_h_ D/-_/°
Hubble Space Telescope High Speed Photometer Orbital Verification Test Report
Space Science and Engineering Center and Space Astronomy Laboratory University of Wisconsin Madison, WI
November 1991
(NASA-CR-189333) HUBBLE SPACE N94-24226 TELESCOPE HIGH SPEED PHOTOMETER _P3ITAL VERIFICATION Test Report (Wisconsin Univ.) iO0 p Unclas
G3/18 0204210
HSP OV Report(VI.0)
1. Purpose of HSP OV FinalReport...... 4 2. Executive Summary ...... 4 3. HSP Performance ...... 4 3.1 Thermal ...... 4 3.2 Power ...... 5 3.3 Electrical and Mechanical ...... 5 3.4 Depressurization ...... 6 3.5 Flight Software ...... 6 3.6 Detectors ...... 6 3.7 Alignments ...... 7 3.8 Magnetic Shielding and effects ...... 7 3.9 Sensitivity to SAA ...... 7 3.10 Contamination ...... 7 3.11 Throughput ...... 7 3.12 Sensitivity to bright objects ...... 7 3.13 Primary Mirror Spherical Aberration ...... 8 3.14 Jitter ...... 8 4. Program Development, Execution, and Results ...... 8 4.1 Program Development ...... 8 4.2 OV Events in Chronological Order...... 9 4.3 Test Specific Performance ...... l0 Launch Configuration ...... 10 HSP-iA - Off to Safe - OVIS seq l0 ...... 10 2201 - Part 1 - Safe to Hold ° Part 1 ...... 10 2201 - Part 2 - Safe to Hold - Part 1I - 901241K3 ...... 10 1499 - Command Response - 901252K1 ...... 11 2113 - Memory Dump - 901252K1 ...... 11 1500 - Detector Data Test - 901271M1R ...... 11 1502 - Part 1 - HV Turn On - part 1 - 901352M2 ...... 11 1502 - Part 2 - HV Turn-on - 901413M5 ...... 12 1502 - Part 3 - HV Turn-on - 901452M8 ...... 12 1379 - Part 1 - Dark Count - 901562P4 ...... 12 1379 - Part 2 - Dark Count - 901613A3 ...... 13 1502PMT-1 - PMT Special Test - Part 1 - 901773B3 ...... 13 1502PMT-2 - PMT Special Test - Part 2 - 901823A3 ...... 13 1502PMT-3 - PMT Special Test - Part 3 - 901844A9 ...... 14 1380 - Aperture Map - 901974A3 ...... 14 1502A - PMT - PMT HV Turn On - 902165B5 ...... 14 1379 - PMT - PMT Dark Count - 902314A4 ...... 14 1380 - UV1 - Aperture Map - 902384A6 ...... 14 1380 - UV2 - Aperture Map - 902494A6 ...... 15 1503 - U-V1 - Phase 1I Alignment - 902537AB ...... 15 1503 - UV2 - Phase II Alignment - 902607D2 ...... 16 1382 - UV1/2 - PAD Threshold Test - 902817B8 ...... 18 1504 - UV1 - Phase HI Alignment - 902957A9 ...... 18 1526 - UV1/2 - Aperture Map - SV - 903027AC ...... 19 3069 - 10.2 Test - 903104A4 ...... •.... 19 1503 - UV1/2 II - FGS/HSP Coarse Alignment - 910217BD ...... 19 3140 - Phase III Alignment - (partial)- 910427D6 ...... 19 3093 - Aperture Map - Det 1 & 3 - 910707C6 ...... 19 3152 - Phase IV Align - Det 4 - 910707C6 ...... 19 3152 - Phase IV Align - Det 2 - 910707C6 ...... 20 3072 - Target Acquisition UV1 - 910917BC ...... 20 3073 - Target Acquisition UV2 - 910917BC ...... 20 2948 - FGS/I-ISP Fine Alignment UV2 - 910987C9 ...... 20 2949 - FGS/I-ISP Fine Alignment UV1 - 910987C9 ...... 20 3152 - Fine Alignment VIS & POL - 911057D5 ...... 20 3007-UV2 - Jitter (SAO) - 911197B8 ...... 20 HSP OV Report (V1.0)
3074 - Mode II Target Acq - VIS - 911276A2R ...... 21 3071 - Mode II Target Acq - POL - 911276A2R ...... 21 3233 - Fine Alignment - UV - 911337C8 ...... 21 3233 - POL - Fine Alignment - POL - 911547D3 ...... 21 1385 - Photometric Performance - 911547D3 ...... 22 3233 - VIS - Fine Alignment - VIS - 911547D3 ...... 22 4.4 Database Updates ...... 22 4.5 OV Anomalies ...... 23 4.6 End of OV Status and Liens ...... 27 5. Modifications and Recommendations ...... 27 5.1 Trend Monitoring Recommendations ...... 27 5.2 Instrument Operational Recommendations ...... 27 5.3 Conclusions & Lessons Learned ...... 27 Appendix A - HSP OV, SV, & GTO proposal numbers and names ...... 29 Appendix B - PMT High Voltage Turn-On Investigation ...... 31 Appendix C - PMT Bright Object Safmg Report ...... 34 Appendix D - HST Flight SMS sequence ...... 37 Appendix E - HSP Filter and Aperture Diagrams ...... 38 Appendix F - OV Timelines ...... 44 HSPOVReport(VI.0)
1. Purnose of HSP OV Final Renort
The purpose of this report is to provide a summary of the results of the HSP Orbital Verification (OV) tests and to report conclusions and lessons learned from the initial operations of the HSP. The HSP OV plan covered the activities through fine (phase III) alignment. This report covers all activities (OV, SV, and SAt) from launch to the completion of phase III alignment. Those activities in this period that are not OV tests are described to the extent that they relate to OV activities.
_, Executive Summary
All HSP systems were verified and performed as designed. Difficulties encountered during OV were not the fault of the hardware, software, or design, but were the result of incomplete understanding of the orbital environment (the brightness of the bright earth, for example), test design errors (the PMT high voltage turn-on test, for example), incomplete information about other HST systems (the alignment of the FGS, for example), the effects of spherical aberration (the inability of the original HSP fine alignment test to obtain the required information, for example), or ground system problems (inability to capture and verify HSP memory, for example). At the end of OV the HSP is fully capable of supporting the planned SV, SAt, and OLT programs. Most SV activities as well as several OV tests had to be redesigned to accommodate the effects of spherical aberration.
3. HSP Performance
HSP performance throughout OV has been nominal. There have been no failures of any hardware or software and the HSP continues to operate in the original pre-launch configuration; there have been no redundant unit reconfigurations. There have been two soft single event upsets affecting engineering telemetry later cleared by a system controller "reboot". There have been two cases of bright object protection limits being exceeded and the HSP sating as a result. Thermal performance, power consumption, and general operation have been as expected.
3.1 Thermal
The major requirements for the HSP thermal control system were to maintain detectors as cool and stable as possible, to keep the electronics temperatures within design limits, and to meet the HST interface temperature requirements that were generally imposed on HSP external surfaces near other HST structures. Selected areas of the HSP were required to be maintained between -20 and + 20 degrees Celsius. These interfaces were required to be maintained while the HSP is operating and while in the "hold" mode. Hold mode power was limited to 58 watts orbital average which, given the cold orbit effective sink temperatures, required careful balancing of the thermal design. While the design had to meet the worst case combination of interface requirements, it was recognized that the actual environment in orbit might prove to be much more benign than the interface documents implied because of the conservatism inherent in the interface definition. Therefore, the HSP thermal design provided for the possibility of taking advantage of operational experience.
The general approach was a passive thermal design radiating heat from the electronics and detectors to external radiators. Because the detectors were to be maintained as cool as possible, they are thermally isolated from the higher power dissipation electronics. The detectors and electronics are thermally coupled to their own radiator surfaces, which are isolated from each other. The forward and aft bulkhead interface surfaces required to be kept within ICD limits are equipped with heaters. One problem faced early in the design was that of controlling power supplied to the heaters while the input bus voltage varies between interface limits of 24 to 32 volts. The HSP heater control application processor in the NSSC-1 monitors the input bus voltage and controls the power applied to the heaters. The heaters can be set for a specified power level and can be controlled to any of 20 power levels in sequence providing for a 20 point "warm up" curve. The heaters also can be controlled in a thermostat mode in response to a specified telemetry temperature monitor. The specific monitor, turn on temperature, and turn off temperature can all be
4 HSP OV Report(V1.0)
changed on command. The capability also exists to inhibit heater switching during specified times. All parameters in the heater control processor can be loaded from the ground.
The flexibility built into the design of the HSP thermal control system has already been used several times. The original pre-launch HSP hold mode used the heater control application processor to apply a constant orbital average power to the forward and aft bulkhead to maintain the interface temperature above -20 degrees Celsius with all other electronics off. In that case, when the HSP made hold to operate mode transitions, the electronics were subjected to large temperature changes. A year or so before launch, a "new hold" mode was defined that kept the common electronics on to maintain HSP temperatures but left all heaters off. Thermal model predictions suggested that in worse case cold orbit conditions, some limited areas of the HSP aft bulkhead might reach -25 degrees Celsius. The change was never formally adopted in the interface control documents because agreement could not be obtained from all parties, but was nevertheless adopted by the Space Telescope Science Institute into the standard operating procedures. It was felt that the increased reliability from the lessened thermal transitions outweighed the potential problems due to out of limit interface temperatures. Several months after launch, the HSP "new hold" mode was put into operation and has proven to be very successful. Temperature changes between hold and operate are now small and because the aft shroud thermal environment is warmer than worst case predictions, interface temperatures only rarely drop below -20 degrees Celsius and then only during unusual circumstances, such as vehicle sat'rag events. The only hitch was that for several weeks in the fall of 1990 just after the "new hold" mode was put into effect, both the old and new hold modes were actually running. The heaters were on and being controlled to the old hold values while the system controller was also on. There was no danger or urgency to correct the error on an emergency basis so the correction was simply incorporated into the SMS pipeline and took effect about two months later. The new hold has proven to be a stable and effective mode with no known disadvantages. Power consumption in the new hold mode is 46.3 watts. The old hold mode power consumption is 58.0 watts.
Spacecraft power may become more critical as solar arrays degrade or for other reasons. HSP detector temperature may later prove to be critical for some kinds of observations. The HSP thermal control system, unlike systems based on conventional thermostatically controlled heaters, can adapt to new conditions as they occur. For example, if information developed later in the mission suggests the need to control detector or bulkhead temperatures, the heater control processor can be operated in the "software thermostat" mode to control the area of interest to the desired temperature, subject to available power. A test of that capability was requested several times but not approved. Since this thermal control method has many advantages over conventional techniques, many of which have already been exploited to the advantage of the HST mission, it seems short sighted not to demonstrate the remaining capabilities, even briefly. Orbital verification of the HSP thermal control system has been satisfactory to the extent that it has been done, but it has not exercised more than a limited portion of its capabilities.
3.2 Power
HSP power consumption has been as predicted throughout the OV/SV period to date. The present "new hold" mode consumes less power (46.3 W) than the fixed power "old hold" mode (58.0 W). Because there are no hardware thermostats, HSP power consumption is predictable and is not a function of aft shroud temperature.
3.3 Electrical and Mechanical
Contrary to prelaunch expectations, analysis of the aperture mapping tests (1380, 3093, and 1526) suggests that there is no discernible "banana" effect, i.e., a distortion of the optical bench caused by thermally- induced forces. Motions of the apertures are not temperature dependent as far as can be determined, indicating that the structure is more stable than expected. Also, the stable thermal environment contributes to HSP mechanical stability.
There have been no electrical problems. The HSP continues to operate on the primary (prelaunch) set of redundant electronics, including the RIUs. There have been no electrical reconfigurations. HSP OV Report (V1.0)
There is, however, a known EMI problem which may or may not require additional work. The reply bus driver is in the RIU. The level of conducted emissions was far in excess of specified limits during pre- launch RIU electromagnetic interference (EMI) testing. The out-of-limit condition was resolved by the project office by increasing the allowed limit rather than by pursuing a technical solution. There has been some indication that reply bus noise can be found in certain detector data. Later SV tests are expected to determine if the reply bus noise is a significant problem or not. The reply bus can be turned off if needed during critical observations. A test of this scheme was written (SV 2749) and submitted but stiU awaits implementation; so the required commanding has not been incorporated into SOGS.
The RIU reply bus emissions appear to be readily correctable by incorporating an internal shield in the reply bus transformer. Such a correction should be investigated before this RIU is used in another spacecraft.
3.4 Depressurization
The HSP has no pressure gauge. There was no evidence of any significant partial pressure in the HSP when the high voltage was turned on. The dark count was nominal and there was no sign of noise caused by arcing or corona.
3.5 Flight Software
Flight software has operated as expected with no anomalies and no revisions. Especially noteworthy was that the flight software calculated correctly the magnitude and direction of the small angle maneuver required for target acquisition. No corrections or modifications were required. As indicated above, the heater control application processor has been only partially exercised.
3.6 Detectors
All five detectors have operated satisfactorily. There have been three detector operational problems that have been resolved and were not the fault of the detectors themselves.
The PMT signal during the high voltage turn-on test increased in a manner suggesting an approaching bright object. This was originally though to be the bright earth, but later was shown to be a characteristic of turning on the high voltage well below the nominal operating voltage of the corotron, a gas discharge regulator used to drop the high voltage power supply voltage down to the level required by the PMT. When the PMT was turned on with a higher voltage on the corotron (1900 volts, rather than 1500 volts), closer to but still somewhat below the nominal corotron operating voltage, performance was normal. There has been no recurrence of any anomalous output since the PMT was confined to the higher turn-on voltage. See Appendix B for additional details of the investigation of this problem.
The fu'st attempt to perform the PMT dark count test ended with a bright object saf'mg when the bright earth came into view of the PMT. Later analysis shows that the PMT is safe to operate with the bright earth as a target. The bright earth protection limits have been relaxed to allow such operation.
Similarly, the first attempt to perform aperture mapping on the VIS detector ended in a bright object safing when the read beam intersected the finding aperture during a mapping with the bright earth (which occasionally is about 50 times brighter than had been expected) in view. It was later determined that some filters on both the VIS and POL tubes should not be used with the bright earth since they may cause too large a current to be drawn from those detectors. Calibrations are now performed on selected filters with the Orion nebula instead of the bright earth.
In all three cases mentioned above, the problems were the result of incorrect operating procedures. The sating mechanisms worked. Changes were made in the operating procedures and there have been no additional problems with the detectors. HSPOVReport(V1.0)
OVtestinghasalsoshown that the order of the filter strips on the POL detector were reversed from that shown on the drawings. The same drawings define the orientations of the polarizing sunups, which have not been verified yet in the OV or SV program, but will be in later SV tests.
3.7 Alignments
Alignment of the HSP apertures to the HST focal plane, FGS-to-SI alignment, was a major difficulty until the FGS alignment matrices were determined to the required accuracy. Initial attempts to perform the phase II alignment (1503) produced data from the two UV detectors that were not consistent. The phase 11I alignments at first failed (in January and February 1990) completely because the target could not be placed in the desired aperture. In fact, the FGS to SI alignment was not known well enough to place a target reliably in the HSP's ten arc second diameter finding apertures. It was therefore decided to stop further alignment testing in October 1990 until FGS/SI alignment problems were better understood and resolved. Testing was resumed in March 1991 when improved FGS/SI alignment matrices along with the results of a redesigned HSP fine alignment test produced high quality data. The redesigned HSP fine alignment test did not assume that the target could be placed in the aperture with high accuracy and therefore was much more robust and forgiving than the original test. The aperture positions of the image dissector tubes (except the POL tube) are now known to within 0.02 arc seconds, which is better accuracy than was anticipated before Lunch.
The degraded image also contributed to the difficulty of determining accurate alignment. The model used to specify aperture position now uses 13 parameters. Had the HST star images been as predicted, a model with 6 parameters would have sufficed. The two factors, poor FGS to SI alignments and degraded images, both contributed to the delay in determining alignments.
3.8 Magnetic Shielding and effects
The HSP detectors have double magnetic shielding. HSP instrument level acceptance tests verified the detectors would be insensitive to the effects of the earth's magnetic field or HST ICD level fields. There have been no specific OV tests performed to verify magnetic field sensitivity but no evidence has been found to date of any measurable sensitivity.
3.9 Sensitivity to SAA
Tests have been proposed to measure HSP sensitivity to the SAA but none have been approved or scheduled. Most HSP data have been collected outside the SAA.
3.10 Contamination
There is no evidence to date in the OV test data of any contamination effects. The SV program is designed to quantify throughput and will be more likely to detect the presence of contamination, if any.
3.11 Throughput
The SV program, rather than the OV program, is intended to more precisely quantify HSP throughput. However, the targets observed to date in the OV test program verify that the HSP throughput is generally as expected except for a few (two or three) filters, F551W for example, where the data are not consistent with pre-launch predictions.
3.12 Sensitivity to bright objects
The HSP instrument safmgs during VIS tube aperture mapping and PMT dark count tests were caused by the bright earth triggering the HSP bright object protection application processor. The standard operating procedures and the 10.2 reconfiguration software were modified to allow operation of the HSP without unintended safing events because of bright earth limb occultations. The PMT bright object limits are relaxed during warm-up and data-taking and the VIS/POL tube's sensitive filters are not used with the bright earth. HSPOVReport(VI.0)
3.13 Primary Mirror Spherical Aberration
An HST image would have had 70% of its encircled energy within a 0.2 arc second diameter if the telescope mirror specifications had been met. This would have meant over 90% encircled energy within a 1.0 arc second aperture. The degraded image caused by spherical aberration has only about 50 to 70% energy in a 1.0 arc second aperture and about 20% in a 0.4 arc second aperture. The design goal of 0.3 to 3.0% throughput in the 1.0 arc second apertures has been reduced by a factor of two to three. The reduction is about a factor of four or five in the 0.4 arc second apertures. Because of the loss of signal the 0.4 arc second apertures are no longer acceptable for photometry. Test plans have been modified to increase required observation times in the one arc second apertures and remove the 0.4 arc second apertures from the planned program.
Had the telescope's performance been within specification it would have been possible to do accurate photometry in crowded fields. The broad point spread function makes this impossible for separations less than 2.5 arc seconds.
