SMOV4 CLOSURE REVIEW
INTRODUCTION
Carl Biagetti/STScI
SMOV4 CLOSURE REVIEW AGENDA
SMOV Closure Review - Agenda
Biagetti
Introduction
John Wirzburger
PCS
Greg Waldo
EPS
Josh Abel
TCS
Coffee Break
Susana Deustua
WFC3
Tony Keyes
COS
Linda Smith
ACS
Lunch Break
Charles Proffitt
STIS
Ed Nelan, Matt Lallo
OTA/FGS
Keith Noll
ERO
Tommy Wiklind
NICMOS
Biagetti/Burley
Summary
Champagne Reception (Café)
Duration
Start Time
End Time
0:15
0:15
0:15
0:15
0:15
0:30
0:30
0:30
0:45
0:30
0:15
0:15
0:15
0:15
1:30
9:30 AM
9:45 AM
10:00 AM
10:15 AM
10:30 AM
10:45 AM
11:15 AM
11:45 AM
12:15 PM
1:00 PM
1:30 PM
1:45 PM
2:00 PM
2:15 PM
2:30 PM
9:45 AM
10:00 AM
10:15 AM
10:30 AM
10:45 AM
11:15 AM
11:45 AM
12:15 PM
1:00 PM
1:30 PM
1:45 PM
2:00 PM
2:15 PM
2:30 PM
4:00 PM
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
Page 14
Page 26
Page 34
Page 41
Page 87
Page 169
Page 198
Page 238
Page 257
Page 262
2
SMOV PLANNING
SYSTEMS ENGINEERING PROCESS
FLOW
SMOV CONCEPT STATEMENT
SMOV Mgmt Team
REQUIREMENTS DEFINITION
BASELINE PLAN
(ACTIVITIES)
STScI SMOV Team, 441 SMOV Planning Team
STScI SMOV Team, 441 SMOV Planning Team
PROPOSAL SUBMISSION
STScI SMOV Team, 441 SMOV Planning Team
PROPOSAL IMPLEMENTATION
OPERATIONS PLANNING
SMOV OPERATIONS
STScI Proposal Implementation Team
SMOV Ops Working Group, 441 SMOV Planning Team
SMOV Ops Team, SMOV TTRB
(& SMOV CLOSURE)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
3
SMOV CLOSURE PROCESS
•
•
•
•
Requirements baselined Mar. 2007
Plan baselined Oct. 2007
Plan executed May – Oct. 2009
Requirements adjudicated – today
– Agree on a path forward for any unsatisfied
requirements
– Send comments to Biagetti and Burley
• biagetti@stsci.edu
• rburley@hst.nasa.gov
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
4
SMOV4 INFORMATION
• SMOV4 Web Page at
http://www.stsci.edu/smov/smov4.html
– SMOV4 Requirements Review, 21Mar07
– SMOV4 Project Review, 12Oct07
– SMOV4 Status and Planning Meetings (“Morning
Meetings”)
• Meeting Notes
• Supplemental files
• SMOV4 Plan Document (Baselined Sep. 2008)
– SMR-4029 HST SM4 OBSERVATORY VERIF. PLAN
• Sec. 4 = SMOV4 Requirements Traceability Matrix
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
5
SMOV4 Level III Requirements
Document -- SMR 4029, App. L
ITEM
REQUIREMENTS SEC.
=========
===================
WFC3
L.10.4.1
COS
L.10.4.2
ACS
L.10.4.3
NICMOS/ NCS L.10.4.4
STIS
L.10.4.5
ERO
L.10.4.6
OTA/FGS
L.10.4.7
PCS
L.10.4.8
DMS *
L.10.4.9
I&C *
L.10.4.10
SIC&DH *
L.10.4.11
S&M *
L.10.4.12
TCS
L.10.4.13
EPS
L.10.4.14
* No SMOV requirements identified.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
6
SMOVs 2 – 4
EXTERNAL ORBITS
HISTORICAL COMPARISON
SI/SS
WFPC2
FOC
Spacecraft/FGS
NICMOS
STIS
ACS
WFC3
COS
ERO
TOTALS
SMOV2 SMOV2 SMOV3B SMOV4 SMOV4
PLANNEDACTUAL ACTUAL PLANNED ACTUAL
46
77
31
15
15
69
61
41
81
79
194
285
77
34
15
205
267
14
21
19
186
38
28
163
152
196
250
72
75
70
90
91
601
780
419
623
634
Notes:
1. In SMOV2, STIS and NICMOS required more orbits than planned because of
the NICMOS thermal short and the opto-coupler resets in both SIs.
2. SMOV4 was the most complex in terms of realtime interactions and in-line
analyses.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
7
SMOV4 REQUIREMENTS
SUMMARY
TOTAL
SI/SS
RQMTS
PCS
8
EPS
2
TCS
1
WFC3
23
COS
46
ACS
17
STIS
22
OTA/FGS
13
ERO
1
NICMOS
16
SI
1
150
MET
8
2
1
23
46
13
22
10
1
5
1
132
PARTIALLY
MET
NOT MET WAIVED
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
4
0
0
0
0
0
3
0
0
0
3
3
5
0
0
0
3
3
12
Note: NICMOS SMOV curtailed due to SI C&DH anomaly.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
8
SMOV4 EXTERNAL ORBITS
SMOV4 EXTERNAL ORBITS & ENABLE DATES
- Including EROs May 11, 2009 Launch
ERO
BEA PERIOD (1st 3 weeks)
AVAILABLE SCIENCE ORBITS
FGS
PCS
NICMOS
STIS
ACS
COS
WFC3
90
80
60
50
40
30
20
10/19/2009
10/12/2009
10/5/2009
9
9/28/2009
8
9/21/2009
7
9/14/2009
7/20/2009
6
9/7/2009
7/13/2009
5
8/31/2009
7/6/2009
4
8/24/2009
6/29/2009
3
8/17/2009
6/22/2009
2
8/10/2009
6/15/2009
1
8/3/2009
6/8/2009
0
7/27/2009
6/1/2009
0
5/25/2009
10
5/20/2009
ORBITS
70
10 11 12 13 14 15 16 17 18 19 20 21 22
F1 - FGS1R science enabled
F2 = FGS2R2 enabled for guiding
CD – SI C&DH failure
O – Secondary Mirror adjust
J – Jupiter Impact observation
L – LCROSS observation
SC – STIS CCD science enabled
SM – STIS MAMA science enabled
AS – ACS/SBC science enabled
AW – ACS WFC science enabled
WU – WFC3 UVIS science enabled
WI – WFC3 IR science enabled
C – COS NUV/FUV science enabled
SMOV WEEK
F1
CD
AS
SC
F2
AW O WI
WU
J
SM
C
L
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
9
SOME SMOV4 SCHEDULING STATISTICS
(NOT INCLUDING NICMOS SMOV)
•
32 SMS Product distributions
– 22 regular SMS deliveries
– 4 redeliveries
SMS START DATE
– 6 intercepts
09.140
20-May-09
09.142
09.145
09.152
09.159
22-May-09
25-May-09
1-Jun-09
8-Jun-09
09.166
09.173
09.180
09.182
09.187
09.194
09.201
15-Jun-09
22-Jun-09
29-Jun-09
1-Jul-09
6-Jul-09
13-Jul-09
20-Jul-09
09.208
09.215
09.222
09.229
09.236
09.243
09.250
09.257
27-Jul-09
3-Aug-09
10-Aug-09
17-Aug-09
24-Aug-09
31-Aug-09
7-Sep-09
14-Sep-09
NO. OF
DELIVERIES
COMMENTS
1
1
1
2 Intercept - Correct exp gain setting in 1138405
4 ReDeliv#1 - COS FUV visit misscheduled around SAA
ReDeliv#2 - Remove all ACS/WFC + gs change for 11458D2
Intercept - Add back ACS/WFC 11371 & 11510
1
1
1
1
2 Intercept - Pull all STIS after 191:14 + updated COS instructions
1
3 ReDeliv#1 - COS instruction update
Intercept - Observe Jupiter Impact
2 Intercept - Replace COS 1148703 to prevent local rate check violation
2 Intercept - STIS MAMA2 limit change on rampup to prevent suspending
1
1
1
2 ReDeliv#1 - Remove use of TDRS-S
1
1
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
10
SMOV4 TTRB ACTIVITY
TTRB MEMBERS: Biagetti, Burley, Niedner, Sembach, DCTaylor
5/18/2009
5/22/2009
6/1/2009
6/2/2009
6/3/2009
6/29/2009
6/30/2009
7/1/2009
7/7/2009
7/8/2009
7/29/2009
7/30/2009
8/3/2009
8/3/2009
8/3/2009
8/4/2009
8/4/2009
8/18/2009
8/24/2009
COS
ACS
STIS
ACS
STIS
WFC3
COS
WFC3
STIS
COS
ERO
ERO
COS
COS
COS
COS
STIS
COS
COS
FUV door open request
Revisions to SMOV Prop 11510
TTRB justification for 11384 visit 5 change
Visit deletion from 11510
Request to SMOV TTRB for changes to proposal 11389
Request for repeat of SMOV 11435 visit01
Additional visit to 11468 COS-to-FGS Alignment
Request to add POSTRG to Proposal 11426
Focus check
Request to activate 11469 visit 95
Request to repeat failed orbits of 11502
Request additional orbit of Omega Cen
Changes to 11491 COS FUV External Flat Fields
Changes to 11492 COS FUV Sensitivity for uniformly spaced lamp flashes
Changes to 11492 COS FUV Sensitivity Lifetime Adjustment
Request for additional 1147104 orbit - NUV Imaging Acq
Request for additional darks
Request for additional internal orbits for 11488 FUV Wavelength Verification
Additional FUV more dark visits at new, lowered gain
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Approved
Not Approved
Approved
Approved
Approved
Approved
11
SMOV4 BRIGHT EARTH
AVOIDANCE/EXPOSURE
•
Bright Earth Avoidance (BEA) Constraint (CCR 08-026)
–
21 days from Release
•
BE exposure allowances
–
–
–
–
•
Week 1 = 2 hours (for Deploy ops)
Week 2 = 2 hours
Week 3 = 4 hours (not contiguous)
Week 4 – No constraint, but no “prolonged” anti-sun pointing
The following is the flight bright earth exposure following release from SM4 (Information supplied by Merle
Reinhart).
•
–
BEA Week 1: Release to 2009.146:13:00:00
•
–
Total Bright Earth Exposure: 0.50 hours
This is due to SU 1137201 ACS/SBC used for the initial end-BEA check
BEA Week 3: 2009.153:13:00:00 to 2009.160:13:00:00
•
•
–
Total Bright Earth Exposure: 0.00 hours
BEA Week 2: 2009.146:13:00:00 to 2009.153:13:00:00
•
•
–
A 5.0-degree bright-earth avoidance angle was used for the calculations.
Total Bright Earth Exposure: 0.41 hours
This is due to SU 1137202 ACS/SBC used for the final end-BEA check
First post-BEA bright earth exposure was at 2009.162:04:06.
•
SU 1146801 COS08 COS/FGS Alignment
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
12
CROSS-SI LIGHT LEAK TEST
•
SMOV4 REQUIREMENT: L.10.4.2.1.12 (L.10.4.16.1)
– SMOV4 Light-Leak test
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS37 (11515)
•
DESCRIPTION OF METHODS
– a set of external exposures designed to determine whether a particular SI is
susceptible to light leaks resulting from photons escaping from the calibration
system of another SI. For a specific combination of SIs, the SI assumed to be the
light source carries out a calibration activity while, in parallel, the other SI
performs an external exposure.
•
DESCRIPTION OF RESULTS
– Initial positive detections in ACS and WFC3 all proved to be unrelated to a light
leak from another SI.
– Analyses led to discovery of internal glints, etc. in ACS and WFC3
•
SUPPORTING DOCUMENTATION
– See SMOV Meeting Notes, ACS Update of Sep. 3, 2009
• “Review of ACS-R Performance During SMOV4”
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
13
Pointing Control System
John Wirzburger
CROSS-SI LIGHT LEAK TEST
•
SMOV4 REQUIREMENT: L.10.4.2.1.12 (L.10.4.16.1)
– SMOV4 Light-Leak test
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS37 (11515)
•
DESCRIPTION OF METHODS
– a set of external exposures designed to determine whether a particular SI is
susceptible to light leaks resulting from photons escaping from the calibration
system of another SI. For a specific combination of SIs, the SI assumed to be the
light source carries out a calibration activity while, in parallel, the other SI
performs an external exposure.
•
DESCRIPTION OF RESULTS
– Initial positive detections in ACS and WFC3 all proved to be unrelated to a light
leak from another SI.
– Analyses led to discovery of internal glints, etc. in ACS and WFC3
•
SUPPORTING DOCUMENTATION
– See SMOV Meeting Notes, ACS Update of Sep. 3, 2009
• “Review of ACS-R Performance During SMOV4”
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
15
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.1
– Following release, the HST Pointing Control System will be returned to normal
operations for SMOV with four gyros in the active control loop, (no shadow
mode). A fine attitude reference will be uplinked to the spacecraft and the
spacecraft will be maneuvered to point to the BEA attitude. The gyro biases will
be determined and maintained to within 0.014 arc-seconds per second to allow
successful guide star acquisition at the transition to the Science SMS.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– PCS-01, PCS-02, PCS-03, PCS-04, CP-154, CP-167
•
DESCRIPTION OF METHODS
– Coarse Sun Sensors used to initialize on-board quaternion and Fixed Head Star
Trackers employed to trim attitude and maintain gyro bias
•
DESCRIPTION OF RESULTS
– Gyro bias errors maintained to < 0.011 arc-sec/sec, allowing for successful guide
star acquisitions
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
16
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.2
– If any gyros are changed out, the gyro to FHST calibration shall be updated to an
accuracy that reduces the attitude error following a vehicle maneuver to one arcsecond per degree of slew or less. This calibration will be performed
immediately after the end of the BEA period. Until then, history has shown slew
miss-distances of about six arc-seconds per degree of slew.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– PCS-04, PCS-06
•
DESCRIPTION OF METHODS
– Following the BEA period, a series of SMS scheduled vehicle maneuvers
bracketed by FHST maps are conducted to calibrate the gyros by comparing
integrated gyro rate counts to the FHST measured attitude change
•
DESCRIPTION OF RESULTS
– Slew miss-distances are currently maintained to 0.5 arc-seconds/degree of slew,
meeting CEI Requirement 3.3.4.1.1(1) of 3.5 + 1 arc-second/degree of slew
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
17
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.3
– The PCS shall acquire guide stars in fine lock.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– PCS-07, SMS
•
DESCRIPTION OF METHODS
– The ability of each of the three FGSs to acquire a primary guide star will be
demonstrated while another FGS acquires a secondary guide star
•
DESCRIPTION OF RESULTS
– Successful SMS execution demonstrates ability to acquire guide stars in fine lock
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
18
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.4
– Once guide star acquisitions have begun, 2-FGS acquisitions will be scheduled
such that the HST486 on-board gyro bias update algorithm will maintain the gyro
drift rate bias to within 0.005 arc-seconds per second.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– SMS
•
DESCRIPTION OF METHODS
– Based on predicted gyro bias drift rates following release, 2-FGS acquisitions
were scheduled frequently to maintain low bias errors
•
DESCRIPTION OF RESULTS
– Scheduling of 2-FGS acquisitions following release allowed for autonomous bias
management and greatly reduced the need for ground updates. Early in SMOV,
brief excursions outside the 0.005 arc-second per second limit due to settling of
the Gyro 5 bias were managed through ground or on-board updates.
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
19
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.5
– The vehicle jitter during periods of gyro hold shall be measured.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– Routine
•
DESCRIPTION OF METHODS
– Sixty-second RMS values of the V2/V3 position path are calculated to obtain a
measurement of vehicle jitter
•
DESCRIPTION OF RESULTS
– For the current operational gyro configuration, 3-4-5, trending shows an average
jitter value of 0.0035 arc-seconds, meeting the CEI Requirement 3.3.4.3 of 0.007
arc-seconds
•
SUPPORTING DOCUMENTATION
– MOSES Observatory Performance Assessment Report, Section 6 – PCS,
LMSS/C090363
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
20
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.6
– Perform a Vehicle Disturbance Test (VDT) to characterize HST lineof-sight jitter,
structural dynamic responses, and disturbance sources. The VDT is a passive
test (not a forced response test) using a low-bandwidth attitude control law
during gyro-hold with the rate gyros in low mode. Obtain gyro measured
disturbance time responses due to SCM, SA-3, HGAs, RWAs, SSM thermal
gradients, and COS and WFC3 mechanism articulation. The VDT shall consist
of three separate tests that need not occur consecutively. The overall duration of
the VDT is at least 12 orbits of spacecraft time including (1) at least 2 orbits at
+V3 sunpoint while performing COS and WFC3 filter wheel articulation simulating
routine flight operations, (2) at least 5 orbits at +V3 sunpoint after achieving
thermal equilibrium (at least 36-hours at +V3 sunpoint), and (3) at least 5 orbits
at –V1 sunpoint.
– Status = MET
• Instrument mechanism articulations were waived/descoped from the VDT periods
• Remainder was MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– PCS-08
•
DESCRIPTION OF METHODS
– Time and frequency domain analysis of flight telemetry to identify and
characterize disturbance sources acting upon HST
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
21
PCS
L.10.4.8
•
•
SMOV4 REQUIREMENT: L.10.4.8.6
DESCRIPTION OF RESULTS
– The predominant persistent disturbance post-SM4 continues to be due to HGA
articulation exciting HST structural modes. Post-SM4 HST science jitter
continues to be near the lowest levels experienced on-orbit, based mainly on the
replacement of SA2 with SA3 during SM-3B. Minor changes in vehicle
performance due to hardware installed during SM-4 and the seven intervening
years between SMOV-3B and SMOV-4 are noticeable in the VDT data, but
currently present no concern to the operations of HST.
•
SUPPORTING DOCUMENTATION
– MOSES EM#1331, Vehicle Disturbance Test Report for SMOV-4, Sept. 2009
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
22
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.7
– All gyros will be left in a powered on state through the gyro to FHST alignment
calibration, if it is to be performed. Following the completion of the gyro to FHST
alignment calibration, the two gyros not in the active control loop will be
configured off. Following the VDT or gyro to FHST calibration, which ever occurs
last, one of the four gyros will be removed from the control loop and powered off.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– SMS
•
DESCRIPTION OF METHODS
– All six gyros will be calibrated to improve performance following future gyro
reconfigurations. When four gyros are used in the control law during VDT
activities, a lower noise floor is obtained. Three gyros in the control law is the
preferred long-term configuration.
•
DESCRIPTION OF RESULTS
– Gyros were successfully calibrated and HST was transitioned to a 3-4-5 gyro
configuration following the VDT with gyros 1-2-6 powered off.
