! File: 2142C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:01:32:45 coverpage: title_1: RAM DEGRADATION/OTA THROUGHPUT MONITORING TEST proposal_for: SV/OLT pi_fname: OTTO pi_lname: RICHTER pi_inst: ST SCI pi_country: USA pi_phone: (301) 338-4809 hours_pri: 2.00 num_pri: 1 fos: Y hrs: Y realtime: Y ! end of coverpage abstract: line_1: During the normal course of HST operations, HST will line_2: experience the "Ram Effect" due to the residual line_3: earth's atmosphere present at the HST altitude. For this effect line_4: to occur, the HST velocity vector must be in the same direction line_5: as the HST pointing vector. At these times, the reflectivity of line_6: the primary mirror could change due to the ram effect on the MgF line_7: coating. Alterations in the performance would initially line_8: appear at short (UV, Lyman alpha) wavelengths and advance towards line_9: redder wavelengths with time. This OLT will line_10: periodically monitor the spectrum of a very hot star with a near line_11: featureless continuum in the UV for possible evidence of HST OTA line_12: degradation. Both HST spectrographs will be used starting as early line_13: as possible in the OV phase and extending throughout the SV phase. line_14: If there is spectroscopic evidence of HST OTA throughput degra- line_15: tion then further tests will be devised to determine its severity. line_16: Mission constraints also may be imposed on the pointing of the line_17: HST. Last two Revisions 8/88, 5/89. line_18: Revised 10/89 by PStanley to resolve SELECT conflicts. ! ! end of abstract general_form_proposers: lname: RICHTER fname: OTTO title: DR. mi: G. inst: ST SCI country: USA esa: Y ! lname: LUPIE fname: OLIVIA title: DR. mi: L. inst: ST SCI country: USA ! lname: EBBETS fname: D. title: DR. inst: BALL AEROSPACE country: USA ! lname: DOWNES fname: R. title: DR. inst: APPLIED RESEARCH CORP. country: USA ! lname: FASTIE fname: BILL title: PROF. inst: JHU country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Test Description: line_2: The primary mirror of the HST might suffer an unknown amount line_3: of degradation due to the residual atmosphere ram effect. Also, line_4: the OTA may become contaminated due to outgassing effects. The line_5: proposed observations are of a very hot star UV standard star. line_7: Both HST spectrographs will be used line_8: to minimize the chance that possible Science Instrument optical line_9: degradation in one of the two spectrographs could be mistaken line_10: for OTA degradation. Decreasing performance in the 1200 and line_11: 1800 Angstrom regions will indicate an increasing molecular line_12: contamination, whereas a gradual loss (10% or so) over the line_13: entire region of 1200 to 1500 Angstroms will suggest a thinning line_14: of the MgF quarter-wave overcoating. If a significant fraction line_15: of the primary surface becomes oxidized as a result of the loss line_16: of the MgF overcoating, then the deterioration in the 1200 to line_17: 1500 Angstrom region would be quite serious and proceed line_18: rapidly. ! question: 3 section: 1 line_1: Test Procedure: line_2: Initially, the onboard acquisition capabilities for the line_3: HRS and FOS may not have been tested. Therefore, the line_4: exposure lines include conditionals on the use of onboard line_5: sequences. As an alternative, interactive acquisition will be line_6: used in the case of the HRS, and because of the stellar brightness, line_7: a non-interactive step/dwell grid is the alternative for the FOS. line_9: - FOS WAVE calibration: FOS/BL, G160L, exp time 2S. line_10: - FOS Spectra - 2000A: FOS/BL, Aper 1.0, G160L, 1150-2300A. line_11: SPATIAL SCAN: Step/Dwell, 3.0x3.0", stepsize 0.5", exposure time line_12: 3S/dwell. No real time analysis required. The full stellar image line_13: will appear