3.14 Jitter
Because the image is larger, more of the energy is spread out to the edges of the 1.0 arc second apertures making photometric performance much more sensitive to centering and jitter. The design goal for long term (weeks to months) photometric stability was 0.1%. It is expected that centering errors will introduce 1 to 2% errors in long term photometric stability. The short term (seconds to weeks) photometric stability design goal was 0.001 to 0.01%. Assuming nominal jitter performance, errors of 0.01 to 0.1% at 0.1 to 0.6 Hz may be introduced.
4. Program Development. Execution. and Results
4.1 Program Development
The HSP OV program was an extension of the ground test program beginning at the sub-box level and extending though VAP, A&V at LMSC, and the various GSTs at LMSC and KSC. The orbital verification program was designed to activate and verify the HSP in a methodical, step-by-step manner, minimizing risk but also conserving operations timeline. The OV program was based on the overall HST OV program in that the test pre-requisites were intended to be consistent with the state of verification of the other ST elements upon which the operation of HSP depends. All essential functions were included but no redundant units were activated or verified. Tests were deliberately made as similar as possible to previously run ground tests to take advantage of experience in both test design and the ground database.
Some tests were changed during OV in response to experience, the degraded HST image, and to correct problems in test design. The prelaunch planning tended to be success oriented and overly optimistic about HST capabilities upon which the test objectives depended. Experience has shown the wisdom of planning tests in small, incremental steps with provisions incorporated to get the desired results even if the assumed HST performance is less than nominal. A major example is the HSP fine alignment test. The test (1504) design assumed that the FGS to SI alignment would be known to a fraction of an arc second when the test was performed but in fact, a target could not be reliably placed within the HSP 10 arc second finding aperture. Because the HSP detectors had such large finding apertures, thought to be adequate to allow for any conceivable HST pointing errors or uncerlainties, no spiral scan routine was provided in HSP's target acquisition flight software. The impact on the HSP OV program of the FGS alignment problems were, therefore, significant. HSPOVReport(VI.0)
4.20V Events in Chronological Order
Launch (liftoff) of HST occurred on April 24, 1990 at 12:32:52 UT
The major events in the OV period are listed below:
Test number Test Name SMS Date
Launch 4/24/90 HSP-iA Off to Safe (first power to HSP - HSP in safemode) n/a 4/24/90 2201 - Part 1 Safe to Hold - part 1 (heater control AP started) n/a 4/24/90 2201 - Part 2 Safe to Hold - part 2 (log dump executed) 901241K3 5/4/90 1499 Command Response 901252K1 5/5/90 2113 Memory Dump 901252K1 5/6/90 1500 Detector Data Test (trailing logs lost by SDF cutoff) 901271M1R 5/8/90 1502 - Part 1 HV Turn On - Part 1 901352M2 5/15/90 1502 - Part 2 HV Turn On - Part 2 (PMT data anomalous) 901413M5 5/22/90 1502 - Part 3 HV Turn On - Part 3 901452M8 5/25/90 1379 - Part 1 Dark Count (UV1 & VIS) 901562P4 6/5/90 1379 - Part 2 Dark Count (UV2 & POL) 901613A3 6/11/90 1502PMT- 1 PMT Special Test - part 1 901773B3 6/27/90 1502PMT-2 PMT Special Test - part 2 901823A3 7/2/90 1502PMT-3 PMT Special Test - part 3 901844A9 7/4/90 1380 Aperture Map (I-ISP bright object saving by VIS) 901974A3 7/17/90 1502A - PMT PMT I-IV Turn On 902165B5 8/6/90 1379 - PMT PMT Dark Count (HSP bright object sating by POL) 902314A4 8/19/90 1380 - UV1 Aperture Map UV 1 902384A6 8/26/90 1380 - UV2 Aperture Map UV2 902494A6 9/7/90 1503 - UV1 Phase II Alignment UV 1 902537AB 9/13/90 1503 - UV2 Phase II Alignment UV2 902607D2 9/22/90 1382 - UV1/2 PAD Threshold Test UV1 & UV2 902817B8 10/2/90 1504 - UV1 Phase III Alignment (target not placed in 1.0" aperture) 902957A9 10/22/90 1526 - UV1/2 Aperture Map- SV CtJV1 & UV2) 903027AC 10/29/90 3069 10.2 Test (VIS, POL, & PMT) 903104A4 1118/90 1503 - UV1/2 II Phase II Alignment (UV1 & UV2, repeats) 910217BD 1/21/91 3140 Phase IlI Alignment - partial (failure: target not acquired) 910427D6 2/11/91 3093 Aperture Map - VIS and POL 910707C6 3/11/91 3152 Phase IV Align - UV2 (first revised alignmen0 910707C6 3/11/91 3152 Phase IV Align - UV 1 910707C6 3/15/91 3072 *Target Acquisition UV 1 910917BC 4/1/91 3073 *Target Acquisition UV2 910917BC 411/91 2948 *FGS/HSP Fine Alignment UV2 (old scheme) 910987C9 4/10/91 2949 *FGS/I-ISP Fine Alignment UV1 (old scheme) 910987C9 4/10/91 3152 Fine Alignment VIS & POL 911057D5 4/21/91 3007 -UV2 **Jitter (SAO) (data timing problem) 911197B8 5/9/91 3074 *Mode II Target Acq - VIS 911276A2R 5/9/91 3071 *Mode II Target Acq - VIS 911276A2R 5/9/91 3233 *Fine Alignment - UV 911337C8 5/18/91 3233 - POL Fine Alignment - POL 911547D3 6/3/91 1385 *Photometric Performance 911547D3 6/5/91 3233 - VIS Fine Alignment - VIS 911547D3 6/8/91 * SV Test ** SAO Test HSPOVReport(V1.0)
4.3 Test Specific Performance
Orbital verification began with the initial application of power to the HSP, proceeded through verification of the various functions of the HSP, and ended with phase III alignment.
Launch Configuration
The HSP launch configuration is: all power off and all redundant units configured to the A side.
HSP-iA - Off to Safe - OVlS seq 10
The initial application of power and transition HSP to the safe mode occurs soon after deployment and is performed by real time commanding from the ground. All relays are commanded to the launch configuration, power bus relays are closed, HSP primary power is turned on, and one forward and one aft heater is turned on. This leaves the HSP preregulator and two heaters on and everything else off.
The first HSP operation in orbit was the transition from the prelaunch configuration with all power off to the thermal safe mode. The HSP safe mode requires the primary power relay on, and two bulkhead heater circuits on, one on the forward and one on the aft bulkhead. The commands were sent by PSTOL procedures from the MOR at GSFC. Engineering telemetry verified the commands were received and the HSP was in the correct configuration. Temperatures during the period remained within expected limits.
2201 - Part 1 - Safe to Hold - Part 1
The HSP was reconfigured from thermal safemode to hold mode. In hold mode, the HSP bulkhead heaters are controlled by the NSSC-1 heater control application processor. The heaters can be controlled in several ways: a selected state can be maintained, a specific temperature range can be selected (the "software thermostat" mode), or a power level can be chosen for each heater. In the constant power mode, a series of power levels can be arranged in sequence to provide a desired "warm up" transition. In OV, only the constant power mode was exercised. The heater control application processor performed as designed and the resulting HSP temperatures were as expected. The initial heater control configuration involved cycling all three bulkhead heaters. This was later changed to a single heater to reduce relay cycles.
Still later in OV, use of the heater control application processor was discontinued when the "new hold" mode was put into use. In the "new hold" mode, the heaters are not used but the HSP system controller is turned on to provide thermal input to maintain interface temperatures. The "new hold" mode has several advantages: the thermal transients between hold and operate modes are greatly reduced, thereby increasing the HSP optical path stability. Power consumption is less than in the hold mode. Because thermal cycling is reduced, greater reliability is expected because thermally induced slyesses are less.
2201 - Part 2 - Safe to Hold - Part II - 901241K3
The second part of the safe to hold transition was the dump of the HSP Standard Header Packet and Unique Log (SHP & UDL). The dumps were successfully executed by PSTOL procedures sent from the MOR and the data were transmitted to the ground. The procedures worked as designed even with an unplanned hold in mid-procedure ordered by the Mission Operations Manager to restore order in the MOR. But, because the ground system design did not provide for this type of data (logs dumped by themselves with no associated science data), the data were inaccessible and never reviewed. No fix was ever made for this problem because logs without a "normal" data collection is not a normal operation and is not ever expected to be repeated.
10 HSPOVReport(V1.0)
1499 . Command Response - 901252K1
In the HSP command response test, all commands are exercised except those involved in HSP reconfiguration with redundant subsystems. The test is divided into six sections separated by two hours to avoid confusion in interpretation of results. The six sections are: One each for each of the five detector's serial commands, and one for serial commands not specific to any particular detector. The engineering telemetry was examined to verify that the commands were received and properly executed. The test was completed and all responses were nominal. All commands were verified to be functioning properly.
2113 - Memory Dump - 901252K1
In this test the HSP system controller RAM was dumped four times. The HSP would have liked to have the resulting data delivered in a manner similar to normal science data, but, the ground system is not presently capable of delivering HSP memory dump data. The ground system was designed to compare the memory dump with a ground master image and report the number of miscompares. The number of reported miscompares was about twelve thousand because the ground master image did not consider the memory locations that are subject to change. To evaluate the memory dump properly the data must be available for review. In the current system, the data go to a trouble file from which they are extremely difficult to retrieve. A paper listing of the data was eventually provided for our analysis. This enabled us to determine that the memory dump contained the expected values, but review of voluminous paper listings is extremely error prone.
Recently (June 1991) there was a telecon with HSP and ST ScI personnel to agree on a reasonable procedure for dumping the HSP memory, including the bus director memory (which was not dumped by the 2113 procedure), and making it available in standard FITS file format, similar to normal science data. The new procedure would be useful in analyzing future instances of single event upsets and other possible anomalies. Without it, reviewing HSP memory is difficult and extremely error prone.
1500 . Detector Data Test - 901271M1R
This test exercises the data collection capability of each detector electronics using simulated science data having a constant value depending on the integration time selected. Verification consists of checking the resulting science data to make sure the data values are as predicted and that all the data were received. This test uses the spacecraft clock as a simulated data input to store a predictable number of counts, determined by the integration time chosen, into the science data words. The data are sent to the ground system and if the values are all as expected, the data path from the HSP to the ground is verified. The test was executed and the science data were as expected. The standard practice for lISP data collections is to dump both the Standard Header Packet (SLIP) and the Unique Data Log (UDL) before and after the data collection. However, some SlIP and UDL data were missing from the data received on the ground. It was later determined that the missing SI-IP and UDL were the result of an error in the time calculated in the SMS for the science data path to the tape recorder to be enabled. The time calculation algorithm was subsequently corrected and, since then, no SI-IP and UDL data have been lost.
1502 - Part 1 - HV Turn On - part 1 - 901352M2
This test is designed to turn on high voltage to each detector in a careful, step-by-step manner to minimize the chance of damaging the detectors because of arcing or corona discharge. The pressure in the HSP is intended to be less than 10-5 tort before high voltage is tamed on. This test was therefore scheduled to begin no earlier than day 22 of the mission and would hay been postponed if ST aft shroud pressure data indicated the pressure was significantly higher than desired. The test consists of a 192 second data collection during which the high voltage power supply is commanded on. The test is performed in segments separated by at least 24 hours as follows:
1. Turn on detector 1 HV to the lowest program value.
11 HSPOVReport (V1.0)
2. Detector 1 HV at 0.5x105 gain setting, detectors 2-5 at lowest program value.
3. Detector 1 HV at 106 gain setting, detectors 2-5 at 0.5x105.
4. Detector 1 HV at 2x106 gain setting, detectors 2-5 at 106.
5. Detectors 2-5 at 2x106 gain setting.
The data from each segment, consisting of the 192 seconds of science data from each detector (192 words because the integration (sample) time is one second) is examined for evidence of noise due to corona or arcing. If the data indicates there is no problem, a command is sent from the ground to change the state of a flag on board and the next segment is performed as scheduled. If the command is not sent, the HSP is automatically put in the safemode.
The design of the HSP prevents damage from most operations, but turning on high voltage is one of the few where damage is possible. If the voltage level is set too high or if there is incomplete venting of the instrument, arcing or corona is possible. The first turn-on of the high voltage power supplies was therefore planned to be done in a careful step-by-step manner allowing time to retreat before damage could be done if problems were encountered. The first pall of the high voltage turn on involved only one detector, detector one, the POL tube. The high voltage power supply was turned on for 38 seconds at its lowest setting, approximately 1500 volts, during a science data collection. The data collection was started before the high voltage was turned on and continued after it was turned off so that the transients could be seen in the data. There was no evidence of any problems in the first part of the test.
1502 - Part 2 - HV Turn-on - 901413M5
The intent of the second part of the high voltage turn-on test was to repeat the first part for the high voltage power supply exercised in the first part, but at a higher level (the lowest of the three nominal gain settings for the detector) and to perform the first part of the test on the remaining four high voltage power supplies. There were no problems discovered in the operation of the high voltage power supplies, but the test design was faulty because the high voltage level cannot be changed during a data collection. Therefore, the test did execute to completion as planned. The test was later modified to be performed at nominal high voltage gain but in steps of increased analog output sensitivity.
A second problem occurred in this part of the high voltage turn-on test. The PMT output appeared to represent a signal of increasing brightness that was first thought to be the approaching bright earth limb.
1502 - Part 3 - HV Turn-on - 901452M8
The results from the third part of this test were identical with the first two parts except that some stray light was detected. The anomalous PMT response was the same as in part two. A series of special tests were planned to further explore the PMT response.
1379 - Part 1 - Dark Count - 901562P4
This test was intended to provide the In'st baseline dark count data from all five detectors. The tests consist of collecting data for five minutes at each of three cathode locations with high voltage on and one cathode location with high voltage off (to verify electronic noise level) on all four image dissector tubes. Five minutes of PMT data are collected with high voltage on and five minutes with high voltage off.
Verification consists of analyzing the data to determine the level and frequency characteristics of the noise. The integration time used for this test is 0.1 second, which will facilitate detection of RIU reply bus noise interference if it exists.
12 HSPOVReport(VI.O)
Inthisfirst part, detector two and three (UV-1 and VIS) were tested. The test executed as planned and data were satisfactory.
The VIS tube dark counts were:
Location Counts/see Dark 1 0.238 Dark 2 0.295 Dark 3 0.198
The UV-1 dark counts were:
Dark 1 0.090 Dark 2 0.100 Dark 3 0.137
Electronic noise ("dark count" with high voltage off) in both detectors were zero.
1379 - Part 2 - Dark Count - 901613A3
Detectors one and four (POL and UV-2) were tested in part two of the dark count test. The results were as expected and dark counts were satisfactory.
The UV-2 results were:
Ix)cation Counts/see Dark 1 0.264 Dark2 0.218 Dark 3 0.231
The POL results were:
Dark 1 0.224 Dark 2 0.174 Dark 3 0.167
Electronic noise in both detectors were zero.
1502PMT-1 - PMT Special Test - Part 1 - 901773B3
This special test was designed to replicate the PMT high voltage turn on test but with shorter integration time and with the "all" format to collect analog data (at a gain of 1000nA full scale) as well as pulse counting data. These changes were intended to make the test more likely to be sensitive to subtle noise characteristics not detectable with longer integration times and using only pulse counting data. The results were similar to the original high voltage turn-on test and no new insights were gained except that the characteristic output was clearly repeatable and apparently not due to partial pressure in the aft shroud.
1502PMT-2 - PMT Special Test - Part 2 - 901823A3
This second part of the PMT special test was a repeat of the f'n-st except that a higher analog gain, 100nA full scale, was used in an attempt to gain insights into the characteristics of the anomalous signal. The results were nearly identical with those in Part 1.
13 HSPOVReport(V1.0)
1502PMT-3- PMT Special Test - Part 3 - 901844A9
The third part of this test was a repeat of part two but at still higher analog gain, 10nA full scale. Again, the results were similar to the earlier data At this point it was concluded that the characteristic behavior was repeatable and possibly caused by the fact that the PMT and corotron and were operating far below their nominal operating voltage. A subsequent test at higher operating voltage confh'med operation is normal at higher voltages.
1380 - Aperture Map - 901974A3
This test was designed to map all apertures of all four image dissector tubes (about 200 total) using the bright earth as a "flat" field. The filter strips are scanned using the HSP Map mode with a 12 x 80 raster using 0.4 arc second steps. Selected apertures are then mapped using a 20 x 20 scan using 0.1 arc second steps. The test began with the VIS detector but when the clear (no filter) finding aperture came into view of the VIS (detector three) read beam, the bright object application processor sensed a value in excess of the limits and triggered an HSP safmg. The application processor operated as planned and turned off all HSP high voltage. The bright object application processor limits were set too low to accommodate the actual bright earth that is occasionally much brighter than we had anticipated. The aperture mapping tests were redesigned to use the Orion Nebula as the "flat field" for the particular filters on the VIS and POL detectors that allow excessive throughput with the bright earth. The bright earth was used for the remaining filters.
The sating occurred after most of the VIS f'dters had been mapped. The test succeeded in getting useful information about VIS aperture positions from the 12 x 80 filter strip scans. The 20 x 20 scans of individual apertures were less successful, however, because the apertures had moved significantly in deflection space from their pre-launch values, as anticipated. The aperture mapping test was revised to increase the size of the individual aperture scans to 30 x 32 and the filter strip scans to 16 x 60.
1502A - PMT - PMT HV Turn On - 902165B5
This is the revised PMT turn-on test incorporating the turn-on at 1900 volts. The test ran satisfactorily but the science data went to the trouble fde because the 1900 volts used in this test is not one of the standard operating voltages incorporated into the data base. The data were extracted manually and were satisfactory. No corrective action was taken because data are not normally taken at 1900 volts.
1379 - PMT - PMT Dark Count - 902314A4
A problem was encountered in the dark count test of the PMT. The PMT high voltage is turned on before the observation to allow time for the detector noise to settle down after the turn-on transient. During the time before the dark count observation was to begin, the bright earth occulted the dark target. The bright object protection application processor sensed an analog output higher than the limit and safed the HSP high voltage. The operation of the bright object application processor was as intended. The limit was exceeded because the bright earth was occasionally much brighter than expected. The eventual corrective action for this problem was to allow the PMT to view the bright earth with the bright object limit disabled during occultations.