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
23
PCS
L.10.4.8
•
SMOV4 REQUIREMENT: L.10.4.8.8
– The time allowed for OBAD maneuver will be managed to aid in attitude
maintenance until the slew miss-distances and gyro biases are reduced to a
sufficient level to permit successful FGS acquisitions. The time will be increased
from 66 seconds for a 300 arc-second maneuver to 105 seconds for a 1200 arcsecond maneuver if large attitude errors are anticipated prior to FGS
acquisitions.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– SMS
•
DESCRIPTION OF METHODS
– Based on predicted slew miss-distances and vehicle drift rates following release,
attitude correction durations will be managed to allow for successful removal of
the errors prior to the start of FGS acquisitions
•
DESCRIPTION OF RESULTS
– Following the gyro to FHST calibration, slew miss-distances were reduced
sufficiently to allow a return to nominal timing for attitude correction maneuvers
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
24
PCS SMOV4
REQUIREMENTS MATRIX
SMOV4 RQMT
L.10.4.8.1
RELEVANT ACTIVITY
TITLE
PCS-01, PCS-02, PCS-03,
BEA and Tranistion to Science SMS
PCS-04, CP-154, CP-167
RQMT STATUS
MET
L.10.4.8.2
PCS-04, PCS-06
Gyro to FHST Calibration
MET
L.10.4.8.3
PCS-07, SMS
Acquire Stars in Fine Lock
MET
L.10.4.8.4
SMS
Gyro Drift Rate Management
MET
L.10.4.8.5
Routine
Vehicle Jitter
MET
L.10.4.8.6
PCS-08
VDT
MET
L.10.4.8.7
SMS
Gyro Power Management
MET
L.10.4.8.8
SMS
Attitude Correction Durations
MET
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
25
Electrical Power System
Greg Waldo, Stan Krol
EPS SMOV ACTIVITIES
• EPS Successfully addressed the power system
related SMOV activity requirements and documented
the findings in the form of MOSES engineering
memoranda
• These requirements are: L.10.4.14.1 and L.10.4.14.2
aimed at assessing the replacement battery
performance and to characterize the post SM4
electrical loads respectively
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
27
Battery Performance
EPS-01 / L.10.4.14.1 - Characterize the Replacement Battery Performance
• The Replacement Battery system performance will be characterized during the
Battery Functional Tests and throughout the SM4 Mission Timeline and SMOV
period. Battery voltage, current, temperature and pressure performance will be
analyzed. Battery performance will be verified by analysis of normal EPS
telemetry. No special test is required during SMOV since telemetry is available
during SMS commanding.
Conclusion:
• During Servicing Mission 4 and since HST release from the orbiter, the
replacement batteries have exhibited excellent performance.
– The battery State Of Charge (SOC) continues to increase with generous margin
vs the safemode limits
– The battery voltage performance provides good margin to support the Science
Instruments
– The batteries also demonstrate good loadshare balance and temperature
performance
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
28
Battery SOC Performance
540
95
530
90
520
85
510
80
500
75
490
Individual Battery SOC (Ah)
100
70
BAT1CAP
BAT2CAP
BAT3CAP
BAT4CAP
BAT5CAP
BAT6CAP
System Battery SOC (Ah)
Individual Battery and System State Of Charge
(DOY 139‐301, 2009)
480
Total SOC
65
470
139
159
179
199
219
DOY 2009
239
259
279
299
29
Post SM4 Electrical Load
EPS-02 / L.10.4.14.2 - Characterize the Science Instrument and NCS Electrical
Loads
•The Science Instrument electrical loads will be characterized throughout the
SM4 Mission Timeline and SMOV period. Science Instrument and NCS current
/ power data will be gathered and compared to the various instruments modes
configured throughout the SM4 timeline and SMOV period. Electrical loads will
be verified by analysis of normal EPS and SI telemetry
Conclusion:
•The completion of the highly successful Hubble Space Telescope Servicing
Mission 4 restored and extended the satellite’s science capabilities with the
installation of advanced science instruments.
– The enhanced capabilities increase the vehicle electrical load from 2124 watts to
approximately 2621 watts.
– The present power system is capable of accommodating the load while
maintaining the battery performance.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
30
Post SM4 Power
System Performance
Vehicle Load Power and Total Battery SOC
DOY 139 ‐ 307, 2009
3000
Electrical Load Power (Watts)
2750
2500
NCS Operating
2250
2000
1750
1500
Avg. Load (watts)
1250
1000
130
150
170
190
210
230
250
270
SMOV4 CLOSURE
DOY 2009 REVIEW
Nov. 18, 2009
290
310
330
350
31
Post SM4 Full Science Load
PROJECTED HST LOAD CAPABILITY (Case 11)
SA INCIDENCE ANGLES 0, 5.8, 15, 20 and 25 DEG.
3500
2 Batts reach charge cut-off, 5 minutes of trickle charge
Orbit day durations w ere based on an approximation of
the Beta Angle and may not reflect the actual dates for
the peaks.
3400
3300
2-SIGMA PEAK
3200
3100
Bus Load (Watts)
3000
2900
2800
2700
2600
2500
SM4
MEAN
2400
2300
2200
2100
2000
2-SIGMA PEAK
MEAN
NICMOS, ACS (Side 1 SBC),
WFPC2, NCS
(Case 11)
NICMOS = Norm Op
NCS = Norm Op (7100 RPS)
STIS = Norm Op (CCD On, MAMAs On)
ACS = Norm Op, Side-1, 2-Ch
WFC3 = Norm Op Side2
COS = Norm Op (FUV, NUV)
1900
2008
2009
2010
2011
2012
2013
2014
YEAR
MB_Pwr_0deg
MB_Pwr_5.8deg (min slew cmd)
MB_Pwr_15deg
MB_Pwr_20deg
Pre-SM4 ACS 1-ch Mean
Pre-SM4 ACS 1-ch 2-Sigma Peak
Post-SM4 Mean
Post-SM4 2-Sigma Peak
MB_Pwr_25deg
32
Post SM4
NICMOS=Safe, NCS=Safe
PROJECTED HST LOAD CAPABILITY (Case 6)
SA INCIDENCE ANGLES 15, 20 and 25 DEG.
3500
2 Batts reach charge cut-off, 5 minutes of trickle charge
Orbit day durations were based on an approximation of the
Beta Angle and may not reflect the actual dates for the
peaks.
3400
3300
3200
3100
Bus Load (Watts)
3000
2900
2800
2700
2600
2500
SM4
2400
2300
2200
2-SIGMA PEAK
2100
MEAN
2000
(Case 6)
NICMOS = Safe
NCS = Safe
STIS = Norm Op (CCD On,
MAMAs On)
ACS = Norm Op 2-Ch
WFC3 = Norm Op Side2
COS = Norm Op (FUV, NUV)
2-SIGMA PEAK
MEAN
NICMOS, ACS (Side 1 SBC),
WFPC2, NCS
1900
2008
2009
2010
2011
2012
2013
2014
Post-SM4 Mean
Post-SM4 2-Sigma Peak
YEAR
MB_Pwr_15deg
MB_Pwr_20deg
MB_Pwr_25deg
Pre-SM4 ACS 1-ch Mean
Pre-SM4 ACS 1-ch 2-Sigma Peak
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
33
Thermal Control System
Josh Abel
TCS
L.10.4.13.1
•
•
SMOV4 REQUIREMENT: L.10.4.13.1
–
Verify predicted temperature changes due to NOBL installation on SSM Bays 5, 7 and 8. Note: Prelaunch
predictions are documented in EM FSS 1714 (9/15/2008)
–
Status = MET
RELEVANT SMOV4 ACTIVITY
–
•
DESCRIPTION OF METHODS
–
•
N/A
Flight telemetry trending and thermal math model correlation
DESCRIPTION OF RESULTS
Temperature
Reduction
Comments
Bay 5
18°C
As predicted
Bay 7
None
As predicted, NOBL prevents potential failure of MLI blanketing
6°C
8
• BaySUPPORTING
–
Reduction is 3°C less than predicted
(Attributed to PSEA optical property assumptions within Bay 8.
DOCUMENTATION
NOBL installation successful. EM MOSES 1334)
See following chart(s) and EM MOSES 1334
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
Impacts
No impact to science
scheduling or HST
operations
35
TCS
L.10.4.13.1
Bay 5 Flight Telemetry Trending (Ref EM MOSES 1334)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
36
TCS
L.10.4.13.1
Bay 8 Flight Telemetry Trending (Ref EM MOSES 1334)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
37
TCS
(Special Topic)
•
SI C&DH-R SMOV Thermal Assessment
– Due to the increased power draw of the replacement unit and the increase in
science data volume following SM4, operational temperature mitigations for the
SI C&DH-R were planned following a review of the SMOV thermal performance
(Ref. SI C&DH-R Pre-Ship Review)
– During SMOV, observed critical temperatures were 3-4°C higher than predicted
(but have remained within ground system limits)
– While the thermal interface between the SI C&DH-R and the Bay 10 door could
not be fully characterized in ground testing (flatness tolerances of each surface
are large and the profile of the on-orbit door was unknown), prelaunch model
predictions were made based upon a series of pressure tests using a simulated
interface
– Thermal model flight data correlation has subsequently estimated that the
tray/door conductance is ~25% of the expected value (still significantly improved
from the pre-SM4 interface as a result of thermal modifications to the –R unit)
– The Bay 10 Thermal Restrictions Operations Working Group (B10TROWG) has
been formed. The group includes the STScI in the development of an operations
plan which maintains critical temperature limits with a minimal impact to science
operations.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
38
TCS
(Special Topic)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
39
WFC3
(Special Topic)
•
WFC3 SMOV Thermal Assessment
– The WFC3 UVIS and IR detectors are actively cooled using a system of thermoelectric coolers (TECs) and an external thermal radiator
– This system is working well on orbit, maintaining the desired detector
temperatures with significant margin still available from the TECs
– However, the design of the system does present the possibility of a thermal
feedback loop (i.e. a “runaway”)
•
•
•
As power from the TECs increase, the temperature of the radiator increases
As the radiator temperature increases, more power is required from the TECs… continues until a
stable point is reached
If the environmental heating of the radiator is too high, the concern is that a stable point may not be
reached within the control authority of the TECs, resulting a temporary loss a temperature control on
the detectors
– A team, including the STScI, WFC3 engineering team, and TCS, was formed to
evaluate on-orbit thermal performance
•
•
•
The observed TEC power was higher than predicted by the prelaunch model
Extensive flight trending and model correlation was performed, however, the team was unable to rule
out the possibility of a short term lack of control in the worst case
Temperatures and TEC performance continues to be closely monitored as analysis continues
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
40
Wide Field Camera 3
Susana Deustua
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
WFC3 Team
The WFC3 Science Integrated Product
Team (2009)
Sylvia Baggett
Tiffany Borders
Howard Bushouse
Linda Dressel
Susana Deustua
Michael Dulude
George Hartig
Bryan Hilbert
Robert Hill (GSFC)
Jason Kalirai
Jessica Kim Quijano
Randy Kimble (Instrument Scientist, GSFC)
Vera Kozhurina-Platais
Knox Long
John MacKenty (Deputy Instrument Scientist)
Brian McLean
Peter McCullough
Cheryl Pavlovsky
Larry Petro
Nor Pirzcal
Abhijith Rajan
Adam Riess
Elena Sabbi
Alex Viana
Michael Wong
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
Past Science IPT Members
Wayne Baggett
Howard Bond
Tom Brown
Laura Cawley
Ed Cheng (GSFC, now Conceptual
Analytics)
Ilana Dashevsky
Don Figer
Mauro Giavalisco
Shireen Gonzaga
Christopher Hanley
Ron Henry
Pat Knezek
Ray Kutina
Casey Lisse
Olivia Lupie
André Martel
Neill Reid
Massimo Robberto
Michael Robinson
Megan Sosey
Massimo Stiavelli
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
The WFC3 Scientific Oversight Committee
Bruce Balick, University of Washington
Howard E. Bond, Space Telescope Science Institute
Daniela Calzetti, Space Telescope Science Institute
C. Marcella Carollo, Institute of Astronomy, ETH, Zurich
Michael J. Disney, Cardiff University
Michael A. Dopita, Mt Stromlo and Siding Spring Observatories
Jay Frogel, AURA
Donald N. B. Hall, University of Hawaii
Jon A. Holtzman, New Mexico State University
Randy Kimble, NASA Goddard Space Flight Center (ex officio)
Gerard Luppino, University of Hawaii
Patrick J. McCarthy, Carnegie Observatories
John MacKenty, Space Telescope Science Institute (ex officio)
Robert W. O’Connell, University of Virginia (Chair)
Francesco Paresce, European Southern Observatory
Abhijit Saha, National Optical Astronomy Observatory
Joseph I. Silk, Oxford University
John T. Trauger, Jet Propulsion Laboratory
Alistair R. Walker, Cerro Tololo Interamerican Observatory
Bradley C. Whitmore, Space Telescope Science Institute
Rogier A. Windhorst, Arizona State University
Erick T. Young, University of Arizona
WFC3 Management, Engineering, and Contractor Teams
Thai Pham and Jackie Townsend, GSFC Instrument Managers
GSFC Engineering Teams in Codes 400, 500, and 600 (plus Code 300
reviewers)
Ball Aerospace, Swales Aerospace (now ATK), Teledyne, E2V, and many others
300-400 people made significant contributions to the development of Wide Field
Camera 3
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
42
WFC3 SMOV4 Requirements Matrix
SMOV4 RQMT
L.10.4.1
L10.4.1.1
L.10.4.1.1.1
L.10.4.1.1.2
L.10.4.1.1.3
L.10.4.1.1.4
L.10.4.1.1.5
L.10.4.1.1.6
L.10.4.1.1.7
L.10.4.1.1.8
L.10.4.1.1.9
L.10.4.1.1.10
L.10.4.1.1.11
L.10.4.1.1.12
RELEVANT
ACTIVITY
WFC3
PROPOSAL
ID
01
11
01
02
03
8
9a
9b
10a
10b
14
19
20
9a
9b
10a
10b
15
19
20
6
7
4
5
16
17
18
13
11454
11424
11454
11357
11358
11421
11422
11529
11423
11543
11427
11432
11433
11422
11529
11423
11543
11428
11432
11433
11419
11420
11431
11426
TITLE
WFC3 Verification
WFC3 Engineering Verification
Activation Test
UVIS Initial Alignment
Activation Test
Load and Dump On-Board Memory
Science Data Buffer Check
Channel Select Mechanism Test
SOFA Test
UVIS Tungsten Lamp Cross Check
IR FSM Test
IR Tungsten Lamp Cross Check
UVIS Shutter Test
UVIS Internal Flats
IR Internal Flats
SOFA Test
UVIS Tungsten Lamp Cross Check
IR FSM Test
IR Tungsten Lamp Cross Check
D2 Calibration Lamp Test
UVIS Internal Flats
IR Internal Flats
UVIS Detector Functional Test and Gain
IR Detector Functional Test and Gain
UVIS CCD Activation/Cooldown
IR Detector Activation/Cooldown
UVIS TEC Performance
IR TEC Performance
UVIS Hot Pixel Anneal
UVIS SMOV Contamination Monitor
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
RQMT STATUS
COMMENTS
MET
MET
MET
MET
MET
MET
Three SOFA wheels miss 1 step on
occasion. Focus corrector tip/tilt
mechanism showed nonreproducible "wobble".
MET
MET
MET
MET
MET
MET
43
WFC3 SMOV4 Requirements Matrix
L.10.4.1.2
L.10.4.1.2.1
L.10.4.1.2.2
11
12
21
22
11
12
21
22
23
24
27
28
27, 28
11424
11425
11434
11435
11424
11425
11434
11435
11436
11437
11440
11441
11549
WFC3 Optical Alignment Requirements
UVIS Initial Alignment
IR Initial Alignment
UVIS Fine Alignment
IR Fine Alignment
UVIS Initial Alignment
IR Initial Alignment
UVIS Fine Alignment
IR Fine Alignment
UVIS Image Quality
IR Image Quality
UVIS Pointing Stability
IR Pointing Stability
UVIS and IR Pointing Stability
L.10.4.1.2.3
L.10.4.1.2.4
L.10.4.1.3.2
L.10.4.1.3.3
L.10.4.1.3.4
L.10.4.1.3.5
L.10.4.1.3.6
L.10.4.1.3.7
MET
MET
25
26
11438
11439
31
32
29
30
33
34
35
36
13
37
38
19
20
39
40
44
11444
11445
11442
11443
11446
11447
11448
11449
11426
11450
11451
11432
11433
11452
11453
11808
L.10.4.1.3
L.10.4.1.3.1
MET
UVIS PSF Wings
IR PSF Wings
WFC3 Calibration Requirements
UVIS Plate Scale
IR Plate Scale
FGS-UVIS Update
FGS-IR Update
UVIS Dark Current, Noise, Background
IR Dark Current, Noise, Background
UVIS SAA Passage
IR SAA Passage
UVIS SMOV Contamination Monitor
UVIS Photometric Zero Points
IR Photometric Zero Points
UVIS Internal Flats
IR Internal Flats
UVIS Flat Field Uniformity
IR Flat Field Uniformity
UVIS Bowtie Monitor
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
REPLACED BY PROP 11549
REPLACED BY PROP 11549
REPLACED PROP 11440 & 11441.
Minimal excursion from stability
requirement. Occurs once in 2
orbits for IR and UVIS. This is less
than in ground tests.
MET
MET
MET
MET
MET
MET
MET
MET
44
Highlighting
• IR and UVIS sensitivity and throughput
• IR and UVIS geometric distortion and plate
scale
• IR encircled energy (EE) and Point Spread
Function (PSF)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
45
WFC3 SMOV4 ISRs
(to date)
2009-15
2009-16
2009-17
2009-18
2009-19
2009-20
2009-21
2009-22
2009-23
2009-24
2009-25
2009-26
2009-27
2009-28
2009-29
2009-30
2009-31
2009-32
2009-33
2009-34
2009-35
2009-36
2009-37
2009-38
2009-39
2009-40
2009-41
In preparation
In preparation
In Preparation
In preparation
In preparation
WFC3 SMOV Proposal 11454: Activation Test
WFC3 SMOV On-Orbit Darks ((Proposals 11419, 11426, 11431,and 11446)
WFC3 SMOV Proposal 11552: Calibration of the WFC3 G141 grism
WFC3 SMOV Proposal 11552: Calibration of the WFC3 G102 grism
WFC3 SMOV Proposal 11452: UVIS Flat Field Uniformity
WFC3 SMOV Proposal 11798: UVIS PSF Core Modulation
WFC3 SMOV Proposal 11446: IR Channel Dark Current, Readnoise, and Background
WFC3 SMOV Proposal 11421: Channel Select Mechanism Test
WFC3 SMOV Proposal 11420: IR Channel Functional Tests
WFC3 SMOV Proposal 11808: UVIS Bowtie Monitor
WFC3 SMOV Proposal 11427: UVIS Channel Shutter Shading
WFC3 SMOV On-Orbit UVIS Biases (Proposals 11419, 11426, 11431,and 11448)
WFC3 SMOV Proposal 11422/11529: UVIS SOFA and Lamp Checks
WFC3 SMOV Proposal 11423/ 11543: IR FSM and Lamp Checks
WFC3 SMOV Proposal 11419: UVIS Gain
WFC3 SMOV Proposal 11451: IR Photometric Performance and Calibration
WFC3 SMOV Proposal 11450: UVIS Photometric Performance and Calibration
WFC3 SMOV Proposal 11549: Image Stability
WFC3 SMOV Proposal 11444: UVIS Geometry Distortion Calibration
WFC3 SMOV Proposal 11445: IR Geometric Distortion Calibration
WFC3 SMOV Proposal 11442: Alignment of the WFC3/UVIS Apertures to the FGS
Coordinate Frame
WFC3 SMOV Proposal 11443: Alignment of the WFC3/IR Apertures to the FGS
Coordinate Frame
WFC3 SMOV Proposal 11437/9: IR On-orbit PSF Evaluation
WFC3 SMOV Proposal 11436/8: UVIS On-orbit PSF Evaluation,
WFC3 SMOV Proposal 11453: IR Flat Field Uniformity
WFC3 SMOV Proposal 11449: IR SAA Passage
WFC3 SMOV Proposal 11798: UVIS PSF Core Modulation
WFC3 SMOV Proposal 11426: UVIS Contamination Monitor
WFC3 SMOV Proposal 11431: UVIS Hot Pixel Anneal
WFC3 SMOV Proposal 11448: UVIS SAA Passage
WFC3 SMOV Proposal 11424/34: UVIS alignment
WFC3 SMOV Proposal 11425/35: IR alignment
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
Petro
Borders & Baggett
Kuntschner et al.