at least once in the 1.0 arcsec aperture. line_14: - FOS WAVE calibration: FOS/BL, G160L, exp time 2S. line_16: - FOS WAVE calibration: FOS/BL, G270H, exp time 2S. line_17: - FOS Spectra - 2900A: FOS/BL, Aper 1.0, G270H, 2230-3309A. line_18: SPATIAL SCAN: Step/Dwell, 3.0x3.0", stepsize 0.5", exposure time line_19: 12S/dwell. No real time analysis required. The full stellar line_20: image will appear at least once in the 1.0 arcsec aperture. line_21: - FOS WAVE calibration: FOS/BL, G270H, exp time 2S. ! question: 3 section: 2 line_1: - Offset to HRS 2.0 aperture. line_2: - HRS: Mode ACQ,INT/ACQ, MAP=DEF,Aper 2.0, line_3: MIRROR,SEARCH-SIZE=3,EXP TIME=(264*9+9)*0.2=477S. line_4: - HRS: Mode ACCUM, Aper 2.0, Spectral Element G140L. line_5: - 20S at 1100 A (S/N>100). line_6: - 10S at 1300A. line_7: - 15S at 1500A. line_8: - 25S at 1700A. line_10: NOTE: If onboard acquisitions operational, replace the HRS line_11: INT ACQ with the following sequences: line_12: HRS: ACQ, MIRROR, MAP=END-POINT, SEARCH-SIZE=3, line_13: EXP TIME= 55S. line_14: NOTE: If onboard acquisitions operational, replace the FOS line_15: step/dwell with the following sequences: line_16: FOS: phase 1- ACQ/PEAK, G570H, SEARCH-SIZE=6, STEP-SIZE=0.5, line_17: 1.0" aperture, TIME/STEP=0.2S line_18: phase 2- Repeat ACQ/PEAK, G570H, SEARCH SIZE=5, STEP-SIZE=0.2, line_19: 0.3" aperture, TIME/STEP=0.2S ! question: 4 section: 1 line_1: Submitted as an Observatory Level Test deemed high priority because line_2: of a potential impact on pointing restrictions. This test line_3: provides a baseline set of UV observations for OTA throughput line_4: monitoring. ! question: 5 section: 1 line_1: General Scheduling Requirements line_3: Because of the the changing environment during the early stages line_4: of the mission and the importance of characterizing throughput line_5: degradation which could be a function of pointing into the HST line_6: velocity vector, this test must be performed initially as early as line_7: possible (OVII) and repeated at 2-3 week intervals for 4 times. line_8: This test has been specifically designed to be an independent line_9: calibration in order to guarantee the data collection, to line_10: establish a baseline, and to minimize the impacts of re-planning line_11: activities during the early stages of SV. Any applicable data line_12: from other FOS and HRS activities will complement these observations. line_14: Both FOS and HRS measurements will be obtained to guarantee line_15: repeated early measurements with at least one SI in case of test line_16: failure or changing SI characteristics. The test will be repeated line_17: on 2-3 week centers for a total of four times. Note that the line_18: 3rd repeat only requests HRS observations because of the proximity line_19: to a similar FOS calibration, FOS 1320, Absolute Photometric line_20: Calibration during that period. ! question: 5 section: 2 line_1: In order to use the data from external FOS/HRS proposals, line_2: the targets should be the same, however, in order to preclude line_3: complicated replanning excercises, we have chosen to minimize line_4: the linkages between proposals and design *this* test to line_5: perform all activities necessary to generate a baseline sequence. ! question: 5 section: 3 line_1: - No observations performed during SAA passage line_2: - HRS and FOS Phase II aperture alignments completed at least line_3: ten days prior to the first execution of this OLT: line_4: HRS1396 and FOS1443. The dwell scan has been designed to line_5: accommodate target acquisition accuracies of about 1.5 arcsec. line_6: - Replace HRS interactive or FOS grid sequences with onboard line_7: target acquisitions only when the latter have been tested: line_8: HRS1352, 1353 and FOS2195. line_9: - Optical image quality at Level 1 (lambda / 