1380 - UV1 - Aperture Map - 902384A6
The original design of this test included all four image dissectors. The first attempt to run 1380 in the 90197 SMS (discussed above) ended with a safmg in the VIS detector portion of the test, which was the first of the four detectors scheduled. It was obvious after that experience that tests should be scheduled in smaller units to create fire walls such that a failure in one part of a test would not waste excessive spacecraft time. Subsequent tests were redesigned and rescheduled one detector at a time. The first instance of this new approach, the UV1 portion of 1380, was executed as planned. The data were satisfactory. The only
14 HSPOVReport (VI.0)
anomaly during this test was a T error caused when the commanded value of a parameter does not agree with the value in the telemetry value table. In this case a deflection value was commanded, for example, to 4098 and the telemetry table was reporting 4098 modulo 4096 or 002. The T error indicated the deflection had "wrapped" and had been commanded to a value modulo 4096 from value in the test procedure. This did not cause any difficulties in either operations or data reduction because the modulo 4096 value is valid and useful data were extracted.
1380 - UV2 - Aperture Map - 902494A6
The results from this test were similar to the UV-1 portion of the test. Satisfactory initial aperture maps were obtained. From these data it was evident that the expected "banana" effect was not as large as expected and the "new hold" mode was providing a stable thermal environment.
1503 - UV1 - Phase II Alignment - 902537AB
This test was the f'trst HSP observation of an actual star, the f'trst old photons detected by the HSP. The test was designed to locate the ten arc second diameter finding aperture to within 0.5 arc seconds in HST V2/V3 coordinates. The general idea of the test was to point the HST to the target star placing it in the 10 arc second finding aperture, then offset to the corner of a 4 x 4 HST step and dwell scan pattern (each step being 2.0 arc seconds) and perform a 20 x 20 HSP map mode scan (using the standard default 0.5 arc second step size) at each of the 16 points of the HST dwell scan. The HSP 20 x 20 map covers the entire finding aperture. The resulting data are a set of "images" of the finding aperture at each of the 16 HST dwell points in a 4 x 4 square pattern. The idea was to locate the target even if the initial blind pointing had errors of several arc seconds. Analysis of the data would provide the location of the f'mding aperture in V2/V3 coordinates. The test was executed as planned but the resulting V2/V3 locations were inconsistent with*he UV2 positions determined in the subsequent test of UV2 in the 90260 SMS. The errors in the FGS-to-SI alignment matrices at the time were the cause of all the difficulties. Later improved matrices were used to reanalyze the data and resulted in consistent and precise positions.
15 HSP OV Report (V1.0)
IDT 2 (UV1) 1503 Results
16_
15
14
12
The chart above shows the position of the target star in the HSP 20x20 map of the finding aperture for each of the 16 positions of the HST step and dwell scan. The target was seen only in steps 1, 2, 7, 8, and 9.
1503 - UV2 - Phase II Alignment - 902607D2
The test method for this portion of the test is the same as for detector UV1 described above. The results for UV2 did not agree with the UV1 results in that there was no rigid body shift of both detectors that could account for the V2/V3 positions derived from the data. Further, the differences between the positions derived from the 1503 data and the prelaunch positions are too large to be accounted for by measurement error. The problems were due to errors in the FGS-to-SI alignment matrices, later improved. Using the improved matrices, the HSP positions were consistent and credible.
16 HSP OV Report (V1.0)
4
!
I
IDT 4 (UV2) 1503 Results
The above chart shows the position of the target star in the 20 x 20 map of the HSP finding aperture for each of the 16 points in the HST step and dwell scan. The target was seen only in steps 7, 8, 9, 10, 15, and 16.
17 HSP OV Report (VI.O)
1382 - UV1/2 - PAD Threshold Test - 902817B8
The purpose of this test was to determine the optimum PAD threshold by observing the bright earth at various threshold levels and plotting the curve of response as a function of threshold level. The unpredictably large variations in the brighmess of the earth proved to be greater than differences between threshold levels and the resulting data (see chart below) were of little value beyond confh-ming that the prelaunch PAD default values were satisfactory.
1382- LIGHT/DARK RATIO
2500,
1$oo
lO_l
5oo
t_ 14
PAD
1504 - UV1 - Phase III Alignment - 902957A9
This test was designed to map precisely the edges of the finding aperture and of selected one arc second apertures. This was accomplished by first acquiring the target in the finding aperture, offsetting the target to near the edge and performing a spacecraft linear step and dwell scan while collecting single color photometric data. The design of the test predated the discovery of spherical aberration and it was executed before good FGS-to-SI alignments were available. The acquisition was successful but the spherical aberration made the length of the step and dwell too small to indicate the edge of the aperture reliably. The FGS alignment was sufficiently imprecise at this stage to place the target in the one arc second aperture. The test did not, therefore, accomplish the intended objectives. The HSP fine alignment test was redesigned to use a spacecraft continuous scan to sweep the target across selected apertures in a raster pattern designed to be sufficiently large to cover the uncertainties in the FGS-to-SI alignment.
18 HSP OV Report (V1.0)
1526 - UVI/2 - Aperture Map - SV - 903027AC
This test is the SV version of 1380, aperture map, for the UV detectors. It ran as planned and the data were used to improve our knowledge of aperture locations in HSP detector deflection space.
3069 - 10.2 Test - 903104A4
This test was run to verify the changes in 10.2 reconfiguration software required to correct the bright earth sating problems encountered in 1380 by the VIS detector and in 1379 by the PMT. The detectors were operated in the same manner as the proposed revisions to the 10.2 reconfiguration software. There were no problems and everything worked as planned. Several interesting and useful results of the test were obtained that were not entirely planned. The VIS, POL, and PMT detectors were operated throughout the orbit, both during the dark target time and earth occultation. This gave not only useful dark count data, but information about the settling time required to return to nominal dark counts after bright earth exposure. That time was shorter than expected and is about five minutes for the PMT. Since the data were taken in the "all" format, both analog and pulse counting data, it was possible to plot pulse counting response as a function of analog output over a wide range of brightness. The variations in brightness of the earth here produced a data set that would otherwise be impractical to obtain with stars. The results shown in the chart on the following page conf'u'med the detector dead time and linearity characteristics.
1503 - UVI/2 II - FGS/HSP Coarse Alignment - 910217BD
This test repeated an earlier test. It was scheduled before it was clear that FGS-to-SI alignment matrix • errors were the cause of the inconsistencies in earlier data. But, once the alignments were determined, this data set and the prior data verified repeatability of the alignment.
3140 - Phase III Alignment - (partial)- 910427D6
This test was a reduced version of the previously run 1504 test that was scheduled before the new HSP fine alignment test was created and approved. This test was not successful because at the time of execution the FGS-to-SI alignments were not known to the required precision. HSP system controller T errors were observed in the engineering data. These were later identified as the result of a single event upset in HSP RAM. The HSP system controller was "rebooted" and the problem disappeared.
3093 - Aperture Map - Det 1 & 3 - 910707C6
The VIS detector aperture mapping test was revised to use the Orion Nebula for selected filters and the bright earth for others. It was run as soon as the revised 10.2 reconfiguration software was available. The test executed as planned, except for some missed bright earth observations because of a problem between SOGS and PASS in calculating when the bright earth limb was in view. The data were used to refine aperture positions as a function of detector deflections.
3152 - Phase IV Align - Det 4 - 910707C6
This is the first use of the revised HSP fine alignment test using a raster scan of the target across selected small apertures. The data proved to be remarkably good and led to more precise determination of aperture positions than was originally anticipated. The data also are useful for determining the point spread function of a target in the HSP apertures. This was also the first test run after the T error (single event upset) reboot and since there were no T errors or other anomalies it confkmed that there were no permanent consequences of the single event upset.
19 1 I I I I I
30000
Plot of PMT data from 3069: Observation 20000 number v0el0109t pulse counting data (.d0h) plotted as a function of analog data (.d2h)
Thu Nov 8 04:29:32.00 1990 Program ID: 0El, Obs set: 01, Obs ID: 09 'x3 Rate: 32 Kbits/sec mode: SCP dfmt: ALL WPL: 960 LPF: 1 FPO: 156 reqdet: 5 voltage: 2184 V (168 counts) itime: 5 ms 10000 dtime: 0 ms PAD: 300.9 mV (20 counts) CVC gain: 10000 nA bytes per observation: 299520 bytes per sample: 5 samples per observation: 59904 collect time = 299.918 s xmit time = 85.5771 s Stop: Thu Nov 8 04:34:31.92 1990) HST RA: 02H 51M 25.903S HST Dec: +16D 25' 53.547" HST PA: +106D 57' 21.302"
I I I I I I I I I I 1 1000 2000 3000 4000
Analog output (raw counts: 4096 = 10,000 nA) HSP OV Report (V1.0)
3152 - Phase IV Align - Det 2 - 910707C6
This test of UV1 executed smoothly as did the portion for UV2. The data were high quality and similar to the 3152-UV2 data.
3072 - Target Acquisition UV1 - 910917BC
In this SV test the first HSP mode 11(on-board) target acquisition was done. The target was acquired and all algorithms performed as intended on the first try. Several iterations were designed into the test that showed that the accuracy and repeatability of the acquisition improved if it were done twice. The standard Mode II procedures were subsequently modified to perform two acquisitions to more precisely center the target star in the finding aperture, which is critical with the spherical aberration degraded image.
3073 - Target Acquisition UV2 - 910917BC
The results of the UV-2 portion of the test were similar to those obtained for UV-1.
2948 - FGS/HSP Fine Alignment UV2 - 910987C9
This test is the originally planned SV version of the HSP fine alignment test and was put into the schedule before the alignment test was revised. It executed properly and provided good data, considering the limitations imposed by the spherical aberration, but the data were not as useful as that provided by the revised tesL
2949 - FGS/HSP Fine Alignment UV1 - 910987C9
This test is the UV-1 portion of the originally planned SV version of the HSP fine alignment test and was put into the schedule before the alignment test was revised. It executed properly and provided good data, considering the limitations imposed by the spherical aberration, but the data were not as useful as that provided by the revised tesL
3152 - Fine Alignment VIS & POL - 911057D5
Here the first attempt to perform the new modified lISP fine alignment test on the VIS and POL detectors was made. The VIS detector data were satisfactory and met objectives. The POL data appeared at In'st to be the victim of a "missed observation" because the count rate was much lower than expected. Later analysis showed the test executed properly but the f'dters on the POL detector were apparently reversed from the order shown in the drawings. The data also showed that the desired accuracy for determination of the POL tube apertures in both deflection and V2/V3 coordinates could not be obtained because the POL tube has a 16 apertures (rather than the 50 of the other image dissector tubes) with which to fit the 13 parameters of the aperture position model. A new test was devised (3377) to obtain the required data.
3007.UV2 - Jitter (SAO) - 911197B8
This test was intended to check HST jitter by observing a target for an hour with 2.0 millisecond integration times. The test failed for two reasons: the target was not seen in the finding aperture and was therefore not acquired; the HSP did not complete science data transfer to the SDF. The reason the target was missed was incorrect coordinates. The target has relatively large proper motion that was not properly considered. The science data transfer problem was one that was identified in 1984 but was forgotten when the test was designed. The HSP cannot use multi-line frames with the lower data rates (32 kbs and 4 kbs)
20 HSPOVReport(VI.0)
because of the timing constraints between fines. The reasons for this were explained in Richard White's 1984 paper (Timing Considerations for HSP Data Collection, 21 March 1984) as follows:
"Because the SDF was designed for image data, it expects the Sis to send all lines of a given frame in rapid succession. If a line is not ready within 10 msec of when it is requested, the SDF assumes that something is wrong with the SI and puts it off-fine, terminating the observation...
The minimum length for a line when it is written onto the tape is 1 segment, which requires about 30 msec at 32kb. This means that the HSP must require more than 30 msec to collect a fine in order that the tape recorder be able to keep up with it. On the other hand, the HSP to SDF transfer always goes at 1Mb, and takes at the most 15 msec. Thus the difference between the HSP data collection time and the HSP to SDF transfer time must be greater than 15 m sec and must therefore exceed the 10 msec limit. The same arguments apply (with stronger limits) for the 4kb fink. Consequently, all observations using the slow links will have only 1 fine per frame."
This problem would have been exposed earlier by the planned but scrubbed OV test 1501, Data Integrity. (The test was scrubbed because it was a test of the science data path, not of the HSP itself. Arguments that system level interactions should be tested were not accepted. In any case, we were remiss in forgetting this aspect of HSP data collection.) A simple fix has been found that would allow long data collections at the 32 and 4 kbs rates. Since there are no timing constraints between frames, the present HSP upper limit on number of frames could be relieved by resetting the frame count during the data collection.
3074 - Mode II Target Acq - VIS - 911276A2R
The results of this test were similar to 3072 and 3073, mode II target acquisition tests of UV1 and UV2. It was successful and confirmed the need to perform two acquisitions to get the best centering of the target star.
3071 - Mode II Target Acq - POL - 911276A2R
This test was similar to 3072, 3073, and 3074. The results were, as in the other tests, successful, and confirmed the need for two iterations of the mode II acquisition to get the required centering of the target star.
3233 - Fine Alignment - UV - 911337C8
Test 3233 was similar to 3152 except mode II target acquisition was used and the size of the HST raster scan was reduced. The scan was executed twice, in orthogonal patterns, to provide higher quality results. The test was successful and excellent data were obtained.
3233 - POL - Fine Alignment - POL - 911547D3
The results of the fine alignment on the POL tube were satisfactory, but because of the greater uncertainty in the determination of the aperture positions on the POL tube (there are only 16 apertures on the POL tube rather than the 50 on the other image dissector tubes with which to fit a 13 parameter model) the resulting model fit did not produce positions with as small uncertainty as the other image dissector tubes. A new SV test (3377) was devised to produce the required data.
21 HSP OV Report (VI.0)
1385 - Photometric Performance - 911547D3
This SV test was designed to verify the photometric linearity and accuracy of the HSP. The data were satisfactory except for missed targets.
3233 - VIS - Fine Alignment - VIS - 911547D3
The results for the VIS detector were similar to the UV detectors. The data was satisfactory and produced good aperture positions.
4.4 Database Updates
The OV database updates involved two different files: the SICF file containing the positions of the HSP apertures in detector H/V deflection coordinates and the SIAF f'fle containing the positions of the HSP apertures in HST V2/V3 coordinates. The early stages of OV were designed to ref'me the SICF (deflection coordinates) data using the bright earth as a fiat field. Later tests were intended to determine the SIAF (V2/V3 position) parameters using stars once the deflection parameters were well established.
The first test designed to provide SICF input was 1380, HSP aperture mapping. The test provided useful data but also showed that the bright earth was too bright for several filters on the VIS and POL detectors. It was also clear from the initial data from 1380 that the test parameters could be optimized to provide much higher quality data. The size and number of points in the aperture maps were changed to provide more resolution. In 1380, 20x20 maps of individual apertures having 0.5 arc second spacing were used. The revised tests used 30x32 maps with 0.1 arc second spacing. The 80x12 maps of filters were changed to. 60x16 to better fit the dimensions of the filters. The "flat field" target for selected filters of the VIS and POL detectors were changed from the bright earth to the Orion Nebula. The following filters on the VIS and POL detectors and all UV filters use the bright earth: POL: F216M, F237M, & F277M; VIS: F184W, F240W, & F262V. All other filters use the Orion Nebula. Integration times were also adjusted based on the 1380 results to provide improved signal to noise ratio. Data quality was also affected by scattering in the detectors and variations in the brightness of the bright earth during the time of the observation.
The next round of aperture mapping tests, 3093, incorporated the changes described above and produced much better data. The new data were applied to the model and produced some interesting results. It was known that the electron optics in the IDTs had pin cushion distortion but the model results also showed that there were different plate scales for H and V. The standard deviation of the fit for the VIS detector is about 3-4 deflection steps in both H and V.
Early attempts to produce data for the SIAF file were frustrated by the poor FGS-to-SI alignment. In fact, it was so bad that a target could not be reliably placed in a 10 arc second finding aperture. Tests were put on hold for several months until the FGS to SI alignment matrices were sufficiently accurate to continue. In the interval, the test was redesigned to capture the desired information even if the HST pointing had larger than expected errors. The revised scheme involved a five arc second square HST scan of the area around the intended target to insure it was detected. The revised tests were successful and the FGS to SI alignments improved so that the resulting data has uncertainties in aperture positions of 0.01 arc second in V2 and 0.02 in V3.
Once the SICF and SIAF flies were updated, the mode II target acquisition tests were performed. The most significant result was that two iterations reduce the pointing error substantially in some cases. We therefore adopted two iterations as standard practice. A summary of the database updates made in the OV period follows:
Test S MS Database File date of update
1503 90-253, 90-260 PDB SIAF 10-16-1990 91-021, 1-31-1991 1504 90-295 PDB SIAl: 1-31-1991
22 HSP OV Report (V1.0)
1526 90-302 PDB SICF 1-29-1991 3152 91-070 PDB SIAF 3-25-1991 91-105 4-30-1991 3093 91-070 PDB S ICF 3 -29-1991 3233 91-133,91-154 PDB SIAF Not Planned 3071 91-127 None 3072 91-091 None m 3073 91-091 None 3074 91-127 None 1385 91-154 None CDBS CVCCP5R Not Planned CDBS CVCCP4R Not Planned 2769 91-168,91-175 CDBS CVCCP4R Not Planned 3006 91-182 None 3362 91-189 PDB SIAF Not Planned 3363 PDB SIAF Not Planned 3377 PDB SIAF/SICF +3 Weeks 3119 Wk38 PDB S ICF Not Planned 3120 PDB SICF +2 Weeks 3135 PDB S ICF Not Planned 3007 None 1386 CDBS POLEF?. ? +3 Weeks 1383 None 1389 None
4.50V Anomalies
The major unresolved problem from the OV period, although not strictly the result of an OV test, was the data hang in 3007. The fix is straightforward and involves resetting the frame count during the data collection to remove the 255 frame per observation limit.
There were many HSTARs written but most were not indicative of major problems. The major anomalies that occurred during the OV period that had significant schedule impact are:
1. HSTAR 574 - PMT High Voltage Turn-on
The PMT high voltage turn-on anomaly was corrected by limiting operation of the PMT high voltage power supply to higher voltages closer to the nominal operating range of the PMT's corotron. Appendix B contains a more detailed discussion of the PMT high voltage turn on anomaly and subsequent investigation.
2. HSTARS 836 and 1072 - Bright Object Safing
The operational procedures were modified to avoid bright earth limb sating.
3. HSTAR 1537 - Missed Target
The FGS/SI alignment was not sufficiently accurate to support the planned test design when HSP fine alignments were first attempted. Subsequent improvements in both the alignment matrices and the design of the test resulted in satisfactory data. But, there was substantial schedule impact to the HSP OV program because the FGS alignment took much longer than planned.
