 ! linenum: 22.000 targname: HD212571 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 5 req_1: ONBOARD ACQ FOR 23-27 comment_1: 5 SEPARATE OCCULTATIONS comment_2: REQUESTED IN 23-27 ! linenum: 23.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 24.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 23 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 23 AND 25-27 ! linenum: 25.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 24 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 23-24 AND 26-27 ! linenum: 26.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 25 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 23-25 AND 27 ! linenum: 27.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 26 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 23-26 ! linenum: 28.000 targname: HD35149 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S s_to_n: 50 fluxnum_1: 1 priority: 5 req_1: ONBOARD ACQ FOR 29-33 comment_1: 5 SEPARATE OCCULTATIONS comment_2: REQUESTED IN 29-33 ! linenum: 29.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 comment_1: GYROHOLD ! linenum: 30.000 targname: HD35149 config: HRS opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 29 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 29 AND 31-33 ! linenum: 31.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 30 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 29-30 AND 32-33 ! linenum: 32.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 31 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 29-31 AND 33 ! linenum: 33.000 targname: ^ config: ^ opmode: RAPID aperture: 2.0 sp_element: G200M wavelength: 1829 num_exp: 1 time_per_exp: 70S s_to_n: 25 s_to_n_time: 0.9S fluxnum_1: 1 priority: 5 param_1: SAMPLE-TIME=0.9 req_1: AFTER 32 BY 96M comment_1: GYROHOLD comment_2: SCHEDULE ON A SEPARATE comment_3: OCCULTATION FROM 29-32 ! ! end of exposure logsheet ! No scan data records found