Kuntschner et al.
Sabbi
Sabbi
Hilbert & McCullough
Bushouse
Hilbert & McCullough
Baggett & Borders
Hilbert
Borders & Baggett
Baggett, Sabbi and McCullough
Baggett
Baggett & Borders
Kalirai et al.
Kalirai et al.
Brown
Kozhurina-Platais et al.
Kozhurina-Platais et al.
Dressel, Cox, and Lallo
Dressel, Cox, and Lallo
Hartig, Delker, Dressel
Hartig, Delker, Dressel
Hilbert
Barker, Martel, McCullough
Sabbi
Baggett, Borders
Baggett, Borders
Martel, Barker
Hartig, Dressel
Hartig, Dressel
46
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.1
– WFC3 entry into each of four instrument states (Boot, Hold, Operate,
Observe) shall be demonstrated. Operations shall be commanded via
stored commands transmitted over the Supervisory Bus.
– Status=MET
•
SMOV4 REQUIREMENT: L.10.4.1.1.2
– WFC3 entry into each of the defined detector states shall be
demonstrated. Operations shall be commanded via stored commands
transmitted over the Supervisory Bus.
– Status=MET
•
SMOV4 REQUIREMENT: L.10.4.1.1.3
– WFC3 command and engineering data interface via the RIU and
science data transmission via the Science Data Formatter (SDF) shall
be verified by monitoring of normal configuration and science activities.
– Status=MET
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
47
WFC3
L.10.4.1.1 Engineering
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_01 (11454)
•
DESCRIPTION OF METHODS
– Repeats SM4 functional test: command WFC3 to Boot, Hold, Operate and
Observe
– Acquire 4 UVIS Dark, 2 UVIS Flats through 2 filters, and 4 IR Dark images to
verify operations.
•
DESCRIPTION OF RESULTS
– Nominal operation of detectors and mechanisms,
– Nominal transition to science operating temperatures
– Exceptions: Inadvertent SAFE during recovery from SM4 SAFE required
updating limits and procedure.
•
SUPPORTING DOCUMENTATION
– ISR WFC3 2009-15
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
48
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.4
– Onboard memory shall be checked by performing a full dump of the CS (control
section) EEPROM, PROM, and EXEC RAM, and verify a match with the ground
image.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_02 (11357)
•
DESCRIPTION OF METHODS
– Full dump of the WFC3 Control Section (CS) EXEC RAM, EEPROM and PROM
memory with the CS in OPERATE. Dump CS Buffer RAM containing the data as
normal science images. Set WFC3 SI qasi_states to OBSERVE enabling the
Science Data Interface and allowing dumps commanded in the special
instructions to succeed.
•
DESCRIPTION OF RESULTS
– EXEC RAM, EEPROM, and PROM were read out and contained no errors.
•
SUPPORTING DOCUMENTATION
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
49
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.5
– The ability to read and write data from and to the science data buffer shall be
demonstrated.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_03 (11358)
•
DESCRIPTION OF METHODS
– The WFC3 Science Buffer RAM is checked for bit flips during SAA passages.
Followed by a Control Section (CS) self-test consisting of writing/reading a
specified bit pattern from each memory location in Buffer RAM. CS in OPERATE.
•
DESCRIPTION OF RESULTS
– No bit flips in the Science Buffer occurred during SAA passages
– CS self-test executed without error.
•
SUPPORTING DOCUMENTATION
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
50
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.6
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
Observe large nearby galaxy in IR and UVIS channels (CSM)
Obtain flats with one filter in each wheel (UVIS SOFA and CCD shutter), and obtain flats
through all IR filters
Observe GD 153 in UVIS F395N (UVIS shutter)
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_08, 9a, 9b, 10a, 10b, 14, 19, 20 (11421, 11422, 115229, 11423, 11543, 11427,
11432, 11433)
DESCRIPTION OF METHODS
–
–
•
The performance of the Channel Select Mechanism, M1 and IM2 Alignment and Focus
Corrector Mechanisms, UVIS Selectable Optical Filter Assembly, IR Filter Wheel, and UVIS
CCD shutter shall be verified.
Status = MET
Nominal: CSM and IR filter wheel, M1 and IM2 Alignment Mechanism, Shutter shading
0.001 secs across detector
Focus Corrector Mechanism showed a slight wobble
SOFA filter wheel 10 occasionally misses a step.
SUPPORTING DOCUMENTATION
–
ISR WFC3 2009-22, 2009-25, 2009-27, 2009-28
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
51
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.7
– The functionality of the WFC3 Tungsten and Deuterium calibration lamps shall
be verified. Operation of the deuterium lamp shall be deferred for an initial
outgassing period following release of the observatory, as defined in the CARD
3.4.13.11.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_9a, 9b, 10a, 10b, 15, 19, 20 (11422, 11529, 11423, 11543, 11428,
11432, 11433)
•
DESCRIPTION OF METHODS
– Acquire FLATS in all broad band filters (UVIS and IR) with Tungsten lamps and
UVIS filters using deuterium lamp.
•
DESCRIPTION OF RESULTS
– Tungsten lamps are 6-10% brighter on orbit than on ground, decay rate is
consistent with 5-year lifetime.
– Deuterium lamp is nominal
•
SUPPORTING DOCUMENTATION
– ISR WFC3 2009-27, 2009-28
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
52
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.8
– Functionality of the WFC3 UVIS CCD detector shall be demonstrated. This shall
include the proper accumulation of signal over a specified time interval and data
readout, readout of subarrays, and on-chip binning.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_06 (11419)
•
DESCRIPTION OF METHODS
– Acquire fullframe and subarray BIAS, DARK and FLAT (internal lamp) and
evaluate readnoise, dark current, and gain values.
•
DESCRIPTION OF RESULTS
– Gain =1.6 - 1.63 e-/DN (within 3% of ground values)
– Readnoise: Amp A=3.1e-,Amp B=3.2e-, Amp C=3.1e-, Amp D=3.2e– Dark current=1 to 2 e-/pix/hour, much less than CEI spec of 20 e-/pix/hour,
growth rate is ~2e-/pix/hour/year.
•
SUPPORTING DOCUMENTATION
– ISR WFC3 2009-16, 2009-26, 2009-29
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
53
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.9
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Obtain full frame and subarray DARK and FLAT(internal lamp) images to evaluate IR dark
current, readnoise, gain.
DESCRIPTION OF RESULTS
–
–
–
–
–
•
WFC3_07 (11420)
DESCRIPTION OF METHODS
–
•
Functionality of the WFC3 IR detector shall be demonstrated. This shall include the proper
accumulation of signal over a specified time interval and multiaccum data readout, readout of
subarrays, and characterization of the reference pixels.
Status = MET
Mean dark current = 0.030 - 0.048 e-/sec/pixel (SPARS200 Ramps)
CDS Readnoise = 19.6 eGain = 2.28 - 2.47 e-/ADU
Less than 3% difference in signal rate between fullframe and subarray flats.
Exceptions: Identified light leak when pointed at the bright Earth. Commanding CSM to the
UVIS position mitigates the light leak.
SUPPORTING DOCUMENTATION
–
ISR WFC3 2009-23
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
54
Read Noise Improved vs. Ground Test
•
•
•
CDS read noise is 20-22 e- rms (varies with quadrant); same as
ground result; noise in RAPID reads also similar to T-V result
Effective noise reading up the ramp is actually a bit lower in flight than
in thermal-vac for long exposures: (average of the 4 quadrants shown)
# of Reads
3
8
15
Effective noise
(e- rms; SMOV)
19.6
16.0
12.4
Effective noise
(e- rms; thermal-vac)
20.8
17.8
14.6
For SPARS200
sample
sequence
Combined with excellent dark current, very well satisfies goal of being
zodiacal-background-limited for long exposures in broad bands (zodi
rates from a few tenths to >1 e-/pix/s)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
55
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.10
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Cool detectors to operating temperatures
verify that UVIS and IR TECs maintain detector science temperature
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_04, 05, 16, 17 (NONE)
DESCRIPTION OF METHODS
–
–
•
The ability of the TECs to cool and stabley control the detectors shall be tested at a small
number of temperature set points, in order to determine a cold stable operating point. The
goal is to demonstrate that this point be at least as cold as –83C for the UVIS CCDs and
145K for the IR detector. WFC3 detectors cannot be cooled before 21 days in vacuum
(CARD 3.4.13.15).
Status = MET
WFC3 radiator operating slightly above expected temperatures
Nominal operating temperature reached: UVIS CCD@-83C, IR MCT@ -128C.
Correlation of instrument level thermal model is ongoing. Team is confident that focal plane
temperature will be held.
SUPPORTING DOCUMENTATION
–
none
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
56
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.11
– The ability to perform a CCD anneal shall be demonstrated.
– Relevant CEIS requirements: 4.7.2 CCD detector warm operations
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_18 (11431)
•
DESCRIPTION OF METHODS
– CCD detectors are warmed. BIAS and DARK images are taken before and after
each anneal
•
DESCRIPTION OF RESULTS
– Procedure was successfully executed every 4 weeks
– BIAS and DARK images show read noise and dark current remain stable across
the anneals
– >90% of hot pixels are fixed.
•
SUPPORTING DOCUMENTATION
– See following chart, which also includes Cy 17 data.
– ISR WFC3 2009-16, 2009-26
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
57
UVIS Hot Pixel Anneal
Hot Pixel Rate Over 2 Anneal Cycles
58
WFC3
L.10.4.1.1 Engineering
•
SMOV4 REQUIREMENT: L.10.4.1.1.12
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Observe standard star GRW+70 weekly in 18 key filters
Obtain FLAT images in F336W, F438W, and F606W.
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_13 (11426)
DESCRIPTION OF METHODS
–
–
•
WFC3 operations shall be managed to minimize risk of contamination of its optical surfaces
by materials outgassed either internally or from other units installed during the SM as well as
from the payload bay environment during servicing (CARD 3.4.13.15, 3.4.13.16, 3.4.13.17) .
A contamination monitoring program shall be initiated as early as possible after the SM.
Status = MET
Photometry stable to better than 2% as function of wavelength and time.
Internal flats are flat to <1% except for known filter feature shift.
Tungsten lamp output decreased by ~1% over SMOV4 (consistent with expectations).
SUPPORTING DOCUMENTATION
–
–
See following slide
ISR WFC3 2009-16, 2009-26 and one in preparation.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
59
UVIS contamination monitor (11426)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
60
WFC3
L.10.4.1.2 Optical Alignment
•
SMOV4 REQUIREMENT: L.10.4.1.2.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
After each change in focus and tilt position, acquire images of NGC 188 in UVIS F410M and in IR F127M
and measure encircled energy and image diameters of stars in the field.
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_11, 12, 21, 22 (11424, 11425, 11434, 11435)
DESCRIPTION OF METHODS
–
•
The encircled energy and image diameter shall be measured over a grid of focus and tilt positions for both
M1 and IM2 correctors. These measurements shall be used to set the nominal corrector positions.
Status = MET
Phase retrieval and encircled energy measurements of many stars over field used to determine corrector
adjustments required to optimize image quality.
UVIS Corrections: focus = -95, tip/tilt =4,4. UVIS corrector focus wobble was an unexpected challenge
IR Corrections: focus=-24, tip/tilt = 5,-1. Larger than expected corrector cylinder adjustment moving to
region outside experience based, residual astigmatism slightly greater than expected, but within wavefront
error spec.
SUPPORTING DOCUMENTATION
–
–
See next three slides
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
61
WFC3_11: UVIS Initial
Alignment (11424)
Left: corrector offset from each star image.
Right: Encircled Energy within 0.15 arc second diameter.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
62
WFC3_12: IR Initial
Alignment (11425)
Left: corrector offset from each star image.
Right: Encircled Energy within 0.15 arc second diameter.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
63
WFC3_21, 22: UVIS, IR Fine
Alignment (11434, 11435)
Top Left: UVIS encircled energy as function of inner
and outer cylinder step.
Bottom Left: UVIS mean coma as function of inner
and outer cylinder step
Right: IR encircled energy as function of corrector
focus position, corrected for HST OTA breathing
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
64
WFC3
L.10.4.1.2 Optical Alignment
•
SMOV4 REQUIREMENT: L.10.4.1.2.2
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Measure the PSF and encircled energy of stars in NGC 188 using fullframe UVIS F275W & F621M and IR
F098M & F164M images.
DESCRIPTION OF RESULTS
–
–
•
WFC3_11, 12, 21, 22, 23, 24 (11424, 11425, 11434, 11435,11436,11437)
DESCRIPTION OF METHODS
–
•
The image quality at the detectors over the full field shall be measured via broad and narrow band imaging
of stars. The requirement for encircled energy in the UVIS channel field center is 75% within a diameter of
0.25 arcseconds, through the F631N filter. The requirement for encircled energy in the IR channel field
center is 75% within a diameter of 0.60 arcseconds, for a star observed through the F164N.
Status = MET
UVIS and IR: Phase retrieval, encircled energy, sharpness, FWHM over the field meet or exceed
expectation.
Exception: PSF core EE in 0.25 arcsec diameter is below (46% vs. 48%) CEI spec at 1.6 microns, as
expected from TV3 results. No further action required
SUPPORTING DOCUMENTATION
–
–
See next slide
ISR WFC3 2009-37, 2009-38 and one in preparation.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
65
WFC3_23, 24 (11436, 11437)
F275W
F625W
F098M
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
F160W
66
WFC3
L.10.4.1.2 Optical Alignment
•
SMOV4 REQUIREMENT: L.10.4.1.2.3
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Max UVIS excursion in 2-orbit block = 14 mas, specification is 10 mas
Max IR excursion in 2-orbit block = 25 mas, specification is 20 mas
Stability exceptions were less frequent than in ground testing.
Exceptions:
–
•
Observations of IC4499(hot orbits) and NGC 7492(cold orbits) in UVIS F814W and IR F110W. 10 UVIS
images followed by 3 IR subarray images. Implemented as 12 hot orbits, 10 cold orbits, and 2 hot orbits.
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_27,28 (11549)
DESCRIPTION OF METHODS
–
•
The pointing stability of the OTA-WFC3 combination shall be measured over at least three orbits including
hot and cold spacecraft attitudes. The purpose of these measurements is to confirm that the typical thermal
environment after SM4 does not cause unacceptable image drifts.
Status=MET
Meets Cycle 17 performance prediction as expected from TV3 tests, does not meet highly demanding CEI
spec. Minimal impact on GO science.
SUPPORTING DOCUMENTATION
–
–
See next slide
ISR WFC3 2009-32
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
67
WFC3_27&WFC3_28 (11549)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
68
WFC3
L.10.4.1.2 Optical Alignment
•
SMOV4 REQUIREMENT: L.10.4.1.2.4
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Obtain deep exposures of GD 153 in UVIS F275W & F625W and in IR F098M & F160W, in 5
field positions for each filter, to assess PSF wings.
DESCRIPTION OF RESULTS
–
–
•
WFC3_25, 26 (11438, 11439)
DESCRIPTION OF METHODS
–
•
The WFC3 Point Spread Function (PSF) shall be measured over a large dynamic range in
order to study PSF wings and image ghosts.
Status = MET
Encircled energy and azimuthally averaged PSF comparable to predictions out to r~6
arcsecs.
Exceptions: Meets specs but best available model over predicts UVIS EE between 0.2 and
1.0 arcsec likely due to spatial frequency limitation of OTA mirror WFE maps.
SUPPORTING DOCUMENTATION
–
See following slide
–
ISR WFC3 2009-37, 2009-38
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
69
WFC3_25, 26 (11438, 11439)
PSF WINGS
Left: UVIS F275W
Right: IR F160W
20 x 20 arcsec,
6 dex log stretch
PSF Characterization
Encircled energy vs.
Radius (arcsec)
Solid=measurements
Dotted=model
Plusses=specs
Solid=measurements
Dotted=model
Plusses=specs
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
Left: UVIS F275
Right: IR F160W
70
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Observations of globular cluster 47 Tuc in 9 positions in UVIS F606W and IR F160W.
DESCRIPTION OF RESULTS
–
–
–
–
–
–
•
WFC3_31, 32 (11444, 11445)
DESCRIPTION OF METHODS
–
•
The plate scale, orientation and geometric distortion shall be measured for each of the WFC3 channels by
imaging an astrometric field.
Status = MET
UVIS Geometric distortion solution good to 2 mas
UVIS Plate Scale Orientation, CCD1, CCD2 X=0.0396, 0.0399, Y= 0.0393, 0.0398 arcseconds
UVIS Beta X =-41.121 deg, -41.492 deg, Beta Y = 44.957 deg, 44.893 deg.
IR geometric distortion solution good to 8 mas
IR Plate scale is X=0.1354 arcsec, Y=0.1209
IR Orientation is Beta X=44.8161, Beta Y=45.0099.
SUPPORTING DOCUMENTATION
–
–
IDCTAB
ISR WFC3 2009-33 and WFC3 2009-34
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
71
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.2
– The absolute FGS/WFC3 alignment shall be determined .
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– WFC3_29, 30 (11442, 11443)
•
DESCRIPTION OF METHODS
– Use observations of astrometric field in NGC188 to map WFC3/UVIS and
WFC3/IR to the HST FGS frame.
•
DESCRIPTION OF RESULTS
– center of UVIS frame changed by V2=-0.57, V3=+2.71 arcsec. Rotation of -0.74
degrees
– center of IR frame changed by V2=-0.98, V3=+6.18 arcsec. Rotation of -0.15
degrees.
– All aperture definitions included in Aug 3 SIAF update.
•
SUPPORTING DOCUMENTATION
– See ISF WFC3 2009-35, 2009-36
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
72
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.3
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Obtain full frame BIAS and DARK images at regular intervals during SMOV4. Assess and
monitor dark current, readnoise, hot pixels.
DESCRIPTION OF RESULTS
–
–
–
–
–
•
WFC3_33 (11446)
DESCRIPTION OF METHODS
–
•
Dark rate, read noise and CTE shall be measured for the CCD detector. The hot pixel
creation rate shall be assessed and the efficacy of the hot annealing cycle shall be
demonstrated. The stability of these parameters over a 30 day baseline shall be determined.
dark current = 1.5 - 2.0 e-/pix/hr
Readnoise = 3.1, 3.2, 3.1, 3.2 e-, for amps A,B,C, & D, respectively, gain =1.6 e-/ADU
Read noise stability: 1%, 0.4%, 0.7%, and 0.8%, for amps A,B,C, & D, respectively.