The following list of HSP related HSTARs represents our understanding but should be used with caution because HSTARs concerning the HSP are often opened without our knowledge, HSTARs that are opened by HSP team representatives sometimes are lost, HSTAR closures submitted by the HSP team are often lost, and often HSP related HSTARs are closed by others without our knowledge.
23 HSP OV Report (V1.0)
HSP HSTAR dispositions as of 11-07-91:
HSTAR # Description Disposition Due ORG
010 HSP Structure Temp VTPMTPB CLOSED 04-29-90
205 HSP 2113 Mere. Dump Miscompares STGS DR 07-19-90 HSP 1097 207 HSP High Volt Out of Limit CLOSED 06-19-90 HSP
232 DCF Missing Data Packet for CLOSED 06-07-90 LMSC HSP 1500
242 HSP 2113 Mem. Dump Miscompares STGS DR 07-19-90 PORTS 1097 298 HSP High Volt Mon Out of Limit CLOSED 06-19-90 MOC
369 HSP UDL and SHPs Missing CLOSED 06-07-90 LMSC
401 STR P/B of HSP Data Missing CLOSED 08-07 -90 LMSC SHPS and UDLS
529 HSP Data Missing from STR Dump CLDSED 06-12-90 LMSC
530 HSP Data Missing from STR Dump CLOSED 06-12-90 LMSC
574 Unexpected PMT Behavior in 1502 CLOSED 10-05-90 HSP
578 HSP Data from STR Missing CLOSED 06-14-90 STPG SHP/UDL 579 HSP Data Missing from STR Dump CLOSED 07-24-90
581 HSP Data Missing from STR Dump CLOSED 07-24-90 MOC
672 Missing Calibration Files 1500 CLOSED 07-19-90 HSP
836 HSP Safed by BOP in 1380 Det 3 CI.DSED 09 -20-90 HSP
958 HSP Safmg Recovery STBF Error CLOSED 08-28-90 STSCI
998 AN Crossing Times Missing CLOSED 08-17-90 STSCI
999 OSS Not Able to Print CLOSED 08-17-90 OSS Tab Listing 1072 HSP Safed by BOP During CLOSED 09-20-90 HSP 1379 PMT 1112 V'I'PAFB 1/VTPAFB2 Low Lira CLDSED 09-20-90 MOC Violation
1115 VTPNP2C Low Lira Violation CLOSED 09-20-90 MOC
1120 ES S Time Tag Error CLOSED ESS
1145 HSP 1380 T Errors O.OSED 09-26-90 HSP
1186 Third Dump of HSP STR Data CLOSED 09 - 14-90 Missing
1267 OSS Data doesn't Match PODPS CLOSED 01-17-91 STSCI Data for HSP 1503 Det 4
135 8 HSP Clock Overflow Error CLOSED 10-22-90 HSP
1476 HSP Data Contains Inversion CLOSED 11-07-90 LMSC
24 HSP OV Report (V1.0)
1514 HSP Data Contains Multiple CLOSED 11-21-90 LMSC Inversions
1537 Missed Target HSP CLOSED 11-21-90 STPG
1555 Data Inversion In HSP Data CLOSED 01-08-91 CD500
1662 HSP 1526 Failed Observations OPEN 02-04-91 STSCI
1957 HSP TLM Error OPEN 02-20-91 MOC
1959 HSP 3140 Pointing Error CLOSED 02-20-91 PCS Exceeds 2"
1967 VTERROR out of limits CLOSED 02-20-91 HSP
2094 Incorrect Struts in PSTOLS CLDSED 03-19-91 MOC HSPSBYHD & HSPHDSBY
2169 Missing Bright Earth OPEN 03-27-91 STScI in HSP 3152
2208 HSP FITS Header Discrepancies OPEN 04-09-91 STSd
2235 PDB Update Identified Post CLOSED 04-10-91 HSP Final Mode
2274 Missing HSP Observations OPEN 05-03-91 STSd in 2948/2949
2307 HSP SCP Collection Star CLOSED 04-30-91 STPG Not Seen in Aperture
2317 Missing Obs in HSP 3152 POL CLOSED 05-02-91 STPG
2329 Missing Obs in HSP 3007 CLOSED 05-07-91 STIr3
2334 HSP Bus Dir Memory Not Dumped OPEN 05-08-91 STScI
2343 HSP Error Flag OPEN 05-09-91 MOC
2371 HSP Memdump Compare Needs OPEN 05-17-91 MOC Modification
2408 BE of HSP Microprocessor Dump REJ. 05 -28-91 MOC
2420 HSP Obs Not Written to FITS OPEN 05-30-91 STScI FMT Tspe
2471 No Target for HSP Program 1385 OPEN 06-12-91 STScI
2485 Targets Not Seen In HSP 1385 OPEN 06-14-91 STScI
2635 Missing Bright Earth HSP 3362 CLOSED 08-16-91 PCS
2659 Bad HSP 2769 VIS Data Due to CLOSED 08-19-91 PCS SIC Jitter
2660 Inconclusive HSP 2769 Data CLOSED 08-19-91 STScI Using AGK+81DZ66
2661 Missing Bright Earth in HSP CLOSED 08-19-91 STScI 3119
25 HSP OV Report (V1.0)
2681 HSP FITS HEADER KEYWORD OPEN 08 -22-91 STSCI FFSROH._ CALLED-
2697 lISP DATA LOSS DUE TO SIR OPEN 09-03 -91 STSCI TAPE TRACK CHANGE
2733 HSP 1389 DATA DEGRADATION OPEN 09-13-91 PCS
2796 UNEXIK,AINED PERIODIC EFFECT OPEN 10-01-91 SESD IN HSP 1389 SCI-
2868 lISP DATA LOG AFI'ER OUTPLrI" OPEN 10-25 -91 STSCI CEASE
2869 OSS DISCARDED DATA FROM HSP OPEN 10-25-91 STSCI OBSERVATION
OPEN HSP HSTARs as of 11-07-91:
HSTAR# Title Status Asgnee Due
1662 HSP 1526 failed observations Open STScI 02-4-91
2208 HSP FITS Header Discrepancies Open STSd 04-09 -91
2274 Missing HSP Observations Open STScI 05 -03 -91 in 2948/2949
2334 HSP Bus Dir Memory Not Dumped Open STScI 05 -08 -91
2343 HSP Error Flag Open MOC 05 -09 -91
2371 HSP Memdump Compare Needs open MOC 05-17-91 Modification
2420 HSP Obs Not Written to FITS Open STSd 05-30-91 FMT Tape
2471 No Target for HSP Program 1385 Open STSd 06-12-91
2485 Targets Not Seen In HSP 1385 Open STScI 06-14-91
2681 HSP FITS HEADER KEYWORD Open STSCI 08-22-91 PTSROFLG CALLED-
2697 HSP DATA LOSS DUE TO STR Open STSCI 09-03-91 TAPE TRACK CHANGE
2733 HSP 1389 DATA DEGRADATION Open PCS 09-13-91
2796 UNEXPLAINED PERIODIC EFFECT Open SESD 10-01-91 IN HSP 1389 SCI-
2868 HSP DATA LOG AFI_R OUTPUT STSCI 10-25-91 CEASE
2869 OSS DISCARDED DATA FROM HSP Open STSCI 10-25-91 OBSERVATION
26 HSPOVReport(V1.0)
4.6 End of OV Status and Liens
All basic HSP functions have been verified and all are working properly as of the end of the OV period. The fine alignment, especially the POL tube alignment, will continue into the SV period.
No reasonable mechanism is available for dumping the HSP memory and getting the resulting science data in electronic form. The bus directory memory pages require special procedures to dump. The single event upset events (two so far) have demonstrated the continuing need to have a straightforward means to dump and check the HSP memory including the bus director memory. As of the end of OV, an effort is underway to create standard procedures to perform this operation and to provide FITS files of the resulting data.
The commanding change to provide for resetting the frame count during a data collection is needed to restore full HSP capability.
5. Modifications and Recommendations
The major modifications to operations procedures arising from HSP OV results are:
1. The minimum HVPS turn-on voltage for the PMT was increased from 1500 to 1900 volts.
2. The management of bright earth occultations was modified for the VIS, POL, and PMT to avoid bright object safing
3. The mode II target acquisitions include two iterations. (this is actually the result of an SV test)
5.1 Trend Monitoring Recommendations
There are no trend monitoring procedures for the HSP engineering data. However, any significant or sudden unexplained change in temperatures, voltages, or other parameters should be investigated. Any limit exceeded also should be investigated. Detector parameters are monitored as part of the on-going HSP calibration plan.
5.2 Instrument Operational Recommendations
There are several issues unresolved as of this writing. The following actions should be taken before the close of the SV/GTO period:
1. The capability to reset the frame counter should be implemented to allow the HSP to function with the 32 kb link to the tape recorder.
2. The RIU polling on/off capability should be prepared and tested. There is evidence that the RIU reply bus noise is detected by the HSP. The polling on/off capability could be used to perform observations that would otherwise be compromised.
3. The remaining capabilities of the HSP thermal control system should be exercised.
4. The capability to dump HSP memory, including the bus director memory, and to provide fits files of the resulting dump data should be implemented as soon as possible. If there are future single event upsets, or other anomalies, it will be important to have this capability to enable timely analysis of the problem.
5.3 Conclusions & Lessons Learned
27 HSPOVReport(VI.O)
TheOVprogramhasdemonstratedthatthegroundsystemlackstheflexibilityandcapabilitytorespond reasonablytonormalverificationactivities.Theinabilitytoroutinelyprocessgenericsciencedataisone example.Oneshouldbeabletoprocesssciencedatawithotherthananticipateddetectorgainsettings.
Thepre-launchtestdesignandscheduleweretoosuccess oriented. Tests had to be broken into smaller units to prevent large losses of spacecraft time in the event of problems. Tests were scheduled on the assumption that needed spacecraft support capabilities would exist by the time the test was executed. Often these assumptions were incorrect and led to additional test failures, loss of spacecraft time, and additional delays in implementing improved tests.
The OV program has shown that efficient operations depend on being able to adjust operations procedures to meet the conditions actually encountered that may be different than anticipated before launch.
28 HSPOVReport(V1.0)
Annendix A - HSP OV. SV. & GTO nronosal numbers and names
"pgm" classes: OV Orbital Verification SV Science Verifcafion SVD Science Verification (Delta plan) GTO Guaranteed Time Observation SAO Science Assessment Observation /X Cancelled
prop pgm name 1079 GTO Opportunity occultations by small bodies (see 3319) 1080 GTO The size and composition of planetary ring particles(see 3373) 1081 GTO Saturn ring dynamics (see 3371.3375) 1082 GTO Helium abundances in Jovian planet upper atmospheres (see 3354) 1083 GTO Dynamics of planetary upper atmospheres (see 3376) 1084 GTO Lunar occultations with the HST 1085 GTO/X Rotation periods of cometary nuclei 1086 GTO Do Neptune and Pluto have rings? 1087 GTO/X Eclipses and occultations by Pluto and Charon 1088 GTO Small satellites in the Uranian system 1089 GTO Captured satellites of the Jovian planets 1090 GTO Periodic variations in DQ Herculis stars (see 3257) 1091 GTO UV pulsations from X-ray pulsars 1092 GTO Eclipses of cataclysmic variable stars (see 3238) 1093 GTO Observations of ZZ Ceti stars 1094 GTO Search for optical variability assoc, with black holes (see 3255) 1095 GTO Variability of high luminosity stars (see 3252) 1096 GTO Gravitational lenses (part I) (see 3250) 1097 GTO X-ray binaries (see 3234,3256) 1098 GTO Remnant stars in SNRs (see 2953,3251) 1099 GTO Active galactic nuclei (see 3248) 1100 GTO/X Evolution of the nuclei of planetary nebulae 1101 GTO Optical and UV observations of radio pulsars (see 3253) 1102 GTO UV light and polar, variations in Beta Cephei stars 1103 GTO Vis/UV light curves of short period RR-Lyrae stars (see 3254) 1104 GTO High speed photometry of GBS 0526-66 1379 OV Detector dark count test 1380 OV MSC Focus and aperture mapping test (phase I) 1381 SV Target acquisition test (see 3071-3074) 1382 OV Pulse height distribution test 1383 SV Time resolved photometry 1384 SV Color transformation test (see 2769,2770) 1385 SV Photometric performance test 1386 SV Instrumental polarization test 1387 SV Stokes parameter test 1389 SV Short-term photometric stability 1391 GTO Gravitational lenses (part II) 1474 SV Photometric performance test 1499 OV Command response test 1500 OV Detector data test 1501 OV Data integrity test 1502 OV High voltage turn-on test 1503 OV MSC coarse FGS/HSP alignment (phase II) 1504 OV MSC fine FGS/I-ISP alignment (phase III) 1524 SV MSC fine FGS/HSP alignment (phase III) (see 2948-2951) 1526 SV MSC aperture mapping test (phase I) (UV) (see 3093, 3119, 3120) 2113 OV Memory dump
29 HSP OV Report (V1.0)
2201 OV Safe-to-oldhold 2749 SV RILl polling on/off test 2768 SVD Pulse height distribution test 2769 SV Color transformation test 2770 SVD Color transformation test 2771 SV Stellar occultation by planetary rings 2772 SVD Stellar occultation by dark lunar limb 2773 SVD Stellar occultation by planetary atmospheres 2948 SV MSC free FGS/I-ISP alignment (phase III) (UV2) 2949 SV MSC fine FGS/I-ISP alignment (phase III) (UV1) 2950 SV MSC t-meFGS/HSP alignment (phase III) (VIS) 2951 SV MSC fine FGS/I-ISP alignment (phase III) (POL) 2952 GTO X-ray binaries (see 3249) 2953 GTO/X Remnant stars in SNRs (see 1098,3251) 3006 SAO Effect of centering errors on HSP photometry 3007 SAO Effect of jitter on HSP photometry 3069 OV 10.2/Bright earth test 3071 SV Target acquisition test (POL) 3072 SV Target acquisition test (UV1) 3073 SV Target acquisition test (UV2) 3074 SV Target acquisition test (VIS) 3093 SV MSC aperture mapping test (phase I) (VIS) (see 1526) 3119 SV MSC aperture mapping test (phase I) (VIS) (visit 2) (see 1526) 3120 SV MSC aperture mapping test (phase I) 0/IS) (visit 3) (see 1526) 3140 SV MSC fine FGS/I-ISP alignment (phase III) (nelson plan) (see 1504) 3152 OV MSC aperture mapping test (phase II/III) (jwp plan) 3233 OV MSC aperture mapping test (phase II/III) (jwp plan) (see 3152) 3234 GTO X-ray binaries (see 1097,3256) 3238 GTO Eclipses of cataclysmic variable stars (see 1092) 3248 GTO Active galactic nuclei (see 1099) 3249 GTO X-ray binaries (see 2952) 3250 GTO Gravitational lenses (part I) (see 1096) 3251 GTO Remnant stars in SNRs (see 1098,2953) 3252 GTO Variability of high luminosity stars (see 1095) 3253 GTO Optical and UV observations of radio pulsars (see 1101) 3254 GTO Vis/UV light curves of short period RR-Lyrae stars (see 1103) 3255 GTO Search for optical variability assoc, with black holes (see 1094) 3256 GTO X-ray binaries (see 1097,3234) 3257 GTO Periodic variations in DQ Herculis stars (see 1090) 3319 GTO Opportunity occultations by small bodies (see 1079) 3354 GTO Helium abundances in Jovian planet upper atmospheres (see 1082) 3362 OV HSP prop 3233 visit 2 3363 OV HSP prop 3233 visit 3 3371 GTO Saturn ring dynamics (later cycles, see 1081, 3375) 3373 GTO The size and composition of planetary ring particles (see 1080) 3375 GTO Saturn ring dynamics (cycle 1, see 1081, 3373) 3376 GTO Dynamics of planetary upper atmospheres (later cycles, see 1083) 3377 SV Pol detector test 3382 SV Revisit of 1385 to obtain 13th and 15th, but not 9th, mag targs
30 HSP OV Report (V1.0)
Appendix B - PMT High Voltage Turn.On Investipation
7/17/90 S. Ellington
This report summarizes the results of tests done to date in an effort to determine the cause of the noise counts observed in HSP when minimum voltage is applied to the PMT. Several plausible causes of the noise have been investigated. Some of the possible causes have been effectively ruled out, while two of them are consistent with the test results.
1. Flight PMT Noise Description
Noise counts were recorded during several tests of the flight PMT in orbit. These tests were performed with high voltage set to the minimum value (about 1475 Volts), and the PAD threshold set to the normal operating value of 20. There was no significant light at the PMT. At this high voltage setting, there is less than 200 Volts across the PMT dynodes, which is normally much too low to cause any counts.
During these tests, noise counts increased from about 200 counts/see immediately after high voltage turn-on to about 2,00 counts/sec 37 seconds later, when the test was terminated. The increase in count rate resembled an exponential rise until the last few seconds of the test, when it increased more slowly. Analog (CVC) data showed fluctuations, but no significant change in average value. The amplitude of the analog data fluctuations did not change significantly during the test.
2. Test Equipment Description
The HSP Engineering Model instrument with an unpotted flight spare PMT Assembly were used for some tests. Data was collected with the HSP EGSE. Operation of this instrument closely simulates that of the flight instrument.
A PMT Test Circuit was also constructed. It consists of a flight- type Photomultiplier Tube (Hamamatsu R666S) in a metal enclosure, with a tube socket, dynode resistors, and corotron. It is electrically equivalent to the flight PMT Assembly, but is unpotted. The PMT Test Circuit was tested for normal noise level, dark count, and response to light. It's performance appeared similar to the flight unit.
Noise sensitivity measurements were made with a detector system identical with that used in HSP. It has an engineering model Preamp and PAD, with auxiliary circuits to provide a manually adjustable PAD threshold and an interface to a laboratory frequency counter. This system responds precisely as the flight electronics do, while providing more flexibility.
Corotron tests were performed with a simple breadboard circuit, a well as with the flight spare PMT Assembly and the PMT Test Circuit
3. Corotron Oscillation
Tests of 3 different corotron voltage regulators showed that in the PMT circuit they became unstable and produced a relaxation oscillation at low operating currents. The current at which they became unstable ranged from 6.8 to 8.0 microamp at room temperature. The critical current decreases about 3 percent at -5 deg. C, the approximate temperature of the flight PMT. The absolute minimum corolron current in the flight PMT Assembly is 12 microamp, so it is not likely that this type of oscillation is present unless another failure has occurred.