20) line_11: - This OLT will use additional data from FOS1320, Absolute line_12: Photometric Calibration and HRS1354, Low Resolution Calibration line_13: for longer baseline coverage if the targets are the same. line_14: - No parallel observations with internal lamps which may line_15: introduce spurious scattered light. The early reps of line_16: this test will occur before interference checks. ! question: 7 section: 1 line_1: Real Time Data Analysis Requirements: line_2: - Real time Target Acquisition into the HRS - standard. ! question: 7 section: 2 line_1: Off Line Data Analysis Requirements: line_2: - Reduce the HRS and FOS spectra. line_3: - Compare each data set with subsequent data sets to line_4: look for changes in the throughput. line_5: - Compare results with predictions as a fuction of wavelength. ! question: 8 section: 1 line_1: Both the HRS and FOS will obtain data on the target in line_2: multiple executions of this test. This is to insure line_3: consistent target coverage by one of the two instruments in the line_4: even of subsequent test failure by on of the SIs. ! question: 9 section: 1 line_1: Results of this OLT will be documented in an ST ScI Technical line_2: Report with distribution to appropriate personnel. Portions of line_3: this test will be presented at the HST symposium following the line_4: SV mission phase. Test results may also be submitted for pub- line_5: lication in an appropriate technical journal. ! !end of general form text general_form_address: lname: RICHTER fname: OTTO mi: G. title: DR. inst: STSCI addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: 301-338-4809 from_date: 01-JAN-86 to_date: 01-JAN-95 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: BD+75D325 descr_1: SDO WHITE DWARF pos_1: RA=08H10M49.31S +/- 0.3S, pos_2: DEC=+74D57'57.5" +/- 0.5" equinox: 2000 comment_1: PRIME TARGET. comment_2: SAME TARGET IS USED IN THE comment_3: SV FOS-17 TEST AND HRS-08 TEST. fluxnum_1: 1 fluxval_1: V=9.54 +/- 0.02 fluxnum_2: 2 fluxval_2: B=9.27 +/- 0.02 fluxnum_3: 3 fluxval_3: F-CONT(1300)=7.9 +/- 0.3 E-11 fluxnum_4: 4 fluxval_4: F-CONT(1500)=4.5 +/- 0.3 E-11 fluxnum_5: 5 fluxval_5: F-CONT(2800)=7.1 +/- 0.3 E-12 fluxnum_6: 6 fluxval_6: F-CONT(1700)=3.2 +/- 0.3 E-11 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: HRSINT targname: # config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 477S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: MAP=ALL-POINTS req_1: INT ACQ FOR 2-5; req_2: DEC TIME 15M; ! linenum: 2.000 sequence_1: ^ sequence_2: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1100 num_exp: 1 time_per_exp: 20S s_to_n: 100 fluxnum_1: 3 priority: 1 req_1: SEQ 2-5 NO GAP ! linenum: 3.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1300 num_exp: ^ time_per_exp: 10S s_to_n: 100 fluxnum_1: 3 priority: 1 ! linenum: 4.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1500 num_exp: ^ time_per_exp: 15S s_to_n: 100 fluxnum_1: 4 priority: 1 ! linenum: 5.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1700 num_exp: ^ time_per_exp: 25S s_to_n: 100 fluxnum_1: 6 priority: 1 ! linenum: 5.500 sequence_1: DEFINE sequence_2: HRSOBS targname: # config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 55S fluxnum_1: 1 priority: 1 param_1: MAP=END-POINT, LOCATE=YES, param_2: SEARCH-SIZE=3, req_1: ONBOARD ACQ FOR 6-9; ! linenum: 6.000 sequence_1: DEFINE sequence_2: HRSOBS targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1100 num_exp: 1 time_per_exp: 20S s_to_n: 100 fluxnum_1: 3 priority: 1 req_1: SEQ 6-9 NO GAP; ! linenum: 7.000 sequence_1: DEFINE sequence_2: HRSOBS targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1300 num_exp: 1 time_per_exp: 10S s_to_n: 100 fluxnum_1: 3 priority: 1 ! linenum: 8.000 sequence_1: DEFINE sequence_2: HRSOBS targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1500 