CTE growth rateis consistent with ACS using cosmic ray analysis (EPER test deferred to
Cycle 17)
hot pixel creation rate ~1000 pix/day above 54 e-/pix/hr
SUPPORTING DOCUMENTATION
–
ISR WFC3 2009-16, 2009-26
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
73
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.4
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Measure the IR background through broad band filters
Monitor IR dark current and readnoise using Dark images.
DESCRIPTION OF RESULTS
–
–
–
–
•
WFC3_34 (11447)
DESCRIPTION OF METHODS
–
–
•
Dark rate, background level, and read noise shall be measured for the IR detector. IR bad
pixels shall be characterized. The stability of these parameters over a 30-day baseline shall
be determined.
Status = MET
dark current = 0.05 e-/pix/sec
readnoise is 21-22e- per CDS pair
background level (zodi + HST) is ~1 e-/second in broad band filters
readnoise stability is better than 5%
SUPPORTING DOCUMENTATION
–
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
74
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.5
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Acquire DARKs in both WFC3 channels during three visits across the pre-defined SAA contour, skirting the
inner regions of the NE and NW sections and the deepest part of the SAA.
DESCRIPTION OF RESULTS
–
–
–
•
WFC3_35, 36 (11448, 11449)
DESCRIPTION OF METHODS
–
•
The behavior of both channels during SAA passages shall be characterized. The SAA afterimage shall be
measured for the IR detector.
Status = MET
UVIS: Dark current rate and CR hit rate are ~ 20x and 100x greater at the center of the SAA compared to
edge
IR: Deepest region of SAA impacts ~12% of pixels per minute, WFC3/IR can be used for short exposures
inside SAA. Enhanced dark current from SAA passage decays quickly enough that post-SAA passage darks
are not anticipated for WFC3 observations.
Current SAA contours acceptable for Cy 17.
SUPPORTING DOCUMENTATION
–
–
see next slide
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
75
WFC3_35, 36 (11448, 11449)
Peak of deepest SAA passage for the IR channel: ~30% pixels CR affected in 153 seconds
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
76
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.6
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
Obtain images of GD153 in UVIS Amp A 512x512 subarray in 37 filters, and in subset of 8 filters at intervals
of 1 day, 1 week and 1 month. Obtain images of GRW+70 in all 14 UV filters plus F606W & F814W every
week.
Obtain images of GD153 and P330E in all IR filters using 128x128 subarray at intervals of 1 day, 1 week
and 1 month.
DESCRIPTION OF RESULTS
–
–
•
WFC3_13, 37, 38 (11426, 11450, 11451)
DESCRIPTION OF METHODS
–
•
Instrument sensitivity vs. wavelength shall be measured for a subset of WFC3 spectral elements.
Sensitivity measurements shall be performed using astronomical standard stars. The photometric stability
shall be determined over several orbits. As part of this process, UV sensitivity measurements shall be
obtained as early as possible, to enable early trending of UV sensitivity.
Status = MET
Photometric stability is better than 1% in medium and broad bands, better than 2% in narrow bands and in
UV.
Sensitivity is 5-15% higher than predicted, depending on wavelength.
SUPPORTING DOCUMENTATION
–
–
See next slide
ISR WFC3 2009-30, 2009-31.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
77
WFC3_37, 38: (11450, 11451)
Figures show ratio of
observed to predicted
sensitivity. X axis is filter
pivot wavelength.
Top: UVIS sensitivity, GD
153. Dark filled circles are
wide and medium band
filters, grey x are narrow
band filters.
Right: IR sensitivity, GD
153 and P330E. Dark filled
circles are wide and
medium filters, grey x are
narrow band filters.
UVIS: 5-10% boost in efficiency at blue/red ’s, 15-20% at 400-700 nm
IR: 10-15% boost in efficiency at all ’s
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
78
WFC3
L.10.4.1.3 Calibration
•
SMOV4 REQUIREMENT: L.10.4.1.3.7
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
Obtain intflats with tungsten (UVIS & IR) & deuterium (UVIS) lamps.
Observe a) 47 TUC in UVIS (10 pointings per filter and in 3x3 bins) and IR (9 pointings each) and b) Omega
Cen in UVIS.
Obtain 10x full well and short tungsten flatfield exposures to “pin” CCDs
DESCRIPTION OF RESULTS
–
–
–
–
•
WFC3_19, 20, 39, 40, 44 (11432, 11433,11452,11453,11808)
DESCRIPTION OF METHODS
–
–
•
The flat field uniformity per pixel and cosmetic defect fraction shall be measured for both WFC3 detectors.
The ability to determine the residual response variation using the WFC3 internal calibration sources shall be
demonstrated. The difference between sky flats and internal flats and temporal stability of the flat field
correction shall be assessed.
Status = MET
UVIS: intflat features are stable, response variation across detector is ~1-2%, 3% in the UV
Pinning CCDs effectively mitigates QEH (Bowtie)
IR: response variation across detector is ~1.5%.
Temporal stability is better than 1%, Uniformity is between 1-2%.
SUPPORTING DOCUMENTATION
–
–
See charts on the next two slides
ISR WFC3 2009-19 , WFC3 2009-39, and in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
79
WFC3_39 (11452)
UVIS Channel
•
Omega Cen (F225W, F275W F336W, F438W, F606W, F814W) and
•
47 Tuc (F438W,F606W, F814W) using 10 pointings per filter, and 3x3 bins.
•
RMS scatter (in magnitudes)
–
–
–
–
–
–
F225W: 2.4%
F275W: 2.9%
F336W: 2.2%
F438W: 1.6%
F606W: 0.9%
F814W: 1.6%
For F606W, from Top to Bottom:
1st Panel: Chip 1,Rows 1360 and greater
2nd Panel: Chip 1,Rows 680-1360
3rd Panel: Chip 1,Rows < 680
4th Panel: Chip 2 ,Rows 1360 and greater
5th Panel: Chip 2,Rows 680-1360
6th Panel: Chip 2,Rows < 680
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
80
WFC3_40 (11453)
IR Channel
• 47 Tuc (F110W, F125W, F140W and F160W) at 9 dithered pointings.
Photometry variation of sources
across the detector (black dots),
along with binned means (red) in F160W
Plotted are Delta Mag vs. X position
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
81
WFC3_44 Bowtie (11808)
Intflat ratio from Visit 100:
before and after pinning flat
anneal
anneal
Intflat ratio levels since June 11,2009
Left: Image is the ratio of an internal flat before pinning to a flat after pinning from Visit 100
Right: Plot of Internal flat ratios before and after pinning during SMOV4: 2009 June 11 August 10. Pinning mitigates the bowties (QEH).
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
82
WFC3 Cross SI Light Leak Test
(L10.4.16.1 Prop. 11515)
•
•
•
UVIS exposure shows 3 stray light streaks
Horizontal streak contains 2 highly-structured, nearly identical blobs
There are no bright stars in the near field
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
83
No astronomical sources of stray
light in the HST FOV
84
All UVIS exposures contain stray
light & no IR exposures
•
6 UVIS exposures contain stray light
– 4 parallel with COS/NUV Tag Flash and
WAVE exposures
– 1 parallel with ACS Tungsten exposure
– 1 parallel with COS MIRRORA
exposure (should not be a source)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
85
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
86
Cosmic Origins Spectrograph
Charles D. (Tony) Keyes
COS SMOV4 REQUIREMENTS MATRIX
(slide 1 of 2)
SMOV4 RQMT RELEVANT ACTIVITY
L.10.4.2.1.1
COS01
L.10.4.2.1.2
COS23,04,08,05,24,31,34
L.10.4.2.1.3
COS23,06
L.10.4.2.1.4
COS02
L.10.4.2.1.5
COS03
L.10.4.2.1.6
COS04
L.10.4.2.1.7
COS23
L.10.4.2.1.8
COS14,29,31,16,19,09
L.10.4.2.1.9
N/A
L.10.4.2.1.10
COS08,09,22,23
L.10.4.2.1.11
COS06,10,07,23
L.10.4.2.2.1
COS19,34,36
L.10.4.2.2.2
COS22,04,23,07,06
L.10.4.2.2.3
COS22
L.10.4.2.3.1
COS05,06,07,10
L.10.4.2.3.2
COS08,09
L.10.4.2.3.3
COS09,13,19
L.10.4.2.3.4
COS08,09
L.10.4.2.3.5
see following
L.10.4.2.3.5.1
COS11,08,09
L.10.4.2.3.5.2
COS12,08,09
PROPOSAL ID
LSAFE01-04
11356,11355,11468,11466,11482,11489,11492
11356,11467
11353
11354
11355 v01-04
11356
11474,11487,11489,11486,11479,11469
N/A
11468,11469,RT,11356
11467,11496,11355v05,11356
11479,11492,11494
RT,11355v01-04,11356,11355v05,11467
RT
11466,11467,11355v05,[11470,11496]
11468,11469
11469,11473,11479
11468,11469
see following
11471,11468,11469
11472,11468,11469
TITLE
RQMT STATUS
Instrument States
MET
Detector States
MET
Data Interface and Data Transmission Verification
MET
On-board Memory Check
MET
Science Data Buffer Check
MET
MET
Test of NUV Detector Initial Turn-on and Recovery after Ano
MET
Test of FUV Detector Initial Turn-on and Recovery after Ano
Functionality and Operations of Detectors
MET
QE Enhancement Grid Tests
RQMT DELETED
Performance of Mechanisms
MET
Functionality of Lamps
MET
Contamination Management
MET
Upon release the COS instrument shall undergo a period o
MET
Opening of FUV Detector Door
MET
MET
Internal NUV calibrations shall be conducted and measurem
The relationship between the HST coordinate system and
MET
The locations of the spectra for each NUV mode shall be m
MET
The NUV channel shall be focused.
MET
MET
The target acquisition algorithms for NUV operations shall b
MET
NUV undispersed light target acquisition in ACQ/SEARCH a
MET
NUV dispersed light target acquisition in ACQ/SEARCH, A
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
88
COS SMOV4 REQUIREMENTS MATRIX
(slide 2 of 2)
SMOV4 RQMT
L.10.4.2.3.6
L.10.4.2.3.6.1
L.10.4.2.3.6.2
L.10.4.2.3.6.3
L.10.4.2.3.7
L.10.4.2.3.7.1
L.10.4.2.3.7.2
L.10.4.2.3.7.3
L.10.4.2.3.7.4
L.10.4.2.3.7.5
L.10.4.2.3.7.6
L.10.4.2.3.7.7
L.10.4.2.3.8
L.10.4.2.3.9
L.10.4.2.3.10
L.10.4.2.3.11
L.10.4.2.3.11.1
L.10.4.2.3.12
L.10.4.2.3.12.1
L.10.4.2.3.12.2
L.10.4.2.3.12.3
L.10.4.2.3.12.4
L.10.4.2.3.12.5
L.10.4.2.3.12.6
L.10.4.2.3.12.7
L.10.4.2.3.13
RELEVANT ACTIVITY
see following
COS13
COS13
COS13
see following
COS10,14,15
COS16,17,14
COS16,17,14
COS18
COS19
COS20
COS21
COS24,25,27,30
COS26
COS26,31
see following
COS28,26,34
see following
COS27,29,30
COS31
COS32
COS33,36
COS19
COS35
COS33,36
COS11,13,19,34,14,16,31,32
PROPOSAL ID
see following
11473
11473
11473
see following
11470,11474,11475
11476,11477,11474
11476,11477,11474
11478
11479,11481
11480
11481
11482,11483,[11485, 11496],11488
11484
11484,11489
see following
11486,11484,11492
see following
11485,11487,11488
11489
11490
11491,11494
11492, 11491, 11494
11493
11491,11494
11471,11473,11479,11492,
11474,11476,11489,11490
TITLE
RQMT STATUS
The imaging performance of the NUV channel shall be calib
MET
The PSF in NUV imaging (TA1) mode shall be measured.
MET
The plate scale of the NUV detector in imaging (TA1) mode
MET
MET
The throughput of the NUV imaging (TA1) mode shall be te
MET
The spectroscopic performance of the NUV channel shall be
The zero point offsets in the dispersion relations for the NUV
MET
MET
The spectral resolution of the NUV spectroscopic modes sh
MET
The spatial resolution of the NUV spectroscopic modes sha
The flat-field response of the NUV detector shall be measure
MET
The sensitivity of each NUV grating for each central wavele
MET
MET
The stability of a single mode of the NUV channel over seve
The acquisition of spectra having S/N>30 using normal data
MET
MET
Internal FUV calibrations shall be conducted and measurem
MET
The locations of the spectra for each FUV mode shall be me
The FUV channel shall be focused. This is done by conduct
MET
MET
The target acquisition algorithms for FUV operations shall b
MET
FUV dispersed light target acquisition in ACQ/SEARCH, AC
The spectroscopic performance of the FUV channel shall be
MET
MET
The zero point offsets in the dispersion relations for the FUV
MET
The spectral resolution of the FUV spectroscopic modes sh
The spatial resolution of the FUV spectroscopic modes sha
MET
MET
The flat-field response of the FUV detector shall be measure
MET
The sensitivity of each FUV grating for each central wavelen
The stability of a single mode of the FUV channel over seve
MET
MET
The acquisition of spectra having S/N>30 using normal data
The [FUV, NUV] position and [FUV, NUV] throughput of the
SMOV4 CLOSURE REVIEW
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MET
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.1 Instrument States
– COS entry into each of four instrument states (Boot, Hold, Operate, Observe)
shall be demonstrated. Operations shall be commanded via RIU (Remote
Interface Unit) commands transmitted over the Supervisory Bus.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS01 (no program ID; Scheduling Units LSAFE01 – 04 )
•
DESCRIPTION OF METHODS
–
•
DESCRIPTION OF RESULTS
–
•
After release, transition COS from SAFE mode through instrument states Hold, Boot, Operate, and Observe
in preparation for subsequent SMOV activities. The transition from SAFE to Hold used the nominal safing
recovery commanding. Transitions to all states higher than Hold were scheduled automatically as needed for
subsequent SMOV activities..
Scheduling Units LSAFE01 – 04 started execution on 2009.142:10:30:03.00. Engineering telemetry was
received from all modes. The telemetry was examined for correct relay states, voltages, temperatures,
currents, and logical values, positions, and memory values. Relay configurations were also validated with
CCS software tool MON CALC. The formal monitoring was done by the FOT (Flight Ops Team). John
Bacinski (GSFC) and Tom Wheeler also monitored. All transitions were successful without anomalies.
SUPPORTING DOCUMENTATION
–
Day 143 (22 May) morning report by GSFC
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.2 Detector States
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
No special program is designed to exercise these operational modes as routine operation during SMOV will
cause COS to enter each of the defined detector states. All are encountered in normal operation, although FUV
single-segment operation occurs relatively rarely.
• NUV detector states:
•
HOLD, Low Voltage ON (LVON), High Voltage ON (HVON),
•
and High Voltage in SAA (HVSAA)
• FUV detector states:
•
HOLD, BOOT, OPERATE, HV LOW, HV NOMINAL,
•
HV SEGMENT A, and HV SEGMENT B
DESCRIPTION OF RESULTS
–
•
COS23 (11356), COS04 (11355, v01-04), COS08 (11468), COS05 (11466), COS24 (11482),
COS31 (11489), COS34 (11492)
DESCRIPTION OF METHODS
–
•
COS entry into each of the defined detector states shall be demonstrated. Operations shall be
commanded via RIU commands transmitted over the Supervisory Bus.
Status = MET
Entry into all defined detector states occurred nominally. Single-segment operation was utilized in COS34 and
COS31. All other states were utilized repeatedly as part of routine operation.
SUPPORTING DOCUMENTATION
–
N/A
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.3 Data Interface and Data
Transmission Verification
– Science data transmission via the Science Data Formatter (SDF), shall be
verified by monitoring of normal configuration and science activities.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– All programs; e.g., COS23 (11356), COS06 (11467)
•
DESCRIPTION OF METHODS
– Examine any exposure with routine data-taking
•
DESCRIPTION OF RESULTS
– Some early SMOV visits of COS23 (11356 – FUV Initial HV Turn-on) and COS06
(NUV Functional) obtained dark and wavecal exposures; examination of data
products from those exposures was nominal
•
SUPPORTING DOCUMENTATION
– COS IS reports at SMOV morning meetings which discuss relevant data
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.4 On-board Memory Check
– The ability to load and dump on-board memory shall be demonstrated.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS02 (11353)
•
DESCRIPTION OF METHODS
–
This activity is a test and verification of the COS memory dump capability. With the DIB and
CS both in OPERATE, perform full dumps of the CS EEPROM, PROM, and EXEC RAM.
Then copy DIB data from DIB RAM and DIB PROM to CS Buffer RAM and dump the portion
of the CS Buffer RAM containing the DIB data as normal science images. Next, with the FUV
detector in its OPERATE state, copy the DCE RAM to CS Buffer RAM and dump the portion
of the CS Buffer RAM containing the DCE data as a normal science image.
– DESCRIPTION OF RESULTS
– No anomalies; all tests and memory compares successful.
•
SUPPORTING DOCUMENTATION
– 22 May 2009 summary memo (Kelly/Serrano) and HST daily status report
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.5 Science Data Buffer Check
– The ability to read and write data from and to the science data buffer shall be
demonstrated
– The science data buffer shall also be checked for bit flips during SAA passage.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS03 (11354)
•
DESCRIPTION OF METHODS
–
The COS Science Buffer RAM is checked for bit flips during SAA passages. This is followed
by a Control Section (CS) self-test consisting of writing/reading a specified bit pattern from
each memory location in Buffer RAM and a similar test for DIB RAM.
– DESCRIPTION OF RESULTS
– No anomalies; all tests and memory compares successful.
•
SUPPORTING DOCUMENTATION
– 26 May 2009 summary memo (Kelly/Serrano) and HST daily status report
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.6 Test of NUV Detector Initial Turnon and Recovery after Anomalous Shutdown
– The procedure used for initial turn-on and recovery after anomalous shutdown of
NUV MAMA detector shall be tested
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS04 (11355 v01-04)
•
DESCRIPTION OF METHODS
–
Initially turn-on, checkout and verify in a safe and controlled manner the proper operation of
the NUV MAMA detector. Three tests are employed to achieve this:
•
•
•
•
low-voltage only signal processing chain test
slow, intermediate high-voltage ramp with time-tag science image diagnostics
slow, full high-voltage ramp with time-tag science image diagnostics.
DESCRIPTION OF RESULTS
– NUV-MAMA successfully turned on. All engineering and science diagnostic data
were as expected – no problems encountered..
•
SUPPORTING DOCUMENTATION
– Morning status reports (31 May, 1 June, 4 June); TIR in preparation
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.7 Test of FUV Detector Initial Turnon and Recovery after Anomalous Shutdown
– The procedure used for initial turn-on and recovery after anomalous shutdown of
FUV XDL detector shall be tested.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS23 (11356)
•
DESCRIPTION OF METHODS
– Perform the initial high voltage turn on and ramp up in a slow and controlled way
in several visits over several days. Monitor and compare to normal values all
MCP metrics (HV currents, background rate, response to light, pulse height
distributions, etc.).
•
DESCRIPTION OF RESULTS
– Detector behavior was nominal during all ramps and exposures; all DCE dumps
nominal, normal turn-on transients occurred; all subsequent current histograms
nominal, no current transients occurred.