In tests with both the flight spare PMT Assembly and the PMT Test Circuit, the high voltage was reduced below the normal minimum value of 1475 Volts to deliberately induce corotron oscillation when connected to HSP detector electronics. Both the HSP Engineering Model instrument and the separate detector system were used. The corotron was monitored during these tests to verify that oscillation was taking place. No noise counts were observed because of corotron oscillation. This is not surprising, because the rise and fall times of the voltage across the corotron during oscillation are more than a factor of 100 too long to couple sufficient current into the Prcamp through the capacitance of the PMT.
31 HSP OV Report (V1.0)
Corotron oscillations do not appear to be a likely cause of the PMT noise because the operating current is well above the minimum value at which oscillation occurs, the rise and fall times are much too long, and deliberately induced oscillations didn't produce any noise counts.
4. Discharge in Parallel with Corotron
In normal operation, even at minimum PMT voltage, 1300 Volts appears across the corotron. Because the lead spacing is only 2.7 mm (0.105 inches), a parallel discharge path is possible. Because the dynode resistors are in series with the corotron, even a very low voltage discharge across the corotron would not cause the High Voltage Power Supply to shut down at minimum voltage. (A discharge from high voltage to return or chassis would almost certainly cause the HVPS to shut down.) Because the corotron is within the potted portion of the PMT Assembly, such a discharge would probably indicate a potting failure.
Because of the large voltage across the corotron, a parallel discharge could produce very large voltage fluctuations at the PMT cathode. The repetition frequency of the discharge depends on the breakdown and sustaining voltages of the path and, of course, the time constant of the components in the PMT Assembly. The minimum frequency is about 35 Hz, while a frequency of 2 kHz requires that the difference between the breakdown and sustaining voltages be around 10 Volts. These values are consistent with the measured frequency of PMT noise in the flight instrument of 200 Hz to 2 kHz.
A simple spark gap was added to the PMT Test circuit in parallel with the corotron to measure the effect of such a discharge. The spark gap was at atmospheric pressure, so it was not expected to behave precisely as would a discharge around a potted corotron in vacuum. However, periodic discharges were easily induced, which produced extremely large voltages at the preamp input. (A small capacitor was installed in place of the PMT, to avoid possible damage to the PMT.) Peak voltage at the preamp input was measured at 5 to 20 Volts (sic), depending on the size of the gap. (The normal PMT operating PAD threshold is about 150 microvolts.] Count rates of 50 Hz to 1.3 kHz were observed as the size of the gap was reduced. There was no sign of increase in frequency with time with a fixed gap.
5. Erratic Dynode Resistor
One possible cause of the PMT noise is erratic fluctuations in the value of a dynode resistor. Failure of the connection at the end of one of these metal film resistors, perhaps caused by potting stresses, could result in fluctuation of the resistance.
Tests were performed on the PMT Test Circuit with the detector system. The connection at the PMT cathode of the first dynode resistor (R1) was erratically opened and closed. PAD threshold was set to 20. Very large numbers of counts were observed. When a resistor was placed in parallel with the switch, it was found that fluctuations in the value of R1 as small as 10 K Ohms (out of 1.33 Megohms) caused a few noise counts. These tests clearly show that a noisy dynode resistor is a possible cause of the flight PMT noise.
6. PMT Test Circuit Characteristics
Performance of the PMT Test Circuit was measured to verify that its behavior was similar to that of the flight PM'r Assembly. Dark count and light count (at low light levels) were measured at various high voltage settings, with the PAD threshold set to the normal flight unit operating value of 20. Average anode current was also measured. No dark or light counts were observed with the high voltage below 1700 Volts. The maximum signal to noise ratio was observed with the high voltage set to about 1880 Volts. At this setting, the dark count was about 10 counts/see, and the average dark current was about 3 nA.
PMT interelectrode capacitances were measured both directly with an RLC meter and indirectly by injecting current pulses into various electrodes. The equivalent coupling capacitance from photocathode to anode is about 2 pf, while capacitance between various other electrodes ranges from 2 to 7 pf.
7. Conclusions
32 HSP OV Report (Vl.0)
Two possible causes of the PMT noise have been identified: A discharge in parallel with the corolron and an erratic dynode resistor. The corotron instability at low current has essentially been ruled out. No other PMT Assembly has ever shown noisy behavior at minimum voltage, so it is clear that some kind of failure has occurred in the flight unit.
Although either type of failure is can producing the noise observed, the discharge appears more likely. Metal film resistors are generally reliable, and the potting material used in the PMT Assembly (Dow Coming 93-500) is a soft silicone that does no greatly stress components. But, this potting material does have poor adhesion characteristics, so it is possible that it has separated from the surface of the glass corotron envelope, creating a small void containing a small amount of gas released from the material itself. The voltage across the corotron could easily cause a discharge to occur in such a void. Because the dynode resistors are in series with the corotron, the discharge would not cause the HVPS to shut down when the voltage is set to the low end of the range. The change in count rate with time while power is applied could be a result of a change in pressure within the void caused by the heat generated by the discharge.
Tests performed so far have not replicated the increase in count rate with time observed in the flight instrument. This could be because the precise characteristics of the discharge path, or an erratic resistor, have not been duplicated. Of course, there still could be another unidentified mechanism responsible for the noise. If one assumes that one of the above mechanisms IS the cause, it is possible to evaluate the possible effects of further operation of the flight unit. If there is an erratic resistor, operation at higher voltage should cause no harm, and could cause the resistor to become more stable.
However, it appears more likely that there is a discharge across the corotron within a void in the potting material. In this case, operation for a longer period or at higher voltage could result in formation of a permanent conductive path across the corotron, which would render the detector inoperable. It is possible that there is some operating sequence that would clear the discharge path without damage, but further investigation is required to determine whether this is possible. Until such investigation is completed, we must assume that any further PMT operation presents a risk of permanent damage.
7. Further Investigation
Replication of the behavior observed in the flight PMT would greatly increase confidence that the true failure mechanism has been identified. The increase in count rate with time is the obvious characteristic that has not yet been reproduced in laboratory tests.
Because the discharge within the potted portion of the PMT Assembly is the most likely failure mechanism, further investigation should be directed toward producing this type of discharge. Models representing the corotron, and possibly other PMT Assembly high voltage components, would have to be potted and subjected to various types of thermal and mechanical stresses intended to produce small voids in the appropriate places. Since the flight PMT Assembly was potted about 8 years ago, aging of the material may be important, but there may be no way to quickly simulate this aging.
This investigation would be time-consuming, and there can be no guarantee of success. But, at this point it appears to be the only possible way to positively identify the failure mechanism, and determine if there is any way to restore the flight unit to normal operation.
Note: Subsequent to this report, the PMT was operated briefly at a higher voltage, 1900 volts, and no evidence of the "noise" was seen. Subsequent operations were restricted to voltages above 1900 volts and no further anomalous behavior has been seen.
33 HSPOVReport(V1.0)
Appendix C - PMT Bri__ht Oh iect Safint, Renort
HSP 1379 PMT Detector Dark Count test started as scheduled on day 231 beginning at 01:22:25 GMT. At 90:231:01:42:10 UTC HSP entered SAFE MODE due to Bright Object Protection. Analysis of the near real time engineering data shows VCVAMP5 at 10.34 volts just before BOP was tripped indicating that the PMT had been pointed at a bright target. Looking at the PASS HST Occultation Schedule Report, the V1- axis was occulted by the bright Earth at the time of safmg. Although HSP was not in a data collection mode at this time, the high voltage had been ramped to it's full operate level of 2184 v. Note that the V 1- axis was not occulted by the bright Earth at the Lime the f'trst data collection scheduled.
The PMT appearsto have behaved nominally.
HSP PMT SA.P'I[NG
14, Cvc-vam
-"'e'-- Bxilht Em_h •
tl, HVPS
8 10, /
4"
l-
O"
.-2 • . . o • - . . • leO0
The times of the significant events are as follows:
HVPS #5 ramped up to operate level 01:25:18 HST V1 axis crosses bright earth terminator 01:35:17
V374;VCVAMP5:
V374;VCVAMP5 = -0.25279999 S/C= 80237852. UT= 231 12010 V374;VCVAMP5 = 0.54701805 S/C= 80239292. UT= 231 1 23 10 V374; VCVAMP5 = 0.49702942 S/C= 80239612. UT= 231 1 23 50 V374; VCVAMP5 = 0.39705217 S/C= 80239692. UT= 231 124 0 V374;VCVAMP5 = 0.49702942 S/C= 80245292. UT= 231 1 35 40 V374;VCVAMP5 = 0.84694982 S/C= 80245452. UT= 231 1 36 0 V374; VCVAMP5 = 0.89693844 S/C= 80245532. UT= 231 1 36 10 V374; VCVAMP5 = 1.1968702 S/C= 80245612. UT= 231 1 36 20
34 HSPOV Report (V1.0)
V374; VCVAMP5 -- 1.1468816 S/C= 80245692. UT= 231 1 36 30 V374; VCVAMP5 = 1.0968930 S/C= 80245772. UT= 231 1 36 40 V374; VCVAMP5 = 1.9966882 S/C= 80245852. UT= 231 1 36 50 V374; VCVAMP5 = 1.2468588 S/C= 80245932. UT= 231 1 37 0 V374; VCVAMP5 = 1.1968702 S/C= 80246012. UT= 231 1 37 10 V374; VCVAMP5 = 1.3468361 S/C= 80246092. UT= 231 1 37 20 V374; VCVAMP5 = 1.1968702 S/C= 80246172. UT= 231 1 37 30 V374; VCVAMP5 = 3.3963697 S/C= 80246252. UT= 231 1 37 40 V374; VCVAMP5 -- 1.1968702 S/C= 80246332. UT= 231 1 37 50 V374; VCVAMP5 -- 1.1468816 S/C= 80246412. UT= 231 1 38 0 V374; VCVAMP5 = 1.2468588 S/C= 80246492. UT= 231 1 38 10 V374; VCVAMP5 = 4.1961880 S/C= 80246572. UT= 231 1 38 20 V374; VCVAMP5 = 2.4465859 S/C= 80246652. UT= 231 1 38 30 V374; VCVAMP5 = 2.7465177 S/C= 80246732. UT= 231 1 38 40 V374; VCVAMP5 = 2.2966199 S/C= 80246812. UT= 231 1 38 50 V374; VCVAMP5 -- 1.2468588 S/C= 80246892. UT= 231 1 39 0 V374; VCVAMP5 = 3.6463130 S/C= 80246972. UT= 231 1 39 10 V374; VCVAMP5 = 3.7962787 S/C= 80247052. UT= 231 1 39 20 V374; VCVAMP5 = 1.8967110 S/C= 80247132. UT= 231 1 39 30 V374; VCVAMP5 = 4.2461762 S/C= 80247212. UT= 231 1 39 40 V374; VCVAMP5 = 1.1468816 S/C= 80247292. UT= 231 1 39 50 V374; VCVAMP5 = 1.5967792 S/C= 80247452. UT= 231 1 40 10 V374; VCVAMP5 = 1.1968702 S/C= 80247532. UT= 231 1 40 20 V374; VCVAMP5 = 5.4459033 S/C= 80247692. UT= 231 1 40 40 V374; VCVAMP5 = 4.5960970 S/C= 80247772. UT= 231 1 40 50 V374; VCVAMP5 = 6.7456079 S/C= 80247852. UT= 231 1 41 0 V374; VCVAMP5 = 1.1468816 S/C= 80247932. UT= 231 1 41 10 V374; VCVAMP5 = 1.0968930 S/C= 80248012. UT= 231 1 41 20 V374; VCVAMP5 = 0.94692707 S/C= 80248092. UT= 231 1 41 30 V374; VCVAMP5 = 1.0469043 S/C= 80248172. UT= 231 1 41 40 V374; VCVAMP5 = 10.344789 S/C= 80248252. UT= 231 1 41 50 V374; VCVAMP5 = 0.99691570 S/C= 80248332. UT= 231 1 42 0 V374; VCVAMP5 = -0.25279999 S/C= 80248412. UT= 231 1 42 10
V340; VHVPSM5:
V340; VHVPSM5 = 1399.6000 S/C= 80237916. UT= 231 1 20 18 V340; VHVPSM5 = 1941.1608 S/C= 80240316. UT= 231 1 25 18 V340; VHVPSM5 = 2029.8647 S/C= 80240556. UT= 231 1 25 48 V340; VHVPSM5 = 2127.9058 S/C= 80241032. UT= 231 1 26 47 V340; VHVPSM5 = 2202.6040 S/C= 80241232. UT= 231 1 27 12 V340; VHVPSM5 = 2197.9353 S/C= 80241452. UT= 231 1 27 40 V340; VHVPSM5 = 2202.6040 S/C= 80241740. UT= 231 1 28 16 V340; VHVPSM5 = 2197.9353 S/C= 80242476. UT= 231 1 29 48 V340; VHVPSM5 = 2202.6040 S/C= 80242716. UT= 231 1 30 18 V340; VHVPSM5 = 2197.9353 S/C= 80242932. UT= 231 1 30 45 V340; VHVPSM5 = 2202.6040 S/C= 80243412. UT= 231 1 31 45 V340; VHVPSM5 = 2197.9353 S/C= 80243628. UT= 231 1 32 12 V340; VHVPSM5 = 2202.6040 S/C= 80243916. UT= 231 1 32 48 V340; VHVPSM5 = 2197.9353 S/C= 80244388. UT= 231 1 33 47 V340; VHVPSM5 = 2202.6040 S/C= 80244628. UT= 231 1 34 17 V340; VHVPSM5 = 2197.9353 S/C= 80245812. UT= 231 1 36 45 V340; VHVPSM5 = 2202.6040 S/C= 80246308. UT= 231 1 37 47 V340; VHVPSM5 = 2197.9353 S/C= 80246556. UT= 231 1 38 18 V340; VHVPSM5 = 2202.6040 S/C= 80246796. UT= 231 1 38 48 V340; VHVPSM5 = 2197.9353 S/C= 80247516. UT= 231 1 40 18 V340; VHVPSM5 = 2202.6040 S/C= 80247756. UT= 231 1 40 48 V340; VHVPSM5 = 2197.9353 S/C= 80247936. UT= 231 1 41 10
35 HSPOV Report (V1.0)
V340; VHVPSM5 -- 1399.6000 S/C= 80248440. UT= 231 1 42 13
Note the V374 output began to increase at the time of bright earth terminator crossing and varied over a large range until the sating event occurred. Variations in the brightness of the earth over a range of a factor of at least ten can be reasonably expected.
In summary, we currently feel that saFmg occurred due to a bright Earth occultation of the Vl-axis while HSP Detector 5 High Voltage was on and at it's full operate level of 2184 volts. As a result, the maximum current limit of 80% was exceeded which tripped HSP Bright Object Protection. The standing operating procedure for this detector must be changed such that it does not view the bright earth while the high voltage is at standard operating levels.