num_exp: 1 time_per_exp: 15S s_to_n: 100 fluxnum_1: 4 priority: 1 ! linenum: 9.000 sequence_1: DEFINE sequence_2: HRSOBS targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1700 num_exp: 1 time_per_exp: 25S s_to_n: 100 fluxnum_1: 6 priority: 1 ! linenum: 10.000 sequence_1: DEFINE sequence_2: FOSOBS targname: # config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G570H wavelength: 4582-5500 num_exp: 1 time_per_exp: 0.2S fluxnum_1: 3 priority: 1 param_1: SEARCH-SIZE=6, param_2: SCAN-STEP=0.5 req_1: ONBOARD ACQ FOR 11; ! linenum: 11.000 sequence_1: ^ sequence_2: ^ targname: # config: ^ opmode: ACQ/PEAK aperture: 0.3 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 0.3S fluxnum_1: 3 priority: 1 param_1: SEARCH-SIZE=5, param_2: SCAN-STEP=0.2 req_1: ONBOARD ACQ FOR 12-13 ! linenum: 12.000 sequence_1: ^ sequence_2: ^ targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2300 num_exp: 1 time_per_exp: 3S s_to_n: 150 fluxnum_1: 3 priority: 1 param_1: STEP-TIME=0.15 req_1: SEQ 12-15 NO GAP ! linenum: 13.000 sequence_1: DEFINE sequence_2: FOSOBS targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 12S s_to_n: 150 fluxnum_1: 5 priority: 1 ! linenum: 14.000 sequence_1: ^ sequence_2: ^ targname: WAVE config: ^ opmode: ^ aperture: 1.0 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 ! linenum: 15.000 sequence_1: ^ sequence_2: ^ targname: WAVE config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2300 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 ! linenum: 16.000 sequence_1: DEFINE sequence_2: FOSINT targname: WAVE config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2300 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 req_1: SEQ 16-21 NO GAP; ! linenum: 17.000 sequence_1: ^ sequence_2: ^ targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2300 num_exp: 1 time_per_exp: 3S s_to_n: 150 fluxnum_1: 3 priority: 1 req_1: SPATIAL SCAN req_2: SINGLE-EXP; comment_1: DWELL SCAN TO ACCOMMODATE comment_2: ALIGNMENT UNCERTAINTY: 3.0X3.0'', comment_3: STEPSIZE 0.5''. ! linenum: 18.000 sequence_1: ^ sequence_2: ^ targname: WAVE config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2300 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 ! linenum: 19.000 sequence_1: ^ sequence_2: ^ targname: WAVE config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 ! linenum: 20.000 sequence_1: ^ sequence_2: ^ targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 12S s_to_n: 150 fluxnum_1: 5 priority: 1 req_1: SPATIAL SCAN req_2: SINGLE-EXP; comment_1: DWELL SCAN TO ACCOMMODATE comment_2: ALIGNMENT UNCERTAINTY: 3.0X3.0'', comment_3: STEPSIZE 0.5''. ! linenum: 21.000 sequence_1: ^ sequence_2: ^ targname: WAVE config: ^ opmode: ^ aperture: 1.0 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 2S priority: 1 param_1: STEP-TIME=0.1 ! linenum: 40.000 sequence_1: USE sequence_2: FOSINT targname: BD+75D325 req_1: SEQ 40-41 NO GAP; req_2: CYCLE 0 / 40-43; ! linenum: 41.000 sequence_1: USE sequence_2: HRSINT targname: BD+75D325 ! linenum: 42.000 sequence_1: USE sequence_2: FOSOBS targname: BD+75D325 req_1: SEQ 42-43 NO GAP; req_2: AFTER 40 BY 20D +/- 6D; ! linenum: 43.000 sequence_1: USE sequence_2: HRSOBS targname: BD+75D325 ! linenum: 43.500 sequence_1: USE sequence_2: HRSOBS targname: BD+75D325 req_1: AFTER 42 BY 20D +/- 5D ! ! end of exposure logsheet scan_data: line_list: 17 fgs_scan: N cont_dwell: D dwell_pnts: 7 dwell_secs: 3.00 scan_width: 3.0000 scan_length: 3.0000 sides_angle: 90.0000 number_lines: 7 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.5000 wid_offset: 1.5000 ! line_list: 20 fgs_scan: N cont_dwell: D dwell_pnts: 7 dwell_secs: 12.00 scan_width: 3.0000 scan_length: 3.0000 sides_angle: 90.0000 number_lines: 7 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.5000 wid_offset: 1.5000 ! ! end of scan data