•
SUPPORTING DOCUMENTATION
– Various morning status reports (3-25 June); TIR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.8 (slide 1 of 2) Functionality and
Operations of Detectors
– Functionality and operations of the two COS detectors shall be demonstrated. This
shall include: a) the proper accumulation of signal over a specified time interval in
ACCUM and TIME-TAG readout mode, b) readout of subarrays, c) standard autowavelength calibration for ACCUM mode with the PSA and for TIME-TAG and
ACCUM mode with the Bright Object Aperture (BOA), d) TAGFLASH operational
mode (standard wavelength calibration for TTAG mode with the PSA), e) on-board
Doppler correction in ACCUM mode.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS14 (11474), COS29 (11487), COS31 (11489), COS16 (11486), COS19
(11479), COS09 (11469)
•
DESCRIPTION OF METHODS
– Tests include observations that
– a) compare the proper accumulation of signal over a specified time interval in
ACCUM & TIME-TAG readout mode;
– b) perform readout of subarrays;
– c) perform standard auto-wavelength calibration for ACCUM mode with PSA and for
TIME-TAG and ACCUM mode with the Bright Object Aperture (BOA) (FLASH=NO);
– d) use the TAGFLASH operational mode (the standard wavelength calibration for
TIME-TAG mode with the PSA) (FLASH=YES);
– e) perform on-board Doppler correction in ACCUM mode.
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.8 (slide 2 of 2) Functionality and
Operations of Detectors
– Functionality and operations of the two COS detectors shall be demonstrated.
– Status = MET
•
DESCRIPTION OF RESULTS
– ACCUM and TIME-TAG yield similar results;
– ACCUM exposures which proceed nominally verify subarray readouts;
– nominal PSA ACCUM and BOA TIME-TAG verify FLASH=NO wavelength
calibration;
• no BOA ACCUM data taken – no unique functionality is tested by this case which, for
FLASH=NO, is no different from TIME-TAG; FLASH=NO tested for TIME-TAG and
ACCUM with PSA
– nominal default TAGFLASH wavecal processing verifies FLASH=YES
processing;
– COS14 (11474) and COS29 (11487) analysis verifies ACCUM and TIME-TAG
doppler corrected spectra agree to 0.1 pixels for NUV and 0.7 pixels for FUV.
•
SUPPORTING DOCUMENTATION
– ISRs in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
98
COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.9 QE Enhancement Grid Tests
– The functionality of the FUV detector shall be tested with and without the QE
enhancement grid turned on; (a subsequent update has deleted this requirement
and any testing with grid off as COS will not operate with the grid off unless the
grid fails).
– Status = REQUIREMENT DELETED
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– Any SMOV program with FUV exposures, e.g., COS23 (11356) or COS25
(11483)
•
DESCRIPTION OF METHODS
– No special program is designed to test the QE grid as it is always on for any FUV
exposure. The grid will only be turned off if the grid suffers an anomaly or failure.
Any normal FUV data-taking exposure in which the detector is illuminated will
test the functionality of the grid.
•
DESCRIPTION OF RESULTS
– All operation is nominal.
•
SUPPORTING DOCUMENTATION
– N/A
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COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.10 Performance of Mechanisms
– The performance of the external shutter, Aperture Mechanism (ApM), Optics
Select Mechanisms OSM1 and OSM2, and FUV detector door shall be verified
either by execution of engineering tests or as part of normal SMOV operations.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
– COS08 (11468), COS09 (11469), COS22 (no program), COS23 (11356)
DESCRIPTION OF METHODS
–
•
DESCRIPTION OF RESULTS
–
•
Obtain observations, perform tests, or issue commands to exercise the external shutter,
aperture mechanism, OSM1, OSM2, and FUV detector door.
All objectives met; telemetry indicated, and subsequent exposures confirm, successful realtime FUV detector door opening; FUV and NUV wavecal observations indicate OSM1 and
OSM2 function properly; comparison of external exposures using coordinated POS-TARG
and aperture mechanism movements indicate successful aperture motion of proper
magnitude and direction
SUPPORTING DOCUMENTATION
– IS and SISE reports at various morning SMOV meetings
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
100
COS
L.10.4.2.1 Engineering Activities
•
SMOV4 REQUIREMENT: L.10.4.2.1.11 Functionality of Lamps
– The functionality of the COS Pt-Ne and D2 calibration lamps shall be verified
either by execution of engineering tests or as part of normal SMOV operations.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS06 (11467), COS10 (11496), COS07 (11355, v05), COS23 (11356)
•
DESCRIPTION OF METHODS
– Utilize engineering and normal SMOV activities to verify functionality of all lamps.
COS06 verifies Deuterium-1, COS07 verifies Deuterium-2, COS23 and COS06
verify PtNe-1, COS06 and COS10 verify PtNe-2.
•
DESCRIPTION OF RESULTS
– All lamps operate nominally.
•
SUPPORTING DOCUMENTATION
– Various COS IS reports at SMOV morning meetings
SMOV4 CLOSURE REVIEW
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101
COS
L.10.4.2.2 Contamination
•
SMOV4 REQUIREMENT: L.10.4.2.2.1 Contamination Management
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Observe BEA during early SMOV period; commence during SMOV the initial epochs of
routine periodic UV throughput monitoring observations using HST spectrophotometric
standard stars.
DESCRIPTION OF RESULTS
–
–
–
•
COS19 (11479), COS34 (11492), COS36 (11494)
DESCRIPTION OF METHODS
–
•
COS operations shall be managed to minimize the risk of contamination of its optical
surfaces by outgassing material. The COS external shutter shall be used to provide
protection against illumination by the bright earth. A contamination monitor program shall be
initiated as soon as possible after the servicing mission (COS CARD item 3.4.12.20).
Status = MET
All objectives met; no external observations in BEA period;
external shutter operates nominally on external observations; noted in review of SIC&DH
anomaly that shutter is not automatically closed in event of an SI safing
FUV and NUV sensitivity monitor observations commenced following optical alignment,
observational characteristics coordinated with continuing cycle 17 programs.
SUPPORTING DOCUMENTATION
–
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
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COS
L.10.4.2.2 Contamination
•
SMOV4 REQUIREMENT: L.10.4.2.2.2 (page 1 of 2) Upon release the COS instrument shall
undergo a period of depressurization and decontamination.
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
–
–
a) The FUV detector door shall not be opened until the COS internal pressure is less than 100 micro-Torr for 12
consecutive hours.
b) The NUV MAMA detector HV shall not be turned on until the internal pressure is less than 20 micro-Torr for
12 consecutive hours and the MAMA has been operated at LV for at least 12 consecutive hours.
c) The FUV XDL detector HV shall not be turned on until the internal pressure is less than 10 micro-Torr for 12
consecutive hours.
d) The D2 and Pt-Ne lamps shall not be operated until the internal pressure is less than 10 micro-Torr for 12
consecutive hours.
DESCRIPTION OF RESULTS
–
•
Door: COS22 (no program); COS04 (11355 v01-04), COS23 (11356), COS07 (11355 v05), COS06 (11467)
DESCRIPTION OF METHODS
–
•
COS CARD items 2.4.12.3, 2.4.12.4, 2.4.12.7, 2.4.12.8, 3.14.12.14 – listed on following slide
Status = MET
All objectives met. The FUV DVA door was commanded open successfully at 15:20 UT day 2009.142 (22-May2009). As expected a small, brief pressure rise was noted on the COS and NCS pressure gauges (see next
slide). For all pressure-related activity thresholds (see above) COS pressure was substantially below the
required threshold.
SUPPORTING DOCUMENTATION
–
SMOV morning status reports (23 May [FUV Door], 2 June [NUV HV], 5 June [FUV HV and lamps])
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COS
L.10.4.2.2 Contamination
•
SMOV4 REQUIREMENT: L.10.4.2.2.2 (page 2 of 2) Upon release the COS instrument shall
undergo a period of depressurization and decontamination.
–
–
–
–
–
–
Text of relevant COS CARD items:
2.4.12.3: a.) No High Voltage (HV) on a MAMA detector shall be set to a magnitude greater than 50 volts
unless the measured pressure is less than 2x10-5 torr for 12 hours.
2.4.12.4: a.) The MAMA Low Voltage (LV) must be enabled for 12 hours continuously before performing a
MAMA High Voltage Ramp in vacuum after exposure of the MAMA to a non-vacuum environment (launch or
ground testing).
2.4.12.7: a.) On-orbit, the Far Ultra Violet (FUV) Detector Door must not be opened until the following
condition is met: The COS on-board pressure gauge must read a pressure less than 1x10-4 torr for 12
consecutive hours.
2.4.12.8: a.) On-orbit, the FUV detector HV must not be turned on until the following conditions are met:
First the FUV Detector Door must be successfully opened, and second, the COS on-board pressure gauge
must read a pressure less than 1x10-5 torr for 12 consecutive hours.
3.14.12.14: a.) The D2 and PtNe lamps should not be operated in vacuum if contamination sources are
present in the calibration subsystem. Pressure measured by the COS on-board pressure gauge should be
below 1x10-5 torr for 12 hours minimum before operation of the lamp.
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COS
L.10.4.2.2 Contamination
•
SMOV4 REQUIREMENT: L.10.4.2.2.2 Upon release the COS instrument shall
undergo a period of depressurization and decontamination --- STATUS=MET
COS and NCS Pressure
7E-06
6E-06
5E-06
Pressure (Torr)
 COS (LVACPRES)
 NCS (METPSPR)
NUV “fold”
(lamps)
4E-06
3E-06
FUV door
open
NUV initial
turn-on
FUV turn-on
2E-06
1E-06
0E+00
5/22
5/24
5/26
5/28
5/30
6/01 REVIEW
6/03
SMOV4 CLOSURE
Nov.
18, 2009
2009
(UT)
6/05
6/07
6/09
6/11
6/13
6/13
105
COS
L.10.4.2.2 Contamination
•
•
•
SMOV4 REQUIREMENT: L.10.4.2.2.3 Opening of FUV Detector Door
– The HV of the FUV XDL detector and the NUV MAMA detector shall be off when
the FUV detector door opens in case of release of gases during the opening of
the door.
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS22 (no program)
DESCRIPTION OF METHODS
– FUV door opening is a real-time activity.
•
DESCRIPTION OF RESULTS
– All objectives met; door opened successfully. The FUV DVA door was
commanded open at 15:20 UT day 2009.142 (22-May-2009). As expected a
small, brief pressure rise was noted on the COS and NCS pressure gauges.
•
SUPPORTING DOCUMENTATION
– Telemetry; SMOV morning meeting (23 May)
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.1 (slide 1 of 3) Internal NUV calibrations shall
be conducted and measurements of the post-launch alignment of the optics shall
be obtained
–
–
These include: a) a detector dark image, b) an internal wavelength calibration spectrum using
each NUV grating at each central wavelength setting, c) a TA1 image of the wavelength
calibration lamp, d) intensity of each lamp in a single mode.
Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
DESCRIPTION OF METHODS
–
COS05 (11466), COS06 (11467), COS07 (11355 v05), COS10 (11470, 11496)
–
–
Various internal calibrations to assess the post-launch alignment include
a) a detector dark image;
–
b) an internal wavelength calibration spectrum using each NUV grating at each central
wavelength setting;
c) a TA1 image of the wavelength calibration lamp;
d) intensity of each lamp in a single mode.
–
–
•
•
•
•
COS05: Collect long science exposures with the shutter closed and no light on the NUV detector to verify
nominal operation of the detector. Note variations in the dark rate as a function of time and position in the
orbit. Determine the suitability of the current SAA model.
COS06: Verify the functionality and operation of the NUV detector and lamps: obtain a 60-second
deuterium lamp 1 exposure, then wavecal exposures for G185M, G225M, G285M, G230L, MIRRORA, and
MIRRORB with both Pt/Ne lamps.
COS07: NUV fold test uses deuterium lamp 2 as input source.
COS10: Obtain NUV wavecal exposures with PtNe lamp 2 and both mirror settings to establish
performance characteristics;
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.1 (slide 2 of 3) Internal NUV
calibrations shall be conducted and measurements of the post-launch
alignment of the optics shall be obtained
– Status = MET
•
DESCRIPTION OF RESULTS:
– All objectives met.
– COS05: Dark rate away from the SAA is ~65 counts/sec, which is significantly
below prelaunch predictions. Dark rate near the SAA can be substantially higher,
particularly on the western edge (see figure on slide 3 for L.10.4.2.3.8). The SAA
model will be modified in order to better reflect the actual count rate distribution
with position in the orbit.
– COS06, COS10: NUV detector collects and saves data as expected. All lamps
work and have expected fluxes. OSM drift still present.
– COS07: All deuterium lamp 2 exposures nominal; the fold distribution was
compared to previous ground-based fold tests and was found to be consistent
and within expected tolerances. All performance was nominal.
•
SUPPORTING DOCUMENTATION
– ISRs, TIR in preparation
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.3 Science Verification & Calibration
SMOV4 REQUIREMENT: L.10.4.2.3.1 (slide 3 of 3) --- Status = MET
COS05: NUV Darks
(Program 11466)
COS NUV Dark Evolution
– Dark count has increased
from ~70 cts/sec over
entire detector area to
showing signs of leveling
off ~150 cts/sec in midOctober
– Possibly increased
population of metastable
states in detector faceplate
– Remains below initial onorbit predictions based on
ground data (~225 cts/sec)
– Regular monitoring
continues in Cycle 17
Days since launch
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.2 (slide 1 of 3) The relationship
between the HST coordinate system and the COS primary science aperture
(PSA) shall be measured. The NUV channel in the TA1 mode shall be used to
locate the PSA in the HST V2, V3 coordinates.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS08 (11468), COS09 (11469)
•
DESCRIPTION OF METHODS
–
–
–
•
DESCRIPTION OF RESULTS
–
–
•
MIRRORA NUV images of NGC188 astrometric target with astrometric GS used to locate the
PSA in FGS frame (HST V2, V3 coordinates).
Verify coordinates
Effect coarse alignment and focus of NUV channel in COS08 (11469); fine alignment completed
in COS09 (11469)
All objectives met; SIAF update completed on day 215
Exceptions: Additional visit (91) added when POS-TARG frame found to be inverted
SUPPORTING DOCUMENTATION
– ISR in preparation; SIAF update
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110
COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.2 (slide 2 of 3) The
relationship between the HST coordinate system and the COS
primary science aperture (PSA) shall be measured.
– Status = MET
Upper figure: Program 11468 visit 01 pointing (initial
COS blind pointing) aperture location; Lower figure:
after initial derived aperture location offset, first
11469 visit 01 pointing and subsequent refined offset
update
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.2 (slide 3 of 3) The relationship
between the HST coordinate system and the COS primary science
aperture (PSA) shall be measured. --- Status = MET
Target Acquisition
Slew Analysis
– Includes all
centering slews in
all target acquisition
sequences
– Cumulative centroid
continues to be at
approximately +0.3
arcsec in both
along-dispersion
(AD) and crossdispersion (XD)
directions; sigma
~0.4 arcsec in both
coordinates
– No clear indication
of time-evolution of
centroid
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.3 The locations of the spectra for
each NUV mode shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS09 (11469), COS13 (11473), COS19 (11479)
•
DESCRIPTION OF METHODS
– Observe an astronomical target, acquire a spectrum using G185M, G225M,
G285M, and G230L gratings, as well as a TA1 image..
•
DESCRIPTION OF RESULTS
– All objectives met; determined location of spectrum extraction boxes and verifies
target acquisition offset parameters.
•
SUPPORTING DOCUMENTATION
– ISR in preparation; spectrum location reference file; updates to TA parameters in
commanding tables
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113
COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.4 The NUV channel shall be
focused. Conduct a focus scan of each of the NUV gratings at one central
wavelength setting and of the TA1 mirror while observing an astronomical
target.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
DESCRIPTION OF METHODS
•
DESCRIPTION OF RESULTS
•
SUPPORTING DOCUMENTATION
– COS08, COS09 (11468, 11469)
– Use MIRRORA NUV PSA images of astrometric target with astrometric GS for all
observations; all NUV spectral elements are confocal.
– Determine COS optical axis in FGS frame; align aperture to that axis
– Optimize focus and correct alignment to NUV collimator
– All objectives met; NUV imaging performance excellent; as all NUV optical
elements are confocal, no grating focus sweep is required; completed by date of
HST OTA focus adjustment (day 201); SIAF update completed on day 215
– Comment: Additional visits added due to GS hand-off, POS-TARG error,
confirmation of OTA SM focus
– ISR in preparation; SIAF update
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.4 The NUV channel shall be
focused.
– Status = MET
Program 11469 visit 94 [final COS focus verification sweep (post HST
secondary move)]; left: final aperture center location; middle: LSF at
optimum focus; right: PSF width focus sweep
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.5 The target acquisition algorithms for NUV operations shall be tested and verified
•
•
•
•
SMOV4 REQUIREMENT: (slide 1 of 2)
L.10.4.2.3.5.1 NUV undispersed light target acquisition in ACQ/SEARCH and
ACQ/IMAGE mode shall be tested. --- Status = MET
L.10.4.2.3.5.2 NUV dispersed light target acquisition in ACQ/SEARCH,
ACQ/PEAKD and ACQ/PEAKXD mode shall be tested. --- Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
COS11 (11471), COS12 (11472), COS08 (11468), COS09 (11469)
DESCRIPTION OF METHODS
–
–
–
–
COS08: Perform initial ACQ/SEARCH and ACQ/IMAGE TA assessment
COS09: Continue initial testing and validation of all phases of TA; acquire data to assess all
patchable TA parameters
COS11: Program will verify that the COS target acquisition (TA) flight software (FSW) can
properly identify the centroid of a point source in its field and then move that centroid to the
center of the aperture. Four modes will be verified; PSA and BOA for both MIRRORA and
MIRRORB.
COS12: This program will verify the ability of the COS TA FSW to place an isolated point
source at the center of the aperture, both for the BOA and PSA, with dispersed light from the
object using an NUV grating and all available centering and stripe options {CENTER=fluxweighted (FW); flux-weighted-floored (FWF); return to brightest (RTB) and STRIPE=DEF
(medium); short; medium; long}.
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.5 The target acquisition algorithms for NUV operations shall be tested and verified
•
•
•
•
SMOV4 REQUIREMENT: (slide 2 of 2)
L.10.4.2.3.5.1 NUV undispersed light target acquisition in ACQ/SEARCH and ACQ/IMAGE mode
shall be tested. --- Status = MET
L.10.4.2.3.5.2 NUV dispersed light target acquisition in ACQ/SEARCH, ACQ/PEAKD and
ACQ/PEAKXD mode shall be tested. --- Status = MET
DESCRIPTION OF RESULTS
– COS08: Errors found in ACQ/SEARCH FSW and ACQ/IMAGE plate-scale sign convention;
corrected plate-scales and disabled usage of background threshold parameter
– COS09: Determined updates to nearly all patchable TA quantities including plate-scales,
extraction boxes, aperture offsets
– COS11: All modes tested and verified. Refined WCA-to-PSA/BOA offsets for ACQ/IMAGE;
refined search box locations for PSA/BOA MIRRORA/MIRRORB.
•
–
COS12: All modes tested and verified; refined extraction boxes, plate-scales, and spectrum
locations for dispersed light TA.
•
•
Some modes were determined to have different signal-to-noise (S/N) requirements. BOA observations
should be observed to S/N of 60 (3600 counts) because the BOA smears the light over many more
pixels than the PSA.