36 HSPOVReport(VI.0)
Annendix D - HST Flight SMS seauence
The flight SMS sequence is listed below. Interruptions in the "in continuity with", usually associated with safemode recoveries, are indicated by ******
901241k3 902287al 910497e7 901252kl 910567gl 901271mlr ****** 910637c2 901283m3 910707c6 901312m4 900332al 910777d4 901323 m6 902344a7 910847f2 901352m2 902384a6 910917bc 901363ml 902419a5 910987c9 901382m3 902494a6 911057d5 901392m3 902537ab 911127e4 901402m8 902607d2 911197b8 901413m5 900677ab 911267c 1 901432m5 902747bf 901452m8 902817b8 ****** 901463m4 902885a3 901482m6 902932aa 911276a2r 902957a9 911337c8 ****** 903027ac 911407ah 903097el 911477c3 901492n2 911547d3 901503n2 ****** 911617ca 901522n4 911687bg 901534p3 903104a2 911757bl 901562p4 903133b2 911827af 901584a8 903167b3 911897al 901613a3 903237cb 911967d4 901634aa 903307bgr 912037acr 901662b3 903377d6 912107b3 901673b2 ****** 912177d5r 901694a4 912247c7 901713b2 903422a3r 912317e2 901733b3 903447b9 912387cl 901753b2 903517e8 912457d5 901773b3 903587e7 912527e5 901794b6 903657d2 912597bl ****** 912667c4 ****** 912737c6 912807m 901882a3 912877dl 901893cl 912947b4 901915a4 913017b5 901953a6 913087d4 901974a3 910022air 913157aa 900005c8 9100Malr 913227c4 902045a9 910077c9 913297b7 902085ab 910147e4 902125e4 910217bd 902165b5 910287d2 902205a7 910357e7 902245cl 910427d6
37 -12-11 -10 -9 -8 -7 _ -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12 12 ,_,_.'._.'.i.'._.._'_i_',i_'_1.'_.'._*'._._*',_._._._._.'._.'_.'.1,_._._*_'_._`` 12
11 11
I0 10 0 _ _ _ 1_ 1_ 1800 2100 2_ 2700 _0 3300 3600 39_
9 4ooo 9
8 - 38OO 38OO 8 11-. CLRP A CLRP TX CLRP C _ 36OO O-- 0-- O- 36OO 7 CLRP_X 7 340O _PS 340O 6 6 o ILP 320O cLnn_T 3200 F216P 5 5 DARK31 300O 1B F216PO F216P90O F216P135 F216P45 3000 o o o o 4 4 F21( 28OO p_x 2600
3 3 26OO F216M 2600
2 F237P 2400 2400 2 F237PgO F237P135 F237P45 1C F237PO o I 0 o o - 2200 F23 'P_X 2200 1
0 - 2000 DARKll 2OOO 0 F237M o _oK2P -I -- 1800 F277P 1800 F277P135 F277P45 _ 1600 1D F277P0 F277P9O o -2 o o leoo _ -2 F27 )PX O 1400 1400 -3 -3 F277M 120G 1200 -4 F327P -4
IOOG F327P90 F327P45 1E F327P0 F327°P135 1000 _ -5 -5 o o o 8O0 F3_ P_X -6 6OO F327M
-7 4O0
4 -- 200
_F_T.I.J..=. I._. ,.i .,. =.l. =.=.1.= .=.l.=.l.I .,.= .I.,.[. t.= .=.1.=.= .I. =.= .I.= .i.I., i -9 -- _ER( 0 "-g - 300 600 900 1200 1500 1800 2100 2400 2700 3000 3300 3600 390 -'_ -10
-11 -11 ' Deflection stel_a 1 -10
-12 _'_'_`_'_'_'_'_`___`_`_'_`j_ -12 -12 -11 -I0 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 B 9 10 11 12 mm
_t_Ij_I_''''_''''_''''_'''_''''_''''_''''_''''_''''_''''_''''_''''_''_'_'_''''_'ll_I_II_ii_
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
IDT1/POL Data base names
Chart version 1.5 (4/30/91)
Jeffrey W Percival 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3800 3800 4000
4OO0 -- 40O0 -12 -11 -I0 -9 -8 -7 -6 -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12 12 ___i._._.______.___._____.______`_T______.______`______._____._`______" 12 38OO 3800 11 11
3600 36O0 10 FI22U1 CLRU1 10 2L CLRU1F 2M FI22UID FI22UI B FI22UI_A o 9 0 0 - 0 9 34OO FI22UIX 3400
8 8 F122M CLRuOI_ TX 0 3200 7 -; F248U1 CLRoUI_S CLRUI_X 7
,RK3UCLRUI D CLRUI_B CLRoUI_A 2K F248oU1_F F248U1_E F248U1 D F248oU1 C o O o 6 3000 6 oF248_J1 xO - - CLRUI_T 5 5 - F248M F140LP 28OO 28OO 4 - F218U1 F278U1 4
2600 21 F218U1_D F218U1C F218U1_B F218U1A 2J F278U1 A F278U1 B F278U1_C F278oU1 D 26OO 3 O O - O O O o - o -O o 3 F276Ul_X F218U1X 2 2400 2 - F218M F278N
F240U1 I - F184U1 1 22OO 22OO 2H F24OU1 A F240U1 B F24OU1 C F240U1 D 2G F184U1 D F184Ul_C F184U1_B F184U1 A o 0 o - o O 0 0 -6 - o -0 o - 0 F240Ul_X F184Ul_X -1 2000 -1 - F184W _W nAF LJ1 F_2OU1 -2 -- F145U1 -2 1800 1800 " 2E 2F F220U1 A F220U1 B F220UI C F220oU1 O F145U1D F145U1C F145U1_B F145oUIA o - o -0 o - - -3 o - o - O o F220Ul_X F145U1X 1600 -4 -4 F145M F220W
F152U1 -5 1400 ._ - F135U1 1400 2C 2D FI52U1 A F152U1 B F152U1 C F152U1 D 4" F135U1F F135U1 E F135U1_D F13_1_C='_ 0 -- 0 -- O 0 - 0 - -6 O - O - O O F152Ul_X 1200 F135Ul_X -7 "; -- F135W F152M
,F248U1 -':' 1_ 1000 4 = F135U1 -8 2A ZB F135U1A F248U1_A F248U1_B -9 4 -- F13$U1B O O O 8OO o - O O F248U1PX F135UtPX -10 -1 --F135W F248M
600 -1 -- -11 - ._._._._._._._._._._._'_._'_k_I_"_i_'_'_._._._._.'`_.'`_ -12 4OO 400 -I -12 -11 -I0 -9 *8 -7 -6 -5 -4 -3 -2 -I 0 1 2 3 4 5 6 7 8 9 10 11 12 mm
2OO
0 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
Deflection ste_os
Iltllllti,lttilli,liltlliltitillttlltililrittltlrllttitltlt illlltlllt,lttt tit tttltttlllt t,lil,tlttt il
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
V3 IDT2/UV1 Data base names
Chart version 1.4 (11/10/90) Jeffrey W Percival 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000 -"r"l-"l ' I ,-r' I ' r' I' i '-r"r"r" i , i '-r"l"r' 1'1' I' i '1 ' i , I ' r, i-,-i-,-i-,-r,-r, i "1 "1" I ' I, I ' i '1 ' i "1": 4OOO
38OO -13 -ll -II -I0 -I -8 -7 -6 -5 4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 I0 II 12 13 3800 -13 .__.]."__"_1_._._._._._._`_1_T_._._ 13 , - " r ] - ", 36OO 36OO
E
-1,2 . /F750-F320 / , 12 .11- /F320N,'F750W3" F750nF320 11 -- 3400 34OO
jo _,,oo,, _v CLRV J ,o 32OO 3M F400oV_D F40_VB F400oVA 3L o- ' 32OO -9 F40OV_X 9 ":,
3OOO "...8 F400LP DN: K3V cLROv-TX O 8 3OOO CLRV S CLRVT_X -7 F620V o - 7 - 2800 28OO .6_ 3K F62ov_oF%V_Co_%V_B_%v_, C_o_V-" cu_v__C_oV_E 6 _. . F620V_X
26OO -6 F620W F160LP 5 -- 26OO
-4 F551V F419V 4 " 2400 -- 3l F551V_F F551V E F551V D F551V_C 3J F419V_A F419V B F419V C F419V D 24OO _30 o-O o- o O o- O o- o . F551V_X F419V_X 3 _ 22OO 22OO -'2 F551W F419N 2 "-:
:I F450V F355V I ' 2OOO 2OOO 3(3 F450V D F450V C F450V B F450V A DAF l_ll_ F355V_A F355V B F355V_Co F355V D DA K2V -_ o- o- O o- o- -- o:^-_..7 o- _0 o F450V_X r _l_=v _^ , 1600 1_0 • -1 F450W F355M -1 .
1600 --I Fl_,V F,_0v .2 1600 .... 3E F,_,v_O_oF,_VoCOF'_'Vo" F,=V_A == CU_Vo_,CU_Vo_V.CL,Vx°-c CUqVo_D -3 : 1400 --3 F184V X - 1400
--4 FI84W FI60EP -4 . 1200 1200 --:5 F240V F262V -5 -
- 3C F240V F F240V E F240V D F240oV-C 3D F262oV- A F262Vo- B_F262Vu o- C F262oV-D _ • -6 o- o-o o- F262V X -6 ' 1000 -- F240V_X - -- 1000
"-7 F240W F262M -7 - 8OO 8OO r -8 F24OV F551V -8 - 3A F240V A 3B F551V_A F551V B - 6OO ".9 F240V B o- o O o - 6OO o - O F551VPX -9 - F240VPX ;"10 F240W F551W :-10 , 400 4OO
2OO ;--t2L.11 :'-._'_'_._'____`_`__i_i_i_i_-_ ---1112 2OO . -13 -12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12 13
)ElL I., .I .,.I.,. I.,.I. ,.i. ,.I.,. i. ,.I., .I .,.I.,.i .,. I., .i., .t.,.i.,.I .,. I .,m[_l.,.i. ,.I.,.i.,.I., .i., .t.,.i .,.t.,. i., .I.,. I. ,.I .,.I .,. I., .i.,.I.,.I .,.I .,.I., .I., : 0 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4(]00
DeflectiOn Itepl
__'''_''''_'''__'''__''_'_''''_''''_''_`_''''_'__'_'`_'_''''_''''_'_''_''''_''''_''''_iiii_iii__ii___
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc,seconds
IDT3/VIS Data base names
Chart version 1.4 (1 1/10/90) Jeffrey W Percival 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000 :;"J' I'l'l ''" I' '' I' I"I'' "1' ""1"'' I' I"I''' I"l' I 'l' I"=' I' I' I '1' I "1"1 ' F"I" F' I' I '1' I"1""1 4OOO •--j 4000 ,4 -I
-12 -11 -I0 -9 -8 -7 -6 -5 -4 -3 -2 -I 0 1 2 3 4 5 6 7 8 9 10 11 12 38OO -138oo 12 __'___'__i_`___ "'" 12 I
11 :" I1 I --136OO 36OO -I -I 10 F 122U2 _,LRU2 10
34OO 4M F122U2_D F122U2 B F122U2 A 4L CLRU2_F -I_oo 9 o O- o - 9 FI22U2_X O .4 ---132OO 32OO CLRU2 TX O 8 8 F122M CLRU2_S -CLRL_2T X --J 7 FI45U2 DARI 3U2 O 7 -4 3OOO .--q 3000 4K F,45oU2_F F145U2 E F145U2 O F,45U2 C O CLRU2_D CLRU2 B CLRU2 A , OF,45_j2 Xo - o - CLR_2°T o - o - 6 -1 2_0 2600 5 F145M F140LP 5 .] -t 4 F284U2 F152U2 4 26OO 41 F284oU2_D F284U2_C F284U2_B F284oU2 A 4J F152oU2_A F152U2 B F152U2 C F152oUZ_D --4 3 %84_2x° o-oFI52U2_X o- s -t 24oo 2400 2 F284M F152M 2 -t
220C 1 F278U2 F248U2 1 0 4G FJ78oU2_ D F278U2o-oC F278U2o- B F278oU2_A 4H F248oU2_A F248U2%-_xB F248U2o- C FZ48oU2_D 0 2000 F278U2_X DAR)_ 1 U2 DAR ° -1 I F278N o F248M -1 i 1800 -2! F160U2 F218U2 -2
4E F160U2 D F160U2 C F160U2 B F160oU2 A 4F F218oU2 A F218U2 B F218U2 C F218oU2_D -3 o - o - O o - - - o - O o - -3 _2' 1600 1600 F 160U2X F218U2_X o
-4 FI60LP F218M -4 ' 1400 1400 -5 F179U2 F184U2 -5
1200 1200 -6 14(3 F 179oU2-D F179U2_-Or F179U2BO F179°U2-A 40 F184oU2_A F184U2OFl_84_j2BF184U2_Cx° F184oU2_D -6 ': °F179U2_X -"
-7 F179M F184W -7 _' 1000 tOO0 -8 F145U2 F262U2 -8 - 8OO 8OO -9 4A F145U2 B F145oU2 - A 4B F262U2_Ao O F262oU2 - B -9 -- " o - O F262U2PX - F 145U2PX 6OO -- -I0 F145M F262M -I0 _. .. :_ -11 - 4OO 400 _. - _ -12 .,.I,,.I.,.I.,.I.,.I.,.1.,.I.,.I.,.I.,.I.,.I., I.,.I.,.I.,.I.,.I.,.I.,.I., I.,.I.,.I , I.,.t., -12 - -12 -11 -I0 -9 -8 -7 -6 -S -4 -3 -2 -I 0 I 2 3 4 S 6 7 8 9 10 11 12 mm -- 200 2OO
,.I., I ,I.,.l.,.I.,.I.,.I.,.I.,.j.,.I.,.L.,.I.,.I.,-I.,.L, I.,.t.,.I.,.I.,.I.,.I.,.t ,.=.,.I.,.I.,.I.,.i.,.I.,.I.,.I., l.,.I.,.l.,.I.,.I.,.I.,.l.,.I.,.I.,.I-, 0 0 0 200 400 600 800 I000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
Deflection steps
_1_1_j_1I1__tI__t_t__j_t_I_j_1_t_
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
IDT4/UV2 V3 Data base names
Chart version 1.5 (11/10/90) Jeffrey W Percival V2 -12-11 -10 .9 -8 -7 -9 -5 4 -3 -2 -1 0 I 2 3 4 5 6 7 8 9 10 11 12 12 _ - 11 11
10 L 10 • 0 _ _ _ 1_ 1_ 1800 2100 2_ 2700 N0 3300 3600 390( 9 m 4000 :______|______`______I - 4OOO 8
:,..- 380O 8 38OO 8
:_ 38OO 36OO 7 O O 7 CLRP A (_ C 0.65.-C 0.65-0 L.. 34OO 1A 1 3 MOO 8 8 F160LP 32OO 32OO 5 F216P 9O 135 45 5 - 3000 tB 1 2 o D; 3 4 3OOO 4 O O O O 4 - 2800 POLO POL O POLl 35 POL45 26O0 3 3 - 2600 F216M 2600 2 F237P 0 2 - 2400 9O 135 45 2400 1C 1 2 3 4 I 2200 O O O O 22O0 1 POLO POL9O POLl35 POL45 0 "-- 20OO 2OOO 0 F237M o DI oO2 -- 1800 1800 -I F277P 0 9O 135 45 -1 tD 1 2 3 4 '" 1600 1600 -2 m O 0 O 0 -2 POLO POL6O POL 135 POL45 '" 1400 1_0 -3 -3 F277M •" 1200 12O0 -4 F327P 0 gO 135 45 -4 ;" 1000 1E 1 2 3 4 1000 -5 O O 0 0 -5 :- 8OO POLO POL9O POL 135 POL45 800 .6 -6 • 600 F327M o D, 600 -7 m -7 • 400 4OO
.6 -8 ,.. 2OO 2O0
-9 ."" 0 I.l.l.l.l.l.l.l.l.l.l.I. 1.1.1.1.1. I.1..I.1.1.1.1. I.I.I.l.l.l.L.I.I.i.l.l.l.i. Ii, I o 2 -9 0 300 600 900 1200 1500 1800 2100 2400 2700 3000 3300 3600 3900 -10 -I0 Deflexion slepe
-11 -11
-12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 8 7 $ 9 10 11 12 mm
_t____t_t______t_
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
IDT1/POL Proposal names Chart version 1.6 (4/30/91)
Jeffrey W Percival 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
4000 - 4OOO
-12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8 9 10 11 12 12 12 38OO 38OO
. 11 11
36OO 36OO -- 10 F122U1 O B A CLRUI F 10 - 12M 1 2 3 2L 5 • O 9 34OO -- 9 34OO 0,4-B O4-A 1 0-A 0.4-E o 8 - 8 F122M 32OO 3200 7 F248U1 F E D C D B A 7 - 2K 1 2 3 4 1 2 3 3OOO - 6 • O • O 6 3OO0 oD30:-C O,:-D O 0.4-B 1.0-B 04-A 1.0-A I .O-C 5 5 F248M F140LP 2800 2800
. 4 F218U1 D C B A F278U1 A B C D 4 21 1 2 3 4 2J 1 2 3 4 26OO 26O0 3 o o 3 0.4-8 1,0-B0 0._-A* 1.0-A0 1.0-A O.;-A 1,0-B O.;-B 2 240o - 2 F218M F278N 2400
" 1 F184U1 D C B A F240U1 A B C D 1 1 2 3 4 2 3 4 22OO - 2G 2H 1 22OO 0 O 0 0+-B4 1.0-BO 04*A• 10-AO 1.0-A O.:-A I .O-BO O.:-B
2OOO -1 2OOO - -1 F184W F24_
-2 F145U1 D C B A F_OU1 A B C D -2 1800 1800 - 2E 1 2 3 4 2F 1 2 3 4 - -3 O " O • -3 O.:-B I .O-B0 O._-A• I .O-A0 1.@A 04-A 10-B 0,4-B 1600 1600 -4 F220W . -4 IF145M F E D C F152U1 A B C O -5 1400 _ -5 F135U1 1400 1 2 3 4 2D 1 2 3 4
. -6 2C O O -6 0.4-B 1.0-B0 O._-A• 1.0-A0 I+_A 0,_-A 1 ._B O.;-B 1200 +7 . -7 F135W F152M
1000 - -8 F135U1 B A F248U1 A B -8 2A 3 1 2B 3 I -9 O * -9 800 04-C 1.0-C0 10-C 04-C -10 - -10 F135W F248M 6OO , -11 -11
-12 400 : -12 4OO , -12 -11 -I0 -9 -8 -7 -6 -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12
- mm -.'. 200 200 _ -
0 0 0 200 400 600 O00 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 38C0 4000
Defkzclion itepl
IIII Ill II Ill,tit i, ii I,,i ,I, i, il Ii ii II II, I, ,l 11 II II Ill II II IIII 111 ,l,it_It,,tl,,,,l i,,,lll ,, Isllll ,, i,l
-50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
V3 IDT2/UV1 Proposal names Chart version 1.4 (11/10/90)
Jeffrey W Percival 0 200 400 800 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
;' I • I" I "l"-i" I ' I" I ' I "1 ' i ' I " I" I " I • I 1 I" ' I '1 ' 1 ' I ' I ' i ' I ' I ' I " I " I " I"''1'''1 ' I ' I ''1'' i'''l'''l'''l'''l " I "_ 4ooo- -'.4oo0
3800 -- -13 -12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 0 9 10 11 12 13 -- 3800 13 ,'"1" '1'' '1'' '1' " I' " I'' '1' "l"" I"'1 "' I" "1"'1""1""1""1'"1""1""1' "1' "1""1 "_' I'"1""1" "- 13
_2 - IFTs°-F_°_N xl -. _2 - _oo "11 F320N,,I: 750W O 11 - 3400 - A. - -- 3400 .10 F400V D B A CLRV J -- 10 _ 3M I 2 3 3L _ 5 - 3200-9 -- • O /f" T "_ -- 9 --3200 0.4-(3 0.4-A 1.0-A 0.;-E - -
,ooo-7) F620VF,OO pD C B A °3 H F E --- '7 -- 3o0o 2800 " 3K 1 2 3 4 , 2 3 " -- 2800
,' I- o.:.. o o;, 1,0-Ao o;.o 1.0-Co -- ' - 2600 ..5 I-- F620W F16OLP -- 5 -- 2600
24 I" F551V F E D C F419V A B C O -- 4 - 2400 - - 3! 1 2 3 4 3,J I 2 3 4 - -- 2400
'3 - 0.'-B4 1.O-BO 0.;-A ,.O-AO , .O-AO 0.;-A 1.0-BO 0.;-B --. 3 _
2200 -'2 F551W F419N -- 2 -- 2200
2000 _1 - F450V D C B A F355V A B C D u I -- 2000 3G I 2 3 4 D3['II I 2 3 4 - -0 0.'-B4 1.0-80 0.;-A I .O-AO 1.0-AO 0.4-A I .O-BO O.;-B :DD2 "-_ 0 - 1800 - -- 1800 -1 F45OW F355M "_ -I
1600 -',2 F184V D C B A F160V A B C D '_ -2 _ 1600 3E 1 2 3 4 3F 1 2 3 4 -_ -3 O O O O "_ - 1400 - O.;-B 1.O-8 0.;-A 1.0-A 1.0-A 0.;-A 1.0-B O,;-B ._ -3 1400 _4 F184W F160LP "_ -4 -
1200 -':5 F240V F E O C F282V A B C D -5 -- 1200 - 3c 1 2 3 4 30 _ 2 3 4 100o --6 O'-B4 I0 e o.,-A• 1o-Ao 1o-Ao o.-A: IO-Bo O.-B: - .6 --1000 "-7 F240W o F262M - -7 " 8OO 8OO -8 F240V B A F551V A B - -8 " 3A I 3 38 I 3 "_ .g 6OO 8OO .-0 0.--4-C O O ," - • 1.0-(3 1.0-C O..,-C 400' "10_ F240W F551W -- .10 _._ 400 •11 _" .11
200 -72 --`_`_`_`_.__`_'`_.'_`._'._.'`_'._._f```_`_`i_'_`_`_ .12 - 200 . -13 -12 -11 -10 -9 "8 -7 -6 -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12 13 0 ,.i.,.I.,.i.,.I.,.i.,.I.,.i.,.I.,.I.,.l.,.i _i_._i_i_._`_._.m_i_`i`_"__i_`_`_i`_`i_i_ 0 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
Deflection steps
_''''_''''__''__'ii'_''''_'_'__'_'___'_'_'_'__'_'__'_'__'_'____''_i_i__i_i__iiii_ii'__''___'''__'_'__ -50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
IDT3/VIS Proposal names Chart version 1.4 (11/10/90)
Jeffrey W Percival 0 200 400 600 800 I000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000 :.-r,l.l,-I,f-.-l-, I,l.I, I, u-, I , ,-,I,l,-I-, I" I" I'l' I"l' r'l'l"l" I'l' I-, l-,-r,l,l,l,l,l' r"l ,1'1'.1 4000 •-_ 4000 ] -12 -11 -I0 -9 -8 -7 -6 -5 -4 -3 -2 -I 0 I 2 3 4 5 6 7 8 9 10 11 12 3800 .--43800 12 _._._._._._._._.1.__._._._.`_._._._._._._._. 12
11 11 3600 J-
10 FI22U2 D B A C;LRU2 F I0
34OO 4M I 2 3 4L _ 5 • ; o // t
32O0 -1320o
8 F122M _ 8 7 F145U2 F E D C D B A 7 -_ 3000 300G 4K I 2 3 4 C D3 I 2 3 4 --1 6 O,4-B 1.0-B0 0.;-A 1.0-A0 0.4-C 0.4-0 I.O-C0 6 -t 2sc_ 260C 5 F145M F140LP 5
4 F284U2 D C B A F152U2 A B C D 4 --_ 2600 260C 41 1 2 3 4 4J 1 2 3 4
3 0.4-B 1.0-BO 0.4-A 1.0-AO 1.0-AO 0.4-A 1.0-BO 0.4-B 3 --, 2400 2400 2 F284M F152M 2
2200 1 F278U2 O C B A F248U2 A 8 C D 1 -_ 2200 4G 1 2 3 4 4H 1 2 3 4
0 O,_-B 0 0 0 • 0 0 2OOO 1.0-B 0.4-A 1.0-A 1.0-A 0.4-A 1.0-B 0.4-B -20oo
-1 F278N ( P;_4 8M -1 -" 18oo 1800 -2 F160U2 D C B A F218U2 A B C O -2 4E 1 2 3 4 4F 1 2 3 4 1600 1600 -3 0.;-B 1.0-BO 0.:-A 1.0-AO 1.0-AO 0.;-A 1.0-BO O.;-B -3
-4 F 160LP F218M -4 o -- 1400 1400 -5 F179U2 D C B A F184U2 A B C D -5 4C 1 2 3 4 4D 1 2 3 4 1200 1200 • o ; o o • o ; .,
" 1000 I000
4A 1 3 4B I 3 --800 8OO -9 0.4-C I .O-CO 1.0-CO O._-C -9
-- 600 6OO -I0 :I 45M F262M -I0
- -11 -11 -- 400 4OO -12 ___j___'___._ -12 " -12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0 1 2 3 4 5 6 7 8 9 10 11 12 mm 200 200
, L,.I.,.L,.I., I, I., I, I.,.I, I, I.,.I.,.L, I , j , I.,.i.,.I., i ,.I., I ,.I , L, I..I.,.I.,,, , I , I ,.I , I , I , I , I , I-, 1-, I , I ,J , I.,: o 0 200 400 600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600 2800 3000 3200 3400 3600 3800 4000
Deilection st_s
_'''_'I_'''_'_'_'_''_''_''''_'_j'_''_'1_''l_''_'_'_'_1_''_1'''_'_''_i1_'_ -50 -45 -40 -35 -30 -25 -20 -15 -10 -5 0 5 10 15 20 25 30 35 40 45 50 Arc seconds
IDT4/UV2 Proposal names Chart version 1.6 (11/10/90)
Jeffrey W Percival V2 c_ Q. Z Q 0 T E w C_d & -i c_ -r _r LL c_ _r c_ D- I- I- LU W LU It C_I ± UJ @ @ O @ @ O @ @ @ O @ @ C_ C_ c_ 8 c_ (/)
Q.