Comment: There are known minor centering errors (1-2p in cross-dispersion) when using a stripe
other than stripe=B (DEF) due to only one FSW parameter relating the WCA to PSA stripe offsets,
whereas the actual offsets are stripe dependent. Once the final NUV wavelength solutions are in
calcos, additional verifications of the centering in the along-dispersion direction are planned.
SUPPORTING DOCUMENTATION
–
Parameter updates implemented through commanding table updates; ISR in preparation
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.6 The imaging performance of the NUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT:
L.10.4.2.3.6.1 The PSF in NUV imaging (TA1) mode shall be measured
–
•
•
•
Status = MET
L.10.4.2.3.6.2 The plate scale of the NUV detector in imaging (TA1) mode shall be
measured --- Status = MET
L.10.4.2.3.6.3 The throughput of the NUV imaging (TA1) mode shall be tested both
in mirror A and mirror B configurations --- Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
COS13 (11473)
•
DESCRIPTION OF METHODS
•
DESCRIPTION OF RESULTS
•
SUPPORTING DOCUMENTATION
–
–
–
–
–
–
Obtain PSA and BOA NUV MIRRORA and MIRRORB images of HST spectrophotometric standard stars.
Obtain PSA MIRRORA TAGFLASH images at numerous POS-TARG offset locations in aperture. Measure
PSF in NUV imaging mode; measure plate scale in NUV imaging mode; measure imaging throughput in
MIRRORA as well as MIRRORB configurations
PSF was measured in NUV imaging mode throughout full COS PSA aperture
Plate scale in NUV imaging mode was measured for PSA aperture
(0.0238 ± 0.0002 arcsec/pixel)
Imaging throughput results for PSA/MIRRORA, PSA/MIRRORB, BOA/MIRRORA, and BOA/MIRRORB
configurations were implemented in synphot as well as calcos.
Synphot reference file delivery; calcos throughput parameter update; ISR in preparation
SMOV4 CLOSURE REVIEW
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.1 (Slide 1 of 2) The zero point
offsets in the dispersion relations for the NUV spectroscopic modes for each
central wavelength setting shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS10 (11470), COS14 (11474), COS15 (11475)
•
DESCRIPTION OF METHODS
– COS10: Establish the limits of the initial wavelength scales in order to determine
if adjustments are necessary.
– COS14: Observe external radial velocity standard stars with all NUV gratings
and central wavelengths at default FP-POS; observe at all FP-POS for at least
one central wavelength of each grating. Obtain zero-point offsets for the
wavelength scale (internal wavecal lamp scale to external standard wavelength
scale) for all central wavelengths.
– COS15: Verification of the wavelength ranges after any adjustments resulting
from programs 11470 or 11474. Obtain lamp spectra at all grating/cenwave/FPPOS in order to update lamp template reference file.
SMOV4 CLOSURE REVIEW
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119
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.1 (Slide 2 of 2) The zero point offsets in the
dispersion relations for the NUV spectroscopic modes for each central wavelength
setting shall be measured
– Status = MET
DESCRIPTION OF RESULTS
– COS10: Encoder position for G285M/2695 was increased by 3 steps in order to
have complete coverage of Mg II doublet (2796 Å, 2803 Å) in stripe C, as
specified in OP01.
– COS14: Offsets between WCA and PSA data measured for G225M and G285M
using data from vis 01 (HD187691). Used high-resolution STIS echelle spectra
for comparison when possible
• Relative agreement between COS and STIS ~0.0100 Å; absolute STIS wavelength
accuracy ~0.5-1 pixel (0.0056 Å)
•
– COS15: Verified that desired wavelength ranges were obtained, in particular for
G285M/2695, for which OSM2 was adjusted. Lamp template reference file was
produced, containing lamp spectra at all FP-POS, for all NUV grating/cenwave
modes. Measured offsets between lamp template from TV03 and the new lamp
template (for FP-POS=3; needed to update wave. disp. ref file)
SUPPORTING DOCUMENTATION
–
pipeline reference file deliveries; ISR in preparation
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120
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
L.10.4.2.3.7.1 The zero point offsets in the dispersion relations for the NUV
spectroscopic modes for each central wavelength setting shall be measured
SMOV-to-TV03 PSA-to-WCA offset differential for G285M (left) and G225M (right)
as determined from COS14 (11474) radial velocity standard star observations.
Differential is constant for all central wavelength settings of a grating.
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT: (slide 1 of 2)
L.10.4.2.3.7.2 The spectral resolution of the NUV spectroscopic modes shall be
measured
–
•
L.10.4.2.3.7.3 The spatial resolution of the NUV spectroscopic modes shall be
measured
–
•
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Status = MET
COS16 (11476), COS17 (11477), COS14 (11474)
DESCRIPTION OF METHODS
–
–
COS16: To evaluate spectral resolution observe absorption line targets at the central
wavelength of each NUV grating through both PSA and BOA apertures. We also obtained
spectra at spatially offset positions to evaluate the effect of small pointing errors on the
spectral resolution.
COS17: Utilize an emission line target to verify the NUV spatial resolution and plate scale; to
characterize the interdependence of the spectral and spatial resolution; and to quantify the
variation of the spatial profile of a source with off-axis position by measuring variations in
shape, width and flux of the profile as the source is stepped past the aperture.
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
•
•
•
SMOV4 REQUIREMENT: (slide 2 of 2)
L.10.4.2.3.7.2 The spectral resolution of the NUV spectroscopic modes shall be
measured --- Status = MET
L.10.4.2.3.7.3 The spatial resolution of the NUV spectroscopic modes shall be
measured --- Status = MET
DESCRIPTION OF RESULTS
–
–
•
COS16: The spectral resolution meets CEI spec and matches well what was measured
during the thermal-vacuum tests in 2003 and 2006. Due to low S/N in the observed spectra
for COS16, data from other SMOV programs have also been included to provide a more
complete coverage.
COS17: Analysis indicates that displacements in cross-dispersion result in significant shifts
along dispersion, while displacements in dispersion produce only small shifts in crossdispersion. A displacement of 0.5’’ in cross-dispersion produces a shift of ~ 2.5 pixels (1
resel) in dispersion in G185M, G225M and G285M, with negligible shift in G230L. These
results are in line with predictions from target acquisition simulations (TAACOS), and are a
part of the optical design. Results are inconsistent with a simple rotation of spectrum relative
to the detector, since the axes defined by the POSTARGs are not perpendicular. We have
calculated plate scale coefficients and measured the spatial resolution for all four NUV
gratings, and find values consistent with prelaunch predictions.
SUPPORTING DOCUMENTATION
–
ISR in preparation
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123
L.10.4.2.3.7.2 The spectral resolution
of the NUV spectroscopic modes shall
be measured --- Status = MET
NUV PSA Resolution:
LEFT: Solid symbols are from Thermal_Vac 2006,
the open symbols are from SMOV COS16and the
line indicates the CEI specification.
ABOVE: Spectral resolving power, R, defined as
wavelength divided by FWHM of profile; dotted: R
for model LSF without MFWFE typically ~2 pixel
FWHM, solid: R for wavelength-dependent model
LSF FWHM with MFWFE
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L.10.4.2.3.7.2 The spectral resolution of the NUV spectroscopic modes shall be measured
Plate Scales in pixels/arcsecond
G185M
G225M
G285M
G230L
αYY
42.0
43.2
41.0
41.7
αYX
-0.3
…
…
…
αXY
-4.7
-6.7
-5.9
-0.2
αXX
41.3
…
…
…
AG Dra
G185M: Si III] 1890 Å (Stripe B)
G225M: He II 2733 Å (Stripe B)
G285M: He II 2385 Å (Stripe B)
NUV PSA: Dispersion/Cross-dispersion Shifts in
He 2-38
Emission Line Spectra of AG Dra and He 2-38
G230L: C III 1909 Å (Stripe C,
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125
2nd order)
Nov. 18, 2009
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.4 The flat-field response of the NUV detector
shall be measured
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Using the internal deuterium lamp create a deep on-orbit flat field image with a signal-to-noise
ratio high enough to allow flat fielding of science exposure to a level of 30:1 per resolution
element. A comparison to the NUV ground flat file will inform the decision whether it can be used
for pipeline processing.
DESCRIPTION OF RESULTS
–
–
•
COS18 (11478)
DESCRIPTION OF METHODS
–
•
Status = MET
Over 200 counts per pixel were obtained in the combined flat field. This produced S/N > 36 per
resolution element. Divisions with the ground flat showed no residual structure and photon
statistics recovered in the on-orbit flat. Thus it was determined that the ground flat, combined
with the new on-orbit data, can be used for pipeline processing.
The science stripes are vignetted in the first ~160 pixels, in a linear fashion, with up to a 20%
decrease in flux at the edge of the detector. Detailed fits of the vignetting have been made and
incorporated into the flat field image. A single fit is currently used, though this may leave
residuals up to ~2% in the M gratings and ~6% in the L grating (multiple updated flat fields are
currently being prepared).
SUPPORTING DOCUMENTATION
–
ISR in preparation
SMOV4 CLOSURE REVIEW
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126
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.4 The flat-field response of the NUV
detector shall be measured
– Status = MET
NUV Flat Field: ABOVE: On-orbit observations contain ~200 counts/pixel (S/N~36
per resel); ground flat observations obtained ~12,000 counts/pixel. Divisions with
the ground flat showed no residual structure and photon statistics recovered in the
on-orbit flat. The ground flat, combined with the new on-orbit data, is currently
being used for pipeline processing. RIGHT: NUV M grating vignetting profile.
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.5 The sensitivity of each NUV
grating for each central wavelength setting shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS19 (11479, 11481)
•
DESCRIPTION OF METHODS
– Establish COS PSA sensitivity versus wavelength over the entire observable
spectrum for all NUV gratings and central wavelength settings by observing HST
spectrophotometric standard stars to determine the initial on-orbit COS NUV
spectroscopic sensitivity.
•
DESCRIPTION OF RESULTS
– Sensitivity curves have been produced for all PSA settings (on-orbit sensitivities
are within 10-20% of ground values - see attached figures). BOA results are
presented separately (see req. L.10.4.2.3.13)
•
SUPPORTING DOCUMENTATION
– Reference files delivered to CDBS; ISR in preparation
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128
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
Combination of all of the data from program 11479 for the central wavelengths of each NUV grating (clockwise from upper left,
G185M, G225M, G230L, and G285M). Red = data from stripe A, black = data from stripe B and blue = data from stripe C. A
separate sensitivity curve was derived for each stripe which included all central wavelengths. For the G230L the upturn in the
SMOV4due
CLOSURE
REVIEW
apparent sensitivity on stripe B from 3200 - 3600A is actually
to second
order light from 1600 - 1800 A. Stripe C is all129
second
Nov. 18, 2009
order light with a small amount of first order contamination.
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.6 The stability of a single mode of the NUV
channel over several orbits shall be characterized to determine if there are signatures of
structural or thermal distortions in the data.
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
The goal of this program is to measure OTA-COS pointing jitter and OSM drift over time scales of seconds to
hours. NUV spectroscopy and MIRRORA imaging are tested with PSA after precise target acquisition. Fiveorbits each consisting of a single TIME-TAG exposure with TAGLFLASH lamp flashes every 200 seconds are
employed.
DESCRIPTION OF RESULTS
–
•
COS20 (11480)
DESCRIPTION OF METHODS
–
•
Status = MET
CEI stability specs are achieved (e.g., systematic drift: <1 resel [~3 pixels] per hour correctable to 0.25 resel
[0.75 pixels] per hour and random drift: <0.25 resel (0.75 pixels) contribution to FWHM). For the spectral
exposure, from the initial position we measure aggregate shifts in the dispersion and cross-dispersion
dimensions of (+1.05,+0.3), (+1.25,+0.45), and (+1.3,+0.5) pixels after 1, 2 and 5 orbits respectively. For the
imaging observation the aggregate shifts after 1, 2 and 5 orbits were (+1.5,+0.3), (+2.3,+0.55 ), and
(+2.6,+0.75) pixels respectively. The CALCOS measure of these shifts via the overlaid TAGFLASH exposures
agree within <0.3 pixels. There is also an orbital-period oscillation of the positions with amplitude ~0.5 pixels.
SUPPORTING DOCUMENTATION
–
ISR in preparation
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
L.10.4.2.3.7.6 The stability of a single mode of the NUV channel over several orbits shall be
characterized to determine if there are signatures of structural or thermal distortions in the
data.
– 5 CVZ orbit timeseries sampled in
120-second bins
– He II 2205 line
centroid in each bin
– ~0.5 pixel amplitude
orbital variation
along dispersion
– Cumulative drift of
~1.3 pixels along
dispersion
– WCA lamp flash
every 200 sec
– PSA drifts and
oscillations agree
with WCA line
positions to within
0.3 pixels
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.7.7
–
–
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Obtain HST spectrophotometric standard star observations at all FP-POS for at least one central wavelength of
one M mode grating to accumulate high count levels sufficient to demonstrate S/N>100 per resel and, for one
central wavlength of each grating, to demonstrate >30 in individual FP-POS exposures using normal data
acquisition and reduction techniques. Evaluate limiting S/N after FP-POS processing and/or flat fielding.
DESCRIPTION OF RESULTS
–
–
•
COS21 (11481)
DESCRIPTION OF METHODS
–
•
The acquisition of spectra having S/N>30 using normal data acquisition and reduction
techniques shall be demonstrated for each NUV mode.
Status = MET
Spectra having S/N>100 for a single NUV medium resolution mode shall be demonstrated.
Status = MET
Observations of G191B2B produced high signal-to-noise data sets, with individual exposures of S/N up to 80 per
3-pixel resel and spectra combined from 4 FP-POS settings reaching S/N >150 per 3-pixel resel. The analysis
shows that spectra should be able to reach a limiting S/N > 230.
Only the Stripe C spectra on the G230L data did not achieve S/N>30 per resel in the combined spectra and time
allotted due to all counts in this region being much lower throughput second-order spectra. G230L Stripe C
results are consistent with reaching S/N=30 if more time.
SUPPORTING DOCUMENTATION
–
ISR in preparation
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COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.7 The spectroscopic performance of the NUV channel shall be calibrated
• SMOV4 REQUIREMENT: L.10.4.2.3.7.7
– The acquisition of spectra having S/N>30 using normal data acquisition and
reduction techniques shall be demonstrated for each NUV mode.
– Status = MET
– Spectra having S/N>100 for
a single NUV medium
resolution mode shall be
demonstrated.
– Status = MET
– Co-add four FP-POS
spectra of same target
– Demonstrates S/N per
resel in excess of 100:1
for all M mode gratings
– Poisson S/N can be
recovered up to
approximately 70:1
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.8 (slide 1 of 2) Internal FUV calibrations
shall be conducted and measurements of the post-launch alignment of the
optics shall be obtained
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
These include: a) a detector dark image, b) an internal wavelength calibration spectrum
using each FUV grating at each central wavelength setting, c) intensity of each lamp in a
single mode.
Status = MET
COS24 (11482), COS25 (11483), COS27(11485, 11496), COS30 (11488)
DESCRIPTION OF METHODS
–
a) detector dark image;
•
–
–
COS24: Collect long science exposures with the shutter closed and no light on the FUV detector to
verify nominal operation of the detector. Note variations in the dark rate and pulse heights as a
function of time and position in the orbit. Determine the suitability of the current SAA model.
b) an internal wavelength calibration spectrum using each FUV grating at each central
wavelength setting;
c) intensity of each lamp in a single mode.
•
COS25, COS27, COS30: Verify the functionality and operation of the FUV detector and lamps: obtain
a 60-second deuterium lamp 1 exposure, then wavecal exposures for G130M, G160M, and G140Lwith
both Pt/Ne lamps, and finally 120-sec PtNe lamp 1 exposures at every FUV central wavelength and
FP-POS. Make an initial assessment of OSM drift by taking a long exposure with regular lamp flashes.
Deuterium lamp 2 is not used.
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COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.8 (slide 2 of 2) Internal FUV
calibrations shall be conducted and measurements of the post-launch
alignment of the optics shall be obtained
– Status = MET
•
DESCRIPTION OF RESULTS
– COS05: Dark rate away from the SAA is ~15 counts/sec/segment. Dark rate near
the SAA can be substantially higher, particularly on the western edge. The SAA
model will be modified in order to better reflect the actual count rate distribution
with position in the orbit.
– COS25, COS27, COS30: FUV detector collects and saves data as expected.
OSM drift still present. All tested lamps work and have expected fluxes.
– EXCEPTION: Deuterium lamp 2 is not used. NOTE: Deuterium lamp 2 was
successfully tested with NUV and produced nominal output. Lamp 2 is the
backup lamp, and deuterium lamps are not planned for use with FUV detector for
any science-related purpose.
•
SUPPORTING DOCUMENTATION
– ISRs, TIR in preparation
SMOV4 CLOSURE REVIEW
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135
COS
L.10.4.2.3 Science Verification & Calibration
SMOV4 REQUIREMENT: L.10.4.2.3.8 Internal FUV calibrations shall be conducted and
measurements of the post-launch alignment of the optics shall be obtained --- Status =
MET
COS24: FUV Darks (Program 11482)
– Throughout SMOV mean dark count obtained away
from the vicinity of the SAA remained steady at ~15
cts/sec/segment (lower envelope of points in plot)
– Dark rate near the SAA can be substantially higher,
particularly on the western edge. Many of the
samples in the plot are from near-SAA tracks that
were employed to map out SAA in SMOV
COS FUV Dark
Days since launch
SMOV4 CLOSURE REVIEW
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136
COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.9 The locations of the spectra for
each FUV mode shall be measured.
– This is done by observing an astronomical target and acquiring a spectrum using
G130M, G160M, and G140L gratings.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS26 (11484)
•
DESCRIPTION OF METHODS
– Observe an astronomical target, acquire a spectrum using G130M, G160M, and
G140L gratings.
•
DESCRIPTION OF RESULTS
– All objectives met; determined location of spectrum extraction boxes and verifies
target acquisition offset parameters.
•
SUPPORTING DOCUMENTATION
– ISR in preparation; spectrum location reference file; updates to TA parameters in
commanding tables
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
137
COS
L.10.4.2.3 Science Verification & Calibration
•
SMOV4 REQUIREMENT: L.10.4.2.3.10 The FUV channel shall be
focused. Conduct a focus scan of each of the FUV gratings at one central
wavelength setting while observing an astronomical target.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS26 (11484), COS31 (11489)
•
DESCRIPTION OF METHODS
– Conduct a focus scan of each of the FUV gratings at one central wavelength
setting while observing an external target with suitably narrow lines.
– Optimize focus of each FUV grating
– Validate with separate target to check resolution, LSF
•
DESCRIPTION OF RESULTS
•
SUPPORTING DOCUMENTATION
– All objectives met; FUV focus characterized
– Exceptions: Additional visits added to improve focus determination after v1,2
target found insufficient; LSF wings stronger than expected in COS31 validation
observations
– ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
138
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.10 The FUV channel shall be focused --- Status = MET
G130M
-294
G160M
-198
Left: G130M focus sweep data (11484 visit 93);
Right: G140L focus sweep data from 11484 visit 03
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
139
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.11 The target acquisition algorithms for FUV operations shall be tested and verified
•
SMOV4 REQUIREMENT: L.10.4.2.3.11.1 (slide 1 of 2) FUV dispersed
light target acquisition in ACQ/SEARCH, ACQ/PEAKD and
ACQ/PEAKXD mode shall be tested
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS28 (11486), COS26 (11484), COS34 (11492)
•
DESCRIPTION OF METHODS
– COS34: Perform initial FUV TA tests with launch values of TA parameters
– COS26: Evaluate first updates of FUV TA parameters
– COS28: Verify the ability of the COS FSW to place an isolated point source at
the center of the aperture, both for the BOA and PSA, using dispersed light from
the object with the FUV gratings. The various options for target centering should
be exercised and shown to work properly.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
140
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.11 The target acquisition algorithms for FUV operations shall be tested and verified
•
•
SMOV4 REQUIREMENT: L.10.4.2.3.11.1 (slide 2 of 2) FUV dispersed
light target acquisition in ACQ/SEARCH, ACQ/PEAKD and
ACQ/PEAKXD mode shall be tested
– Status = MET
DESCRIPTION OF RESULTS
–
–
–
•
COS34: Revealed segment B-to-A pixel scaling error that caused initial PEAKXD test to fail
COS26: : Initial update to extraction boxes, plate-scales, segment scaling parameters, and
spectrum locations for dispersed light TA.
COS28: All modes tested and verified; additional refinement of all patchable TA parameters.
• Exceptions: Some TA parameters may be tweaked upon further evaluation of 11486,
GO, GTO, and other SMOV datasets. The goal of these tweaks would be to provide an
as consistent as possible centering in the cross-dispersion direction to facilitate flatfielding. Once the final FUV wavelength solutions are in calcos, additional verifications
of the centering in the along-dispersion direction are planned.
SUPPORTING DOCUMENTATION
–
Parameter updates implemented through commanding table updates; ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
141
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.1 (slide 1 of 2) The zero
point offsets in the dispersion relations for the FUV spectroscopic
modes for each central wavelength setting shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS27 (11485), COS29 (11487), COS30 (11488)
•
DESCRIPTION OF METHODS
– COS27: Establish the limits of the initial wavelength scales in order to
determine if adjustments are necessary.
– COS29: Obtain zero-point offsets for the wavelength scale (internal
wavecal lamp scale to external standard wavelength scale).
– COS30: Verification of the wavelength ranges after any adjustments
resulting from COS27 or COS29 (programs 11485 or 11487).
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
142
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.1 (slide 2 of 2) The zero point
offsets in the dispersion relations for the FUV spectroscopic modes for each
central wavelength setting shall be measured
– Status = MET
•
DESCRIPTION OF RESULTS
– COS27: Determined that G140L/1230/FP-POS = 4 sees lamp zero order light.
This FP-POS was disallowed for GOs.
– COS29: Offsets between WCA and PSA data determined for all cenwaves of
G130M and 3 out of the 5 cenwaves of G160M. Used high-resolution STIS
echelle spectra for comparison when possible
• Relative agreement between COS and STIS ~0.0100 Å; absolute STIS wavelength
accuracy ~0.5-1 pixel (0.0056 Å)
– COS30: Determined that OSM1 position adjustments performed in May 2008 led
to overlap (identical wavelength range) between 1309/FP-POS = 4 and 1300/FPPOS = 1. OSM1 positions for 1300 and 1291 increased by +1 motor step to
remove overlap. Obtained WCA lamp spectra at all grating/cenwave/FP-POS to
update lamp template reference file; reference file has been produced.
•
SUPPORTING DOCUMENTATION
– pipeline reference file deliveries; ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
143
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
L.10.4.2.3.12.1 The zero point offsets in the dispersion relations for the FUV
spectroscopic modes for each central wavelength setting shall be measured
SMOV-to-TV03
PSA-to-WCA
offset differential
(left: segment A;
right: segment B)
for G130M (top)
and G160M
(bottom) as
determined from
COS29 (11487)
radial velocity
standard star
observations.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
144
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT: (slide 1 of 2)
L.10.4.2.3.12.2 The spectral resolution of the FUV spectroscopic
modes shall be measured .
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS31 (11489)
•
DESCRIPTION OF METHODS
– Obtain observations of narrow-lined O9 star in SMC previously
observed by STIS echelle with narrow aperture at R~114,000; target
has both narrow and broad saturated ISM lines with sharp edges
– Obtain additional STIS observations for complete comparison with all
medium resolution COS gratings.
– Use all FP-POS for each FUV grating, evaluate LSF, and compare with
model LSF convolved with higher-resolution STIS echelle observations
of the same target.
– Also evaluate LSF, plate scale, and image location for representative
offset pointings from PSA aperture center.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
145
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
•
•
SMOV4 REQUIREMENT: (slide 2 of 2)
L.10.4.2.3.12.2 The spectral resolution of the FUV spectroscopic modes
shall be measured . --- Status = MET
DESCRIPTION OF RESULTS
– COS LSF measured on orbit with HST OTA deviates from profile measured on
the ground.
– Inclusion of mid frequency zonal “polishing” wave-front errors (MFWFE) from
OTA provides better fit to on-orbit data; best fit on-orbit FUV line spread function
profile is non-Gaussian
– LSF power is distributed from core to wings due to MFWFEs
– Effective FUV spectral resolution not quite as good as expected
– Model LSFs have been generated that match on-orbit data and have been
released to the community
– Analysis of offset positions has not been completed.
•
SUPPORTING DOCUMENTATION
– Spectral resolution (LSF): ISR 2009-01(v1) ; model LSF tables distributed to
community
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
146
L.10.4.2.3.12.2 The spectral resolution of the FUV spectroscopic modes shall be
measured . --- Status = MET
COS Spectral Resolution: COS G130M spectrum (thick solid line with pixel-to-pixel variation)
compared with the STIS E140H spectrum convolved with a gaussian of R=20,000 (dotted line) and
with the LSF model containing OTA MFWFE effects (thin solid line). The model containing OTA
SMOV4 CLOSURE REVIEW
147
MFWFE effects fits weak and strong features and
predicts cores of lines.
Nov. 18,correctly
2009
L.10.4.2.3.12.2
The spectral resolution of
the FUV spectroscopic
modes shall be measured
--- Status = MET
1150 Å (G130M)
Above: Spectral resolving power, R, defined
as wavelength divided by FWHM of profile;
dotted: R for 6.5 pixel FWHM (ground value),
solid: R for wavelength-dependent model LSF
FWHM
Left: Model LSF as function of wavelength
including OTA MFWE compared to 6.5 pix
FWHM Gaussian; relative to ground, LSF power
is REVIEW
distributed
from core to wings due to MFWFEs
SMOV4 CLOSURE
SMOV4
CLOSURE REVIEW
148
Nov. 18, 2009 Nov. 18, 2009
L.10.4.2.3.12.2
The spectral resolution
of the FUV
spectroscopic modes
shall be measured
--- Status = MET
NUV Model LSFs:
Upper Panel: NUV model
LSFs without MFWFEs
included (color curves)
compared with model LSFs
with MFWFEs included
(black curves). Detector blur
kernel is included in all
models. Spectral resolution
for λ>2500 Å is not affected
by MFWFE.
Lower Panel: Same plots as
upper panel displayed on a
logarithmic scale
SMOV4 CLOSURE
SMOV4
REVIEW
CLOSURE REVIEW
Nov. 18, 2009 Nov. 18, 2009
149
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT: (slide 1 of 2)
L.10.4.2.3.12.3 The spatial resolution of the FUV spectroscopic
modes shall be measured.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS32 (11490)
•
DESCRIPTION OF METHODS
– Measure the on-orbit spatial resolution by observing a point source with
a pure emission line spectrum at an incremental range of offsets from
the center of the aperture. Also, measure any interdependence
between the spectral and spatial resolution and quantify changes in
profile shape, width and flux of a point source as it is stepped beyond
the edge of the aperture.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
150
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
•
•
SMOV4 REQUIREMENT: (slide 2 of 2)
L.10.4.2.3.12.3 The spatial resolution of the FUV spectroscopic modes
shall be measured. --- Status = MET
DESCRIPTION OF RESULTS
– The spatial resolution on-orbit is similar to pre-launch predictions, with initial
estimates giving a value of 0.75’’/0.94’’ (SegA/SegB) in cross-dispersion for
G130M, and 0.38’’/0.75’’ (SegA/SegB) for G160M, and 0.2’’ for G140L. The
spatial resolution is lowest at the shortest wavelengths in the FUV. Unlike with
the NUV, there is negligible shifting of the spectrum along dispersion with
increasing POSTARG in cross-dispersion. Calculation of the FUV plate scale
partially completed; results so far give values consistent with prelaunch
predictions.
•
SUPPORTING DOCUMENTATION
– ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
151
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.4 (slide 1 of 2) The flatfield response of the FUV detector shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS33 (11491), COS36 (11494)
•
DESCRIPTION OF METHODS
– Observe white dwarf spectrophotometric standard stars at several Y
POS-TARG positions with each grating to produce a two-dimensional
count map of portions of the detector that are illuminated in routine
observation. Compare limiting S/N and efficacy of various FUV flatfielding alternatives: combined or grating-dependent two-dimensional
flat field, one-dimensional flat field, and standard FP-POS processing.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
152
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.4 (slide 2 of 2) The flat-field
response of the FUV detector shall be measured
– Status = MET
•
DESCRIPTION OF RESULTS
– The G140L and G160M 2-d flat components are of relatively low S/N, due to the
observing time allocated. The G130M flat component is of higher quality (S/N ~
25, SQRT(CTS) ~50).
– Analysis of SMOV data to create 2D flats with observations of external sources still
in progress
Pulse-height dependence observed
• Grating dependence observed
• Currently investigating detector walk effect in cross-dispersion direction (~ 3-5 pixels) as
cause of apparent pulse-height and grating dependence of 2-d flats
•
– One-dimensional FF prepared from iterative FP-POS analysis
• Successfully removes grid wires and improves “pixel-to-pixel” fixed-pattern variation on
individual exposure basis
– Iterative FP-POS technique also successful (see L.10.4.2.3.12.7)
•
SUPPORTING DOCUMENTATION
– ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
153
L.10.4.2.3.12.4 The flat-field response of the FUV detector shall be measured --Status = MET
Grid wire removal (single exposure) with 1-d FF template derived from FP-POS data:
For Poisson-limited S/N=54 per resel (G160M seg A, pixel range 2000-5000,1620-1660 A), raw
“pixel-to-pixel” fixed-pattern S/N~15 (blackSMOV4
spectrum);
direct application of 1-d FF template removes
CLOSURE REVIEW
154
Nov. 18, 2009 fixed pattern S/N to 27 (red spectrum).
grid wires, improves individual exposure pixel-to-pixel
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.5 The sensitivity of each FUV
grating for each central wavelength setting shall be measured
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– COS19 (11492, 11491, 11494)
•
DESCRIPTION OF METHODS
– Establish COS PSA sensitivity versus wavelength over the entire observable
spectrum for all FUV gratings and central wavelength settings by observing HST
spectrophotometric standard stars to determine the initial on-orbit COS FUV
spectroscopic sensitivity.
•
DESCRIPTION OF RESULTS
– Sensitivity curves have been produced for all PSA settings (see attached
Figures). Unique COS sensitivity in 920-1050 Å. region. BOA results are
presented separately (see req. L.10.4.2.3.13 )
•
SUPPORTING DOCUMENTATION
– Reference file for all FUV gratings and central wavelengths with PSA delivered
to CDBS; ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
155
L.10.4.2.3.12.5 The sensitivity of each FUV grating
for each central wavelength setting shall be measured
FUV sensitivity curves for the G140L (blue), G130M (red)
and G160M (black), where solid = FUVA and dashed =
FUVB.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
156
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.6 The stability of a single mode of the FUV channel
over several orbits shall be characterized to determine if there are signatures of structural or
thermal distortions in the data
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
DESCRIPTION OF METHODS
–
•
The goal of this program is to measure OTA-COS pointing jitter and OSM drift over time scales of seconds to
hours. FUV spectroscopy is tested with PSA after precise target acquisition. Five-orbits each consisting of a
single TIME-TAG exposure with TAGFLASH lamp flashes every 200 seconds are employed.
DESCRIPTION OF RESULTS
–
–
•
COS35 (11493)
CEI stability specs are achieved (e.g., systematic drift: <1 resel [6 pixels] per hour correctable to 0.25 resel [1.5
pixels] per hour and random drift: <0.25 resel (1.5 pixels) contribution to FWHM).
In the first orbit, the mean position along the dispersion direction of the Segment A and B WCA spectra,
measured with respect to the initial position, slowly oscillates with an amplitude ~0.4 pixels, ending the orbit ~
at initial position. For the next 2 orbits the spectra slowly drift toward +dispersion after which any additional
aggregate offset is too small to reveal. The mean positions for the second through 5th orbits being, +0.2, +0.35,
+0.35,+0.35 pixels respectively. The CALCOS measure of these shifts via the overlaid TAGFLASH exposures
agree within <0.3 pixels. There is an orbital-period oscillation, accurately measured only in the TAGFLASH
positions that has a bimodal amplitude of ~0.5 and 0.7 pixels.
SUPPORTING DOCUMENTATION
–
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
157
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
• L.10.4.2.3.12.6 The stability of a single mode of the FUV channel over several
orbits shall be characterized to determine if there are signatures of structural or
thermal distortions in the data
– Status = MET
– 5 CVZ orbit time-series
– WCA lamp flash every
200 sec; WCA spectrum
centroid in each bin
– ~0.5 pixel amplitude
orbital variation along
dispersion
– Cumulative drift of ~0.8
pixels along dispersion
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
158
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
•
SMOV4 REQUIREMENT: L.10.4.2.3.12.7
–
–
–
–
•
The acquisition of spectra having S/N>30 using normal data acquisition and reduction
techniques shall be demonstrated for each FUV mode.
Status = MET
Spectra having S/N>100 for a single FUV medium resolution mode shall be demonstrated.
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
COS33 (11491), COS36 (11494)
•
DESCRIPTION OF METHODS
•
DESCRIPTION OF RESULTS
–
–
–
–
•
Observe WD spectrophotometric standard with all three FUV gratings; obtain high count
exposures with all four FP-POS settings. Co-add data, assess Poisson S/N, use various
techniques to attempt to improve S/N by removing fixed pattern noise.
Objectives are met
A straight sum of G160M data from 1420-1460 Å. yields Poisson statistical S/N~120, but
produces an actual continuum S/N~40.
An iterative technique using all FP-POS exposures removes fixed pattern noise including grid
wires and yields continuum S/N~110.
SUPPORTING DOCUMENTATION
–
ISR in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
159
COS
L.10.4.2.3 Science Verification & Calibration
L.10.4.2.3.12 The spectroscopic performance of the FUV channel shall be calibrated
• SMOV4 REQUIREMENT: L.10.4.2.3.12.7
– The acquisition of spectra having S/N>30 using normal data acquisition and
reduction techniques shall be demonstrated for each FUV mode. -- Status = MET
– Spectra having S/N>100 for a single FUV medium resolution mode shall be
demonstrated. --- Status = MET
– Demonstrate ability to
achieve S/N > 30 per 6pixel resel: Sum of
G160M data (RED
spectrum) from 1420-1460
Å. yields Poisson statistical
S/N~120, but produces an
actual continuum S/N~40.
– Demonstrate capability to
achieve S/N >100 per 6pixel resel : Iterative
technique using all FP-POS
exposures removes fixed
pattern noise including grid
wires and yields continuum
S/N~110 (BLUE spectrum).
S/N~110
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
160
COS
•
L.10.4.2.3 Science Verification & Calibration
SMOV4 REQUIREMENT: L.10.4.2.3.13 The position and
throughput of the BOA, and spectral resolution of the data acquired
through this aperture (BOA) shall be measured.
– This is done by observing an astronomical target in imaging mode and acquiring
a spectrum in each NUV and FUV grating at a single central wavelength setting.
•
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
DESCRIPTION OF METHODS
•
DESCRIPTION OF RESULTS
•
SUPPORTING DOCUMENTATION
– COS11 (11471), COS13 (11473), COS19 (11479), COS34 (11492), COS14
(11474), COS16 (11476), COS31 (11489), COS32 (11490)
–
Observe HST spectrophotometric standard stars. Obtain PSA and BOA NUV MIRRORA
and MIRRORB images and acquire BOA spectrum with each NUV and FUV grating at one
central wavelength setting. Measure imaging throughput in MIRRORA as well as MIRRORB
configurations. Measure location of BOA relative to PSA. Obtain FUV spectral resolution by
comparison of emission line widths with resolved line widths measured in archival STIS
echelle data; NUV spectral resolution from absorption profiles.
– Imaging throughput results for BOA/MIRRORA, and BOA/MIRRORB
configurations were implemented in synphot as well as in calcos.
– Relative locations of PSA and BOA images and spectra were measured.
– BOA sensitivity functions obtained
– Spectral resolution measured for all gratings
– Synphot reference file delivery; calcos throughput parameter update; BOA flux
calibration reference file in preparation;
ISR in preparation
SMOV4 CLOSURE REVIEW
161
Nov. 18, 2009
L.10.4.2.3.13 The position and throughput of the BOA, and spectral resolution of
the data acquired through this aperture (BOA) shall be measured.
FUV BOA
Resolving Power
Grating
R
G130M
5900
G160M
4400
G140L
1100
FUV BOA Resolution:
Obtained from
comparison of emission
line widths from COS33
(11491) with resolved
measurements of
archival STIS echelle
data.
NUV BOA Resolution: The open symbols indicate SMOV measurements
(COS16, 11476) and the line indicates estimates made from the NUV-BOA
CLOSURE REVIEW
imaging data obtained in thermal-vac 2006. SMOV4Nov.
18, 2009
162
L.10.4.2.3.13 The position and throughput of the BOA, and spectral resolution of
the data acquired through this aperture (BOA) shall be measured.
BOA combined on-orbit transmission function relative to PSA for
COS spectroscopy (solid black curve). NUV obtained from
COS19 (11479) and FUV from COS34 (11492). On-orbit
transmission compared with pre-launch measurements for FUV
CLOSURE REVIEW
(red dashed curve) and SMOV4
NUVNov.
(red
solid curve).
18, 2009
163
Backup Slides
18 November 2009
SMOV4 RQMT
RELEVANT ACTIVITY
PROPOSAL ID
TITLE
RQMT STATUS
L.10.4.2.1.1
COS01
LSAFE01-04
Instrument States
MET
L.10.4.2.1.2
COS23,04,08,05,24,31,34
11356,11355,11468,11466,11482,11489,11492
Detector States
MET
11356,11467
Data Interface and Data Transmission Verification
MET
L.10.4.2.1.3
COS23,06
L.10.4.2.1.4
COS02
11353
On-board Memory Check
MET
L.10.4.2.1.5
COS03
11354
Science Data Buffer Check
MET
MET
L.10.4.2.1.6
COS04
11355 v01-04
Test of NUV Detector Initial Turn-on and Recovery after Ano
MET
L.10.4.2.1.7
COS23
11356
Test of FUV Detector Initial Turn-on and Recovery after Ano
L.10.4.2.1.8
COS14,29,31,16,19,09
11474,11487,11489,11486,11479,11469
Functionality and Operations of Detectors
MET
L.10.4.2.1.9
N/A
N/A
QE Enhancement Grid Tests
RQMT DELETED
L.10.4.2.1.10
COS08,09,22,23
11468,11469,RT,11356
Performance of Mechanisms
MET
L.10.4.2.1.11
COS06,10,07,23
11467,11496,11355v05,11356
Functionality of Lamps
MET
L.10.4.2.2.1
COS19,34,36
11479,11492,11494
Contamination Management
MET
L.10.4.2.2.2
COS22,04,23,07,06
RT,11355v01-04,11356,11355v05,11467
Upon release the COS instrument shall undergo a period o
MET
L.10.4.2.2.3
COS22
RT
Opening of FUV Detector Door
MET
MET
L.10.4.2.3.1
COS05,06,07,10
11466,11467,11355v05,[11470,11496]
Internal NUV calibrations shall be conducted and measurem
L.10.4.2.3.2
COS08,09
11468,11469
The relationship between the HST coordinate system and
MET
L.10.4.2.3.3
COS09,13,19
11469,11473,11479
The locations of the spectra for each NUV mode shall be m
MET
L.10.4.2.3.4
COS08,09
11468,11469
The NUV channel shall be focused.