g
qr |
(/)
(s) C_J_io
L_
8
_rL_i
CY)
C'J Tm 0 0") 0
|
-o
I
_e C_ U3 C_ 0 a.
S
| >-
fQ
g
II
io
E p_ _d O iI C_ .-r Z LLI Z o & w, o?, _J ,,T _r LL r_ n,- n- r-l- rr I-. l-- i-" im j- cr_ 111 ILl LU
OJ LIJ 0 0 0 0 0 o o 0 0 0 0 o 0 0 c_ 0 0 oo
@ o.
crJ
g CO
oo
o
E
0 C_J
o..
c_
=E cs_
| _
0
E
O CTJ CI) Z 0 rr L._ Z t.L -1- & W & & i LL CC c_ n- n" fl II n- n- l- F- Im F-- I-- i-- l-- w LU LAJ ¢I) i,U 0 0 0 0 0 0 0 0 0 0 _J
I cL I _o c_
¢3) Ii
-o 8
c_c_
cD E C_ c_j c_ T-" 0 c_ 0 0 0 0 0 0 0 0 0 0 0 ______o o o o o o o o o o o _ _ i i _ i i
I I o_
S I I |
@.)
g
E
U')
0 o 0 ur, o (.9 8 e., Z OJ E w 0 0 "T o U. r_ m, n- n- n- oc _C n- n,- 8" i-. l-- _C F- i-- F-- uJ w ¢.r
0 0 0 0 0 O O O O O ._i i o o o ¢.)
8
,qr J I II (I)
I P,
b-r_
E cO P, _D O') O 0 Z LIJ Z & IJ.I IN "7 "F n- ft. i- h- C_ W W 8" < ?= W 0 0 0 0 0 0 ,..I o o o o o o if) I
I
g u
_o
I i m 1
0 I
J
I
8
_o
I I
m
i i
E c_
m 0
0 (9 Z c_ I.U Z w, LL IX: II 8" I-- I-- UJ I.U I,U 8"
UJ 0 0 0 0 0 0 --I
0-
8
8
5
8
8
E
0 o O. LL 0 L9 0 Z ,q. l.L (M {M 0 oJ & "T "7, 0 rr LL t CO rr rr n- & rr n" h- f- O0 h- l-- h- Ol UA LU (t) 0 0 0 0 0 LU 0 0 0 0 0 0 ..A O_ 0 o o o o o o o o 00
0. o o
$ 8
oo | o
_9
_o
w
8
E 0
O .o o =. .. =. i i oo uO E O9 ,.qo _o_ 0 O_ (_ Z E -7 11 a n" n" n," 8 F- F- (.0 UJ U.l uJ =E I-- 8" ,,( ± ,,( rr" W O O O O O O O (..) O O O (_ (.9 CO o0 a. 8 S m I ,N I 8 f_ 8 m m D J J E CO O O') 0 0 0 0 0 0 0 0 0 0 0 0 0 _ I _ I i 0 0 0 0 0 0 0 0 = = I i = i = I = = _ !1 I I I I I i ,i i, _o i I I III I I I ! ! I I : I : : :: :: I I • ,_ o, I I oo I I I I § c_O E O4 I.,C) 'T-- O 8 O3 o 0 0_ U_ o r, I.J.. z r,.D OJ 0 0 m- d: I- r_ I.IJ 0 0 0 0 0 0 0 0 0 0 0 ,..I o o o o o o o o o o o _9 ',_r _0 f_ _i _o o_ O_ E CO 0 Z ,_J ill z z & w Cb 0 17 t- rr _r LL O Y I'- C_J r_ 8 LL a- Z I-- I-- I-- C_ LL LL Limb LU LU Ill 8" n 0- & CL LU 0 0 0 0 0 0 ml O -I- -I- -1- -,r I a. $ qr C_ oo _J oo O_ _o oo O _o CJ C_J ,_ln- 0 oo 0 0. LL Z 0. LU Z O4 E & w, 0 0 c_J a LL rr rr c_ rr c_ c_ Z I-- I-- I-- I-- ID c_ iJJ ill W Q_ rr 0 0 0 0 0 c_ C_ 0 0 0 0 0 0 o 0 o o 8 r_ 0 o "l $ o LO 8 0 C_ rr cD -r CD Z CD rr LU Z 0 LI.I z & c_ LL rr n" rr n" rr Z I- F- I-- I-- I-- n,, LU W ILl 0 0 0 0 0 0 0 0 0 0 0 .-I o 0 o o 0 o C_ o o cD n .q. C_ C_ c_Jc_ L_ T _o oo C_J c_ LO CD 0 CO | I 0 (t) C/) _ue J_ 0") r,.rl m .row c') o c) o o 0 0 cD 0 c) 0 0 i,- 0 0 0 0 0 0 0 0 0 rrl _Q 0 e-I rrl m ITI -4 ,-I --I .-Q 0 _b TI ,.Q ,:a ,:o ,:o _Q _o ,-n _o 0 0 f_O f_O m z rn z G_ "/'1 0 (.0 O 0"1 "0 I ! ! ,O I . . [ __.o oo 0 c.O 0 O1 Oo Oo C I c_ _D o 0 im 0 0 0 8 0 0 0 0 0 ITI 9_ 9_ -n c_ g_ i'n ITI I'rl .-I .-I .-I _0 :0 _o _0 "11 0 o P_ rn z ITI G_ Z G_ -rl 0 CD .ink OJ _D OJ C C_ o c_ (,0 -I- -1- c_ C_ c_ o 0 "1- -r -I- 0 0 0 0 f- (D (D (D (D 0 0 0 0 0 ro "0 1) "U "1o "D -1- -I- (.D m I"1"1 CD c@ :D :D Do 11 :D DJ _D Do A c_ -n o o -I- c_ r1'1 -o (D o z -@ 'i- G_ v_ "1"1 0 _D cJD 0 0 C_ 0 S_ = ! c_ O Ul_r_ O_j1 c_ f q_ G_ G_ c_ c_ C_ c_ c_ cD r- 0 0 0 0 O 0 0 O 0 o f-n ..A _3 .8 c_ c_ m m m _h -I --I in -n _J -11 - n O 0 ,j r_ m z m 0 z G_ =rt 03 O3 Z rr Iii z, -1- ,y 0,1 0,1 I.I. rr rr rr rr rr rr rr t-- C/3 t-- I-- I-- I-- LIJ W 0 0 0 0 0 0 0 0 0 .-I 0 0 0 0 0 0 o 0 0 0 (D g 0. _Ou-J 0 _3 g oo -000 oo o o 0"3 _0 QO oo 0 O_ 0 0 0 CO 0 rr CO a. oJ & w, o o t-- I-- I-- I-- I-- I-- W 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 O_ 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 n II II 1 0_._- O4 0 C3 0. u. Z o. LU Z _r E & UJ oJ o4 o qo v.- a c?, _r °7, 14. rr" n- r_ rr rr n_ 4_ I-- I-- F- I-- I-- I.- _r UJ LLI LU _E m, m, _r <3) rl- (0 _E _E _E LU 0 0 0 0 0 0 0 0 0 0 ¢_ c_ ,J C) (.3 C3 (3 C.) (..) C_ 0 c_ (/) O _L g _r-..co (3 o4 _r c_3 .11,-= 0 o_ C_ 0. LL o. Z C_ E w o 0 -r LL rr qN rr Q_ rr 0_ c_ q_ hi- rn I-- )-- I-- ,< (rr) W w ± rr ill 0 O O O 0 O 0 O O c_ c_ C_ C_ D. c_ _J c_ c_J cJ cr_ ym 0 cO ,_ mm Po ,. o. C_ |b m. .t .. I, a. , • -m i t • Ji ,; gJ n_ gl :| om ,| - . . °n ii °• ,, o• ,. o, | ! • . .. al .... im i, ,i •l t_ =o II I i i| °', i I :E = __888 880088,, __ Q. LL o. =7 E w o 0 ,T D LL cr r1- O: n- h- t-r" I.- I.-- i-- I-- I.- ILl 8" Q} i.l.I LLI cq oC LJ.J 0 c_ 1..I 0 0 0 0 0 0 0 C) C_ (fJ el} / oo co w Or) .Q Or) (:) C_ O O_ LL _D Q. z .@ w, £ 04 "7 o o LL < rr d: 8. 8" I-- I-- I-- < I-- I-- I-- < I,.U I..I.I LI.I 8 < ± ± LU O O O O O O O O O O O O O o O o O o cD (.9 't I i 8 ! I I ! i I o 8 } I I I I ! o I | I ! I g O4 ..O CO LO I | O | _x Z _J 2: .--I Z LU Cr_j rr & w I- 0 (.,j i r.. LL 0 n" n- rr ,v, I-- I- h- o_ LL I'-- I'-- $ COCO > u_ c_ oO cO .T-m 0 0_ 0 Q_ LL 0 Q. Z _t q_ u_ oJ C_J E w o O C_J & c_J t_ II II c_ C_ C/) I-- D- Iw bn i-- I-- Cr III LU 0 Cr_ w rr CO W 0 0 0 0 0 0 0 O 0 0 0 c_ c_ 0"_ c_ o o c_ ab o _o q_ o_ c_J c_J Tm 8 c_ 0_ coco oO _o 0 O 0_ u.. Z (%1 C_ 0 0 C_J (%J E (%1 0 0 (%1 & "T I.L rr f_ rr II o_ rr < & c_ rr & j-- j- j-. t-.- I..- j- w tll L.U I.U C) C) 0 0 C) C) O 0 C) (3 0 O 0 J) c_ ...J a) (_ (.) (_ o. .-._o 8 S r_ ¢_ "_u') _co :=o | _2 0 _o_ C_ (%1 (3") T" 0 0 o0 0o o0 o0 o0 o0 o0 _ o0 o0 0o o0 I_ I_ I_ I_ I_ I_ __ I_ I_ _ _ I_ n ! l j • g I n i I U ! m | I I Q 8 _0 "5 " I -" i " I i oo i ii i B I I I I I | | x _o o_ I o I m -- _n 4, cO _n _ 0") 0 o_ 0 0,. u_ o Z 0 r_ oJ LL w o 0 o,J LL "T r_ & r_ r_ r_ r_ o i- I-- I-- I-- 1-- I-- I--' I-- 8 0 0 0 0 0 0 0 LI.I o 0 0 0 _1 o o 0 o o o o o o o _v I 0 m 0 _D | 0 w cO o 0 o n 0 O O i+, O C9 Z ,N oJ W o O ,+ ,,( n" 8" I-- I-- '_ w w w _ , OC W ,N O 0 O O O O O O O O O O O 0 O t O O O O O O O O O 0') O O O O O O O O 1 i II l _o 8 5 ',I" ! o r_ '5 II oo 0 oJ 8 0 c_ t ¢_1e9 g _ m __ i __ B e,i __ B __ B J D _ 0 ctJ "s i" m | _ m .._ oO 0 o4 0 m m 0"_ m m m 0 5 0 ¢;) 0 | .m ,D 0 O_ <+_+'_ _++++++ +..,++++++ii+oo++.., o_ o °_ +..,o+-i8 _+ o_+iio <..,o.__e,o +..,<++°<+ w +,., +t I _+ | t w ii + m T i i. _,_.. i m t t (Xl "O + 0 0 m 0 O_ ! oi ., ., 0. 0 In (/) ! 0 | == oo O4 0 | II II i.n 119 ii 'I"-- Od 0 0") 0 0 0 n I,J.. 6 0 _ x Z _ 0 _ 0_ _ W 0 0 od oJ 0 0 cq i I.LI 0 0 0 0 0 0 0 0 0 0 0") ,-I 0 0 0 0 0 0 0 0 0 o 0 8 88888° i a= 8 t_ O,lo$ 01_0 o.I I'-.- 0 O4 o4 0 Ob o 0 0 0 0_ 0 I.L Z (_1 ('Y o,I 0,1 0,1 ur 0 0 0 OJ ('y , , u. ,+ _: "7 "T "7 rr n" n" nr ,,_ ,,_ ,_ rr n" nr rr nr rr 8" I.-- I-- I-- '_ 0 _ (;) I-- I- I-- F-- I-- I-- Z 8 C) o er ILl (_ 0 0 0 0 0 0 0 0 0 0 0 0 0 0 o o o o o o o o 0 0 0 0 0 o I (..9 (.9 ! 0. 000_ Cy_ $ g cy CY_ | | | 0 o,J o,I o o') C.) 0.. ml OJ Q O & &.U OJ O 0 m O O Of, o. X $ ) (I) Or') 0') O m Od O 0 o 0 0 Ll- o 0 LI- o Z _ o.I 4- it_ OJ o 0 0 oJ fr n" r_ B" I-- I-- I-- I.- o CO o ILl 0 0 0 0 o o o o o o .J 0 0 0 0 0 _0 o_ 0 0 0 0 0 0 0 t/) oo oJ o o_ ! ! _4 | M mm | | | | | m l ,m ,, cO 09 n n 04 0 O3 o 0 i I o 0 0 0 0 0 0 0 0 0 0 0 0 ol _ _ m m _ .u c. o o o o o o o o o o o o _ _ -I- _ :z: 1 i 0 £0 =E g oo :0 : _ | : : | m = -oJ J 8 oo oO t.O 0"_ o_ 0 0") 0 0 0 0 0 0 0 0 0 1 a. u m m A qr eJ 0 (41 m m o ! I'_ o3 O4 0 _,_ o 0 Z _ -- _ W Z 0 0 , , ooooooooooooooooo,______ n j .... I I I I i | | | i i u o to r - u u n m m .. . • ...... l --7 ;', ;; ." ,. °. o I I o .7 _ I c_ .. =. , oo L Oa ,. == 0 u u oJ 0 C_ m mm 0',_" I | Q m | m m • | • -- B i m _W | W = m _ z II i _ m m n r-. m 0 m 0'_ o 0 o 09 rr o o tO _o_ oo _o_ __ o_oe_ o0 o0 o0 o0 o0 o0 o0 o0 0 o0 o0 o0 o0 o o o o o ol a c_ 0 0 i | | | i II ! 0 u) , , ° , § 0 m, °, ml ,, ,, °m oo .-: :: -.: :: t m • | 0 | .q o_ 0 o_ o O o _ _ _ _ _°°°°_ wwww_ 9 _oooooooooooooooooo_oaaooooooooooooooooooooooooo _ 0,. T 4 $ | • m I 01%- 4 m • m m _ B _ w w J _ _ -- ] | ------, Z Z ! I ,,_ n ..Q_01 o _0 o O n 1 o oo CO oo 8 O3 CO CO OJ 0 ,,_,i ,,_i l..iJ a 'm D. eJ o oo o,9_ l I I ! 0 0 0 oo w _ m _ o o _ _ _ , ,_ o _ _ _ _ _o __ ,,_ _ooooooooooooooooooooo__ __ == :l el I u -- $ _o_ o,i o u i i I _J_ r)'_r Oo oJ • m | ., °. I u u _ m i m| n im 0, ml Ii • m _ ._ | =s ,: u u m m .: : .. __ 0_ | p,...... F • . _. o_ oJ 0 o'_ o o_ 0 ' A_ , ,, _ << iI _W _o_ooooooooooooo_oooooooooooo ooo oooooo oo oooooooo o____ IIII_ 1 Q. ) il t_ m _ t/) i m m m i I m m m m m i I i e | | m | I I I ,I m | 0 t_ oJ 0 o3 0 O3 m 0 AA oo _ _ _<_ ooooo oooo_,_ _@IIIIIIIIII IIIII_ ]: .... | o w m o... II lJ ,, | _ • _Cd o .... ,, m. °... r,- : : O_ c_ : " C_ 000000 0oo00o Q. • . m Ii u ul II 0 I I I J .,.._ m m IN 0 i ! cO 0 Ob o v , 0 _ "_ ' _ 0 0 O,J 0.1 0 0 0 0 0 0 0 0 0 d) | | J5 | i 0 o | | | | 2_ '_ 0,,I I | oo I m 1 1 l 1 o,I II | 0 cO 0 A A 00_0 iii w _ zoo0 _ _ n- rr 0 _>> _ 0oooo0 0 0 0ooooosoooosooeeeee0 0 0 0 0 0 0 0 0 0 a a Q a a _ :__ | | | m • • w : _" .. _, m k. m | - _ wh m | m m m , F w I __ ... __ I ! I c_ _0 O3 0 0") o o °°°8888888888°° "I B' II : : l o .. ._ °. ,_ ! | | O4 ,. °. | w i_¢'4 W °. .. ,. ., .. ,, °. ,, °. ,, ,_ ,, 0 t_ CO 0 II m m m n I m _. I =; =L k,- .... "i "" l i I I I ,D ,, mu _n n_ I i I -E I I 8 I M nW T'-- 0 I m 0 o £L U. x _ oo _ _ _ _ i °_ i ooo0 oooooooooooooooO0 0 0 0 0 0 o _ _ o o o o 0 :: F I_ al II • _I iI |I |I_ I I I • I ...... " "" : " i I I I IIII ._ i ii :: n • i i ii _- -: o ii ii ii , , iI ° , .... I .... ,. o. • - ,, i • " I II I ICXl .. ,, i , .... I I I ii ,, mi ,7 i. ,, °l ,, ° ,, ii i ,i ii i. .I _0 i| ii "0 03 03 F 0 0") 0 0 O. I.I_ 0 o 0 0 c 0 I_ l i d: tl: _ ._ '-' _ >, > >- 0 0 0 0 0 0 0 o 0 [, I I I, U J m 04 O4 O3 0 0 0 a a 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 LO Or) 0 O_ O I.I- U) CO co --J Z (9 r_ I.- O Z O n.- o. LLI o,J o,I I.L "I" .,.:r " O CC O o O 0 _ __ h- 8- LL. o o -- _- rf I-- I-- Z _,, I.J. u. I.J- ' O Q. I_ 0- Q.. W o _ _ G0I GO U) (/) ,_1 O O O O O O O I I T -r tO o O O O O O o 0 I O O O O O O 5 i O u) u) _J0o "_0 o ! m II oJ oJ O O O_ . .II . , .. I I I J_ i (..) • w .. • . ° . c#) | | °. .. I I 8 | i I I I I I m ,i | | | I I j i II I m °. . . al ,, I al ,i I • 0 0 o 0 o o o _ _ k d _ _ _ i _ __' =88oooooo ooooooo S .. o , _ 8 = ii ,, ° ======i= =l == =. .. m m -, =, =, =, == °= .... |l =| m , • , , , | m| .- 0= ,= : ,= ,J m ! | : | | | ! "" ii | 0 0 == =, o o --I .1 || o. . . o. ,. ,q. c_ ,, 0. mm _| : • X , _- __ i, u. ml im ii im .. .. -- : _O l II m • im ;| i I ,m| m Ii im ii im | m O0 m i. i .i ; t D °I "" _" ° G. i , i l .! .. | | " 0 ¢/) | I ¢/) ! | oO -. == °... °. =. ,= =. ., °. .- -- .. ,= iii III ,, ,_ | =, ,, CO :- .-: ._. • .. =. i "(3 .0 | I O4 ! 0 (3") 8" i ,, i ,, .. -. ., .[ _. -- ;- | , ,_ .= =. • m i. . . . . il ...... h I I . I '; __ = I m ,_ • = .. r" m o | m r-.. i'_ D = 0 , . . . _ _ooo ) ii ii t mm im m : : : m •: "; • • ),m 1 I' 1I. • • f. m I .... nam nl m m I u u I • i i r)_:r I n, I, mm m -- .. Iii ii °- .. 8 , . Im ! m | • | m m m ),l,(_.a.,;r o_ I h "_ _m 0 "a a. 3: m Ill _ n • i .. D I 00 o i ,. m .. II im 4 -,I- n II II m i ,,q,. II II i o : • . B "l" mm iI m o. o o- (,0 L,_ 0 0") u;., o o _ _ _ 00 oo oooo_ooooo 1 I II l i sl i i i I Q. ,I I i -i .11 i | I i i i I I II i i e,i i i i I Ii i I I I I 0 o e_ c_ I I i i 8 N i ! i I ' I • _ • _ _'Z : = ! 0 I o o XXXXXOXX = __ I====X==_ = ... _O__ .... _8°°°°8888888888888o'o'ooo'ooo''oooo _ _ _ '10 o , ° . S ! .4,. .. e ]i _ .. i u ¢/3 -- o. | ! ..6- d= -i- , , u , , u _ = _ • = m I I I I I | | II i II I I I I I I I I I I ; , i I I 4 II 'f I • = ._= 0 r,,- ,.p. : co _) =_ c) o'J 0 o 0 W W W W _ _ _V rr _" rr 0 0 <, <, <, <, _, _, . ,.,' i&,-,' ,., &&&,-,' ,., ,-, _.. oooooo 000000 ooooooo 0000ooooo, _ _ I I I I III I I III I I _ ._= , I i I I | I I • .... o. I || I S D_ ;.!. ) 0 o= .. ,= ,, i _ ,, ,m =,., R i 11 i, ,, .| • = o m m • m ,. I I =m .= m m n , m _ ] | .... •J _M .w • m .. .= o. u o o o ,r=. a. m m : m i el el E t,o m m l l m m o L m ,. m m ) ) l ) q m m m "(3 C) ,,r-- i 8 4 .... el) o. _. g .... ,i ,i ,, ii i ! ! i ,, _ o. , , o. Ii • .. o. o gl I| ii ii i- q, ii -: -.= ., o. _ k I -- ,.w 04 ii 11 ,w#... r.-. ,,_ co o 'T'" (_ . m ) • | m ) X m • "m n _ m • _ i r- | | _m ) .; l 0 ° .... | °m °. k. .... ! a. m . N i; ,m qm , • "S S; .... m m m m 0 I',-. @--- 0 win,n o 0 AA _ooo o ooooooo oooooaooooo , i" ==== = | | i | a i _o | _ ,....,co i__..v.c0 | i i l Oo (/) q , i I i Cs,lOd i o i r m i i i : i i I i i I i : I I : I i i i I D 0 '.0 | | ! • _ [ I O_ | I rO h- i F cO F" Cb _ (D [ , = "s"-" ! I (_ o b _ , cc cc 0 mmmmm__m m_mmm_ O0 o o o°8888°°°888°°°°°°°88oooooooooo m 0 , m ° , Z:;: 0. i . . .:I: I :]: eJ | 0_'_ J o , . i m .v.o_ | | | | R m B , , n i , m m n , , I_t_ n . , _o_ _O | • ! | _ .._ .,.it- .J tO i "0 t_ 0 ,%,.... O_ & ur, -I- 0"_ 0o 0 0 0o 0 0 0 0 0 _ 0 0 _ o o o o 01 c_ _ .-I0_ | | | m • ii "l 0 =I a0 | ! o,I 0") II .. :. l" m m | | e,i t_ m u -w." , , o o =m ,p B _ i • =| q= 4 ii ,= m q_,_"_r ml n, ,. .m m D ,, =J • i m m ,t i= ,, == =, ,, cO .13 II o 0 _ooo8oooooooooooooo000 00000000000000 o,_ ) . o . . m , m • e , | I el | • m , • • 7 -:i 1 ) 0 p e =. =E m I O0 =. ,, i °...... .. a 00 .,_- M i I i m i I I 0 oo _ _ _888ooooo ooo I | I I .... j m B m _ w .D ,, _ I I I .. ., l I CO P_ I it an an n IN n . ml ¢'1 o,I i i II 8 .= 0 ii • ii | ID ,. a. _ w =m m, . -- I .... i cO o. : 0 o3 o3 m .r m 0') (3 0 0 ( ( 4 a (_ ,m • I I ! • ! | Q. i i • . i . • I i a | . , Q I ! I I ! I a a i I i i . _ I m m ! I I I i | i m | I ! ! I i u i I I I u t : | | I | r , ! 1 I .E (If I',,. (:3 • i I I i 1 I i (:b _ __ _ooo ooo 1 o. _ooo8i°I ' _ _.. i. _0 I ct_ I: • II _O 4_. =w ml O. al aJ | | | • | =, == l .1_ ¢0 ¢.0 • m , , , ,m =m • , gl , , wl Im _tO ...... , ...... ° , ,m •D ,m mD ,. =. • wm C, ) ! % I I = ,, 8888888888 °00 __oo ooo8_oo8_°°°i o _mm _x xx_ _ 0 i I I C_ --d 8 8 ._D I'OO_ | | II !E m_l G_ • II B ro | • I | O .I_ "--: ¸ 8 O _3.. d 8 m O w. I • -o "I II II f_ "5 f_ UN i. i, • i i. i, iw aw o. .. II iw iw m, ,, .-= :: ..... m 4, ml o, im mm Im i m n • NI • DI c_ c_ 18 Q. .. o. I .... 4, '' r4 IJ IE e" .-- n .--- O im i, °, ,. II a, O, .. {o .... 4i e" ID I" II B m m ,. °, a -- | := :: .. °p : ; .... , . .. °. q, O_tt) i in ,, "l" "r =t- ::It- ::It: | ..... °, ,, e _ i ..... | I I 13 (D ,, m. O o _o8o ooooo o o 8 o o o _ _ a _ _ • ! . 1 ' #,. ,N °. °. ID I. f_ II o. .. I i. mn iJ ,, .. o. p" e0 ,, Jn m .. ,, mw In II ii i. O3 O O4 ,I O') o t,,, 1.1.. i.bl 8 n.- ,, ::?, oJ0 '_' 0,1 & <, !" t_r I-- | 1.9, 0 69 -- 0 0 0 0b ,,1,- 0 o o o -r -I- 0 8 8 8 8 °o °o 8 . ; ,4 D.. I e') 0 t_O !_ cO 43 0 ',1"-" 04 "11-- o _ c_ c_ 6 ct_ | _ L_ "o r_ i ! Tin. 0 0 _A 0 Eoooo_0000_000000000000_ oooooooooooo_ "m n | • ,, q, ." '.2' '-- J_ -- w i i g) m J -- o i i l n m " o n m .. am m| m. I m .... k O4 | CO m C_J _u a, _, i 0") ! . . . ° • . I i i | | i | | i I I I = -" 0 11 m a m • _ - _ ., f " • w == 6 " m m • . m . , . op • | ,, u, ,w = IN IN | m | i, i, i 0= =. • m =. I -- -- _= ., 0. • , o t_ m CXl (J cL LL o_ oo_ii__ ii _000 000000 00 80 00Q _ _ a ______+I , . .. .. 'I + ...... ..... , , ° °. ml I , _ ii ii i i ii i| i + ,m ml IN ,, o. g m .. , , .m m In Ir |1 _1 .L II ,, ,_ ii ii 1 D. 3= ii |1 q. .. I °. .. ii lJ i. +J = r I+ ii L i+ i. ii Iv +. ,, ii as _-_._ i" " ' 11 ii q, i. m m r .(3 p,. °, I. (_ L_ a, im T_ (_ o= , i • I ;I{ !! .... = 8 °1 °i • " , , i. ,i o, .= ,i o, I I • i . I °. ., I i I .... =1 , , o= i, . m m r v- I | • I "" ii II | I I • • = , _ == N, / ..... = I-., -- i, C_ .1=... i -| , , ii|1 , i iii o o _ 00 088000 |I o. | | i i .j{Q L) =E i i • | 1 : : | | , : l I I i -- D I I I I I I i i _=_ _== a i i m __ i _ i , , i i , cO m b- Cq u , , i , , O_ (3_ OOOOOOOOO = = :',v _ _-F • I t .... i .... _ i II ; ..... el ,, n, 0 i • u, =J =E 69 u _ in ...... • _ ...... i ..!- ! _ == II m R 4 .... ,, == I .,- _; .u I i 4 i I | 0)"_ '_._ "_ ,, g. I I I II I 4 I HI om 0 (3O £'M _r_ o_ 0 o o o o o oo88 o°o o o o 8888° = 1 o. I I m B ra I, ,L I 8 I ! " i, ,, 0 i _ -q . I | I I I I l I I • J 4 | I _3 °. =. u b ',,_lr 1 I • a. ,. u. ,, u m • L .j o. .. "t3 r_, r-- | co i m @a o_ 1 o. t :-_.::,_:. • =. .. I • I • g" I w e_ _8 8 == .. , , 0 (1) _,. .... _. ,...... ,. m I I ..... I l | | ,. ., I I1" °' II ii .(3 r" r-. , _ ,i ii o_ .i im ,, @4 _r_ O) "m o. }, ¢,p ,= ,, 0 T p- .. °+ __ T .Q i'-, 0 CO .s=..= 0 0 I-- I-- ¢'_ I-- I,- _ 0 0 0 0 0 0 ._1 _, o o o o o o 0o 0o _ 0o _ a n . I . I n q 0 ._ _g_ °_o_ i i , | n m | w I I | "0 I'_ cO 0 cO : I I i I o _..,,.T_._.=_ _.,r i _ _0_._ _' o o o o o o o o o o i _ _, _ F_ _,oooooooooooooo '11 I :: ."; _. _ _ e, ,N f/) =: z m_. mD °, _ g, i _ o i i i i .. _ h. ii i _, _. D ,. ..:_- • i m m b_ cO o _-, o o o0 o0 ooooo __ am I am i i il il i i • 1' ip i I I I .m ' ' ' " .L Hi i_ |a >_ I I m o. ,_ ,, im B m ! ii i, -. _ 0 CO F REPORT DOCUMENTAT!CJN,PAGE OMBForm Appcoved . o7o4-o1 Publicreportingburdenfor thiscol)ectlonof In_ormEIonb intimated to averageI hourper response,Includingthe timefor reviewingInaructlons,zearch_g o_latlngdata sour(_l, gathorlng andmaintainingthe dataneeded, andcomplattngand reviewingthe collectionof inlormatton.Send oommants regardingthisburden e_lrrmle or any o(Imraspect of thiscollectionof information,includingsuggeetioflefor reducingthis burden,toWashingtonI-leadqtMulemServk:m,D(mctorale/or I_lormatlortOperationsand Re_, 1215Jeff_lcm Davis Highway,Suite 1204, Arlington,VA 22202-4302. and tothe Office o( Mana_lemo_tand Bud_, paperworkReductionProject10704-0188),Wmhin_o_, DC 30503. 1. AGENCY USE ONLY (Leave b/ank) 2. REPORTDATE 3. REPORTTYPE AND OA¥_._ COVERED November 1991 Contractor Report 4. TITLE AND SUBTITLE 5. FUNDING NUMBERS Hubble Space Telescope High Speed Photometer Orbital Verfication Test Report NAS5-24487 6. AUTHOR(S) Evan E. Richards, HSP Program Manager 7. PERFORMING ORGANIZATION NAME(S) AND ADDRESS{ES) 8. PERFORMING ORGANIZATION REPORT NUMBER Space Science and Engineering Center University of Wisconsin - Madison 1225 West Dayton Street Madison, WI 53706 9. SPONSORING/MONITORING AGENCY NAME(S) AND ADDRESS{ES) 10. _I_IG AGENCY REPORTNUMBER National Aeronautics and Space Adminislxation Washington, D.C. 20546-0001 11. SUPPLEMENTARY NOTES 12a. DISTRIBUTION/AVAILABIUTY STATEMENT 121). DISTRIBUTION CODE Unclassified-Unlimited Subject Category 18 13. ABSTRACT (Maxknum 200 words) The purpose of this report is to provide a summary of the results of the HSP Orbital Verification (OV) tests and to report conclusions and lessons learned from the initial operations of the HSP. The HSP OV plan covered the activities through fine (phase III) alignment. This report covers all activies (OV, SV, and SAO) from launch to the completion of phase III alignmenL Those activities in this period that are not OV tests are described to the extent that they relate to OV activities. 14. SUBJECT TERMS 15. NUMBEROF PAGES 120 High Speed Photometer 16. PRICE CODE 17. SECURITY CLASSIFICATION 18. SECURITY CLASSIFICATION 19. SECURITY CLASSIFICATION 20. LIMITATION OF AB_I HACT OF REPORT OF THIS PAGE OF ABSTRACT Unclassified Unclassified Unclassified Unlimited NSN 7540-01-280-5500 Standard Form 298 (Rev. 2-89) Pr_cdb*d by ANSi _ 2ss-le, 2M-lo2 2..-