MET
MET
L.10.4.2.3.5
see following
see following
The target acquisition algorithms for NUV operations shall b
MET
L.10.4.2.3.5.1
COS11,08,09
11471,11468,11469
NUV undispersed light target acquisition in ACQ/SEARCH a
MET
L.10.4.2.3.5.2
COS12,08,09
11472,11468,11469
NUV dispersed light target acquisition in ACQ/SEARCH, A
L.10.4.2.3.6
see following
see following
The imaging performance of the NUV channel shall be calib
MET
L.10.4.2.3.6.1
COS13
11473
The PSF in NUV imaging (TA1) mode shall be measured.
MET
L.10.4.2.3.6.2
COS13
11473
The plate scale of the NUV detector in imaging (TA1) mode
MET
MET
L.10.4.2.3.6.3
COS13
11473
The throughput of the NUV imaging (TA1) mode shall be te
MET
L.10.4.2.3.7
see following
see following
The spectroscopic performance of the NUV channel shall be
MET
L.10.4.2.3.7.1
COS10,14,15
11470,11474,11475
The zero point offsets in the dispersion relations for the NUV
MET
L.10.4.2.3.7.2
COS16,17,14
11476,11477,11474
The spectral resolution of the NUV spectroscopic modes sh
MET
L.10.4.2.3.7.3
COS16,17,14
11476,11477,11474
The spatial resolution of the NUV spectroscopic modes sha
MET
L.10.4.2.3.7.4
COS18
11478
The flat-field response of the NUV detector shall be measure
L.10.4.2.3.7.5
COS19
11479,11481
The sensitivity of each NUV grating for each central wavele
MET
MET
L.10.4.2.3.7.6
COS20
11480
The stability of a single mode of the NUV channel over seve
MET
L.10.4.2.3.7.7
COS21
11481
The acquisition of spectra having S/N>30 using normal data
MET
L.10.4.2.3.8
COS24,25,27,30
11482,11483,[11485, 11496],11488
Internal FUV calibrations shall be conducted and measurem
MET
L.10.4.2.3.9
COS26
11484
The locations of the spectra for each FUV mode shall be me
MET
L.10.4.2.3.10
COS26,31
11484,11489
The FUV channel shall be focused. This is done by conduct
MET
L.10.4.2.3.11
see following
see following
The target acquisition algorithms for FUV operations shall b
MET
L.10.4.2.3.11.1
COS28,26,34
11486,11484,11492
FUV dispersed light target acquisition in ACQ/SEARCH, AC
MET
L.10.4.2.3.12
see following
see following
The spectroscopic performance of the FUV channel shall be
MET
L.10.4.2.3.12.1
COS27,29,30
11485,11487,11488
The zero point offsets in the dispersion relations for the FUV
MET
L.10.4.2.3.12.2
COS31
11489
The spectral resolution of the FUV spectroscopic modes sh
MET
L.10.4.2.3.12.3
COS32
11490
The spatial resolution of the FUV spectroscopic modes sha
MET
L.10.4.2.3.12.4
COS33,36
11491,11494
The flat-field response of the FUV detector shall be measure
MET
L.10.4.2.3.12.5
COS19
11492, 11491, 11494
The sensitivity of each FUV grating for each central wavelen
L.10.4.2.3.12.6
COS35
11493
The stability of a single mode of the FUV channel over seve
MET
SMOV4 CLOSURE REVIEW
MET
L.10.4.2.3.12.7
COS33,36
11491,11494
The acquisition of spectra having S/N>30 using normal data
Nov. 18, 2009
[FUV, NUV] position and [FUV, NUV] throughput of the
MET
L.10.4.2.3.13 COS11,13,19,34,14,16,31,32 11471,11473,11479,11492,11474,11476,11489,11The
COS SMOV4 REQUIREMENTS MATRIX
165
SMOV4 CLOSURE REVIEW
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166
SMOV4 CLOSURE REVIEW
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167
COS vs STIS Sensitivity
 COS is superb in FUV
New COS & STIS
 Comparable to
on-orbit sensitivities STIS in NUV
 NUV sensitivity
in G225M &
G285M is as
expected at launch
from grating
degradation
 All within 20% of
ground values
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
168
Advanced Camera
for Surveys
Linda J. Smith
Preamble
• At SMOV Requirements Review on March 21
2007, it was assumed:
– All 3 ACS channels are functioning
• But it was noted:
– In some repair scenarios, all 3 channels may not be
available so some revision to the requirements would
be needed
• HRC was not recovered:
– It is assumed in this presentation that requirements or
sub-requirements for HRC are waived.
SMOV4 CLOSURE REVIEW
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170
ACS SMOV4 Requirements Matrix
SMOV4 CLOSURE REVIEW
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171
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
TECs are turned off and heaters turned on for 12 hours. Following return to operate mode,
biases and darks are measured.
DESCRIPTION OF RESULTS
–
•
ACS04 (11367) - CCD hot pixel annealing
DESCRIPTION OF METHODS
–
•
A hot pixel annealing procedure shall be executed just before CCD activation and every four
weeks thereafter, thus resuming the standard cadence in force before SM4
Status = MET
Biases and darks measured. Hot pixel count follows historic trend. Super-darks and superbias calibration files produced.
SUPPORTING DOCUMENTATION
–
See following figure showing hot pixel count
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
172
ACS: Engineering
Requirements L.10.4.3.1
12 hr anneal
6 hr anneal
Post-SM4
-77 C
-81 C
WFC1 - number of hot pixels vs. time
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
173
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.2
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Command the CCD set point to -81C for WFC and -80C for HRC.
Monitor temperature for 24 hours.
DESCRIPTION OF RESULTS
–
•
ACS05 (11368) - CCD Temperature set point determination
DESCRIPTION OF METHODS
–
•
The ability of the TEC to cool and stably control the CCD at their nominal operating
temperatures shall be tested and verified through the engineering telemetry data during the
course of normal operations. Failure to reach the expected temperature will trigger an
existing contingency program (CCD temperature set point determination) that was used
successfully in SM3B.
Status = MET
Temperature achieved and found stable for WFC. HRC not functioning.
SUPPORTING DOCUMENTATION
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
174
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.3 (WFC)
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
•
•
After reaching the appropriate operating temperature, a mini-functional test shall be executed
for all ACS detectors to characterize their performances in the new thermal and electrical
environment.
Status = MET
ACS06 (11369, 11396) - CCD Functional Test
DESCRIPTION OF METHODS
– Test baseline performance of CCD subsystems using bias, dark, flat field (lamp
usage), and internal CTE exposures with all gain and readout modes.
DESCRIPTION OF RESULTS
– All WFC modes working; confirmed results of optimization campaign
SUPPORTING DOCUMENTATION
–
SMOV Morning meeting notes 09/03/09
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
175
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.3 (SBC)
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
The SBC is brought up to full voltage in four stages with careful monitoring of all voltages and
currents throughout. Finally a “fold analysis” is performed to test the performance.
DESCRIPTION OF RESULTS
–
•
ACS07 (11370) - SBC turn-on and anomalous recovery test.
DESCRIPTION OF METHODS
–
•
After reaching the appropriate operating temperature, a mini-functional test shall be executed
for all ACS detectors to characterize their performances in the new thermal and electrical
environment.
Status = MET
All voltages and currents were in nominal range and the fold analysis results were consistent
with previous measurements.
SUPPORTING DOCUMENTATION
–
SMOV Morning Meeting Notes 05/29/09
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
176
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.3 (SBC)
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
The SBC dark current is measured over a period of about 6 hours to quantify the known
steady increase with time after turn-on. Five 1000 second darks are taken in each of four
contiguous orbits.
DESCRIPTION OF RESULTS
–
•
ACS10 (11373) - SBC dark current measurement
DESCRIPTION OF METHODS
–
•
After reaching the appropriate operating temperature, a mini-functional test shall be executed
for all ACS detectors to characterize their performances in the new thermal and electrical
environment.
Status = MET
The dark current showed temperature dependence which exactly matched previous
measurements. Because these measurements were taken at a slightly higher temperature
than the normal operating value they did not provide useful calibration files, but recent
observations have already supplied these.
SUPPORTING DOCUMENTATION
–
SMOV Morning Meeting Notes 05/30/09
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
177
ACS: Engineering
Requirements L.10.4.3.1
•
SMOV4 REQUIREMENT: L.10.4.3.1.4
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
The ACS/SBC throughput in the far-UV is monitored over 3 visits during and just after the BEA period via
observations of NGC 6681. Aperture photometry of ~50 bright UV sources is compared with photometric
catalogs obtained just prior to SM4 to derive relative changes in sensitivity. Throughput differences within 2sigma (<5%) of historical norms will confirm that UV contamination is negligible and that it is safe to exit BEA.
DESCRIPTION OF RESULTS
–
•
ACS09 (11372) - SBC UV Contamination Check
DESCRIPTION OF METHODS
–
•
The standard UV monitoring program shall resume as soon as possible using an appropriate
choice of BEA targets for which pre-SM4 observations are available.
Status = MET
Relative photometry showed a slight loss in UV sensitivity, where the average sensitivity loss decreased with
increasing wavelength. Losses of ~3% were measured in the bluest (F115LP) filter and decreased to ~0.6%
in the reddest (F165LP) filter relative to data taken immediately before SM4.
SUPPORTING DOCUMENTATION
–
–
See SMOV meeting notes (31 May; 6, 13 June 09) and following figure
ISR on SBC photometric stability in preparation (expected Dec 2009)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
178
ACS: Engineering
Requirements L.10.4.3.1.4
Sensitivity Loss
Following SM4
-------------------F115LP = 3.0%
F125LP = 1.5%
F140LP = 2.1%
F150LP = 0.7%
F165LP = 0.6%
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
179
ACS: Target Acquisition
Requirements L.10.4.3.2
•
SMOV4 REQUIREMENT: L.10.4.3.2.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
WFC coordinate frame is mapped to the FGS frame using images of the astrometric standard
cluster NGC 188 obtained in Program 11379.
SBC is assumed to move in lock-step with WFC (as previously seen).
DESCRIPTION OF RESULTS
–
–
•
ACS12 - ACS to FGS alignment (associated with ACS17/Prop 11379)
DESCRIPTION OF METHODS
–
•
Reference apertures of all ACS channels will be determined with respect to FGS reference frame to
within 1 arc sec in V2-V3 coords and ≤ 10 arc min in rotation using well-observed dense stellar field.
Status = MET
Initial WFC aperture location off-nominal by 0.67 arc sec (translation) and 0.06 arc min (rotation),
which immediately satisfied requirement.
SIAF update not needed, but performed anyway.
SUPPORTING DOCUMENTATION
–
STScI PR #63200, “Update to ACS SIAF”, http://www.ess.stsci.edu/prsystem/servlet/prbrowse/pr.63200
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
180
ACS: Target Acquisition
Requirements L.10.4.3.2
•
SMOV4 REQUIREMENT: L.10.4.3.2.2
•
The location of the coronagraphic spots shall be measured with one set of
observations.
•
•
Status = WAIVED
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– ACS15 (11377) - HRC coronagraphic spot location.
•
DESCRIPTION OF METHODS
•
The position of the 1.8 arcsecond HRC coronagraphic spot is located in the field of
view by measurements of earth flats.
•
DESCRIPTION OF RESULTS
– The HRC was not recovered so this activity was not carried out. No further HRC
coronagraphy can be performed.
•
SUPPORTING DOCUMENTATION
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
181
ACS: Optical Alignment
Requirements L.10.4.3.3
•
SMOV4 REQUIREMENT: L.10.4.3.3.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
–
•
Phase retrieval image analysis of point sources over the FOV (WFC)
Comparison of encircled energy curves with pre-SM4 observations (SBC)
DESCRIPTION OF RESULTS
–
–
•
ACS16 (Program 11378) - SBC PSF Measurement
ACS17 (Program 11379) - CCD Image Quality, PSF, ACS to FGS Alignment
DESCRIPTION OF METHODS
–
–
•
The camera mode image quality at the detectors over the full field shall be measured via broad and
narrow band imaging of a sparse stellar field.
Status = MET
WFC focus and encircled energy measurements showed < 1 deviation from pre-SM4 focus
monitor (see L.10.4.7.1)
Encircled energy curves pre- and post-SM4 showed no systematic focus change
SUPPORTING DOCUMENTATION
–
–
ISR-TEL: HST Focus during SMOV4, in preparation
See following figure for SBC
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
182
ACS: Optical Alignment
Requirements L.10.4.3.3
• no systematic focus changes pre and post-SM4
• focus changes seen are within the range of
orbital “breathing”
Comparison of encircled energy curves pre- and post-SM4 for SBC
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
183
ACS: Optical Alignment
Requirements L.10.4.3.3
•
SMOV4 REQUIREMENT: L.10.4.3.3.2
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
–
•
Phase retrieval analysis performed on well-exposed, isolated stars across the FOV to determine (1)
coma and focus wavefront errors, and (2) corrector offsets needed to optimize focus.
DESCRIPTION OF RESULTS
–
–
•
ACS13 (Program 11375) - ACS Coarse Corrector Alignment
ACS14 (Program 11376) - ACS Fine Corrector Alignment
DESCRIPTION OF METHODS
–
•
Coarse and fine adjustments to the focus and tilt positions of the IM1 and M1 correctors will be
performed as contingency exercises if initial image quality tests (L.10.4.3.3.1) show a 3 or more
decrease in encircled energy.
Status = WAIVED
Initial WFC focus and encircled energy measurements showed < 1 deviation from pre-SM4 focus
monitor.
Contingency proposals waived as unnecessary.
SUPPORTING DOCUMENTATION
–
ISR-TEL: HST Focus during SMOV4, in preparation
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
184
ACS: Optical Alignment
Requirements L.10.4.3.3
•
SMOV4 REQUIREMENT: L.10.4.3.3.3
– The ACS Point Spread Function in coronagraphic mode shall be measured.
– Status = WAIVED
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– ACS18 (Program 11380) - HRC Coronagraphic Acquisition
•
DESCRIPTION OF METHODS
– Confirm ability to acquire bright point source onto occulting spots and bar.
Obtain short and long exposures in 2 filters and use well-exposed PSF to
measure position of star behind occulters and assess characteristics of
coronagraphic PSFs.
•
DESCRIPTION OF RESULTS
– HRC was not recovered during SM4, so this requirement is waived.
•
SUPPORTING DOCUMENTATION
– None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
185
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.2 (SBC)
–
–
•
Detector sensitivities and instrument configurations: SBC observations of reference
stellar fields (NGC6681 & NGC604) shall be used to measure: a) the detector plate scale,
orientation, & geometric distortion; b) the relative location of each aperture with respect to
the FGS reference frame (see L.10.4.3.2.1); c) the relative and absolute sensitivity as a
function of wavelength; and d) the uniformity of the flat field at low frequency
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
ACS20 (11398) - UV Sensitivity, Geometric Distortion, and Flat Fields
DESCRIPTION OF METHODS
a)
b)
c)
d)
The stability of the SBC geometric distortion is measured using dithered observations of
blue stars in NGC 604. The analyses discussed in ISRs 2007-09 & 2008-02 are
independently verified using the same software for both the original analysis and the new
SMOV data.
See L.10.4.3.2.1
The sensitivity in the full set of SBC filters is computed from aperture photometry in single
pointings of NGC6681 and compared with photometric catalogs derived prior to SM4.
Ratios of internal lamp flats are used to verify the stability of the low frequency flat fields
after SM4.
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
186
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.2 (SBC, cont’d)
•
DESCRIPTION OF RESULTS
a)
b)
c)
d)
•
The SBC distortion is found to be consistent with pre-SMOV values to better than 0.5 pixels
See L.10.3.4.2.1
Relative photometry indicates a slight loss in UV sensitivity of ~3% for F115LP and
decreasing with wavelength to ~0.6% in F165LP.
Ratios of internal lamp flats indicate that the low frequency sensitivity is consistent with preSMOV values to better than 0.1%. A formal L-flat solution will be obtained from the dithered
observations of NGC604.
SUPPORTING DOCUMENTATION
–
–
See figure from requirement 10.4.3.1.4
ISR on SBC L-flats in preparation (expected Dec 2009)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
187
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.2 (WFC)
–
Detector sensitivities and instrument configurations: WFC observations of the reference stellar
–
Status = MET
•
field (47 Tuc) shall be used to measure: a) the detector plate scale, orientation, & geometric distortion; b)
the relative location of each aperture with respect to the FGS reference frame (see L.10.4.3.2.1); c) the
relative and absolute sensitivity as a function of wavelength; and d) the uniformity of the flat field at low
frequency
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
ACS11 (11397) - CCD Sensitivity, Geometric Distortion, and FF Stability
DESCRIPTION OF METHODS
a)
b)
c)
d)
The stability of the WFC distortion and low frequency flats is studied in detail for one filter (F606W) using
dithered observations of NGC104. The geometric distortion solutions, PSFs, and Fortran codes from
Anderson & King are used to measure the relative positions of stars in 2009 compared to 2002
(corrected for proper motions).
See L.10.4.3.2.1
The sensitivity of the WFC is obtained from aperture photometry in single exposures spanning the entire
WFC filter set and compared with pre-SM4 measurements.
Both aperture photometry and ratios of internal lamp flats are used to verify the stability of the low
frequency flat fields after SM4.
SMOV4 CLOSURE REVIEW
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188
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.2 (WFC, cont’d)
•
DESCRIPTION OF RESULTS
a)
b)
c)
d)
•
The non-linear component of the WFC distortion is stable to within 0.05 pixels. Timedependent variations in the linear terms are difficult to disentangle from CTE effects but
appear to be consistent with Anderson’s predictions (ISR 2007-08).
See L.10.3.4.2.1
The average sensitivity of the WFC is stable to a fraction of a percent over the ACS
lifetime.
The low frequency flats are stable to ~1%. A formal L-flat solution has not yet been
obtained from the stellar photometry, but ratios of internal lamp flats show little change in
the sensitivity as a function of detector position.
SUPPORTING DOCUMENTATION
–
–
See the following figures.
ISR on WFC photometric stability in preparation (expected Dec 2009)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
189
ACS: Calibration
Requirements L.10.4.3.4.2
Y-pixel position residuals
(2009-2002) as a function of
magnitude.
Brightest
The slope in the residuals and
discontinuity at the chip
boundary (y=2048) are due to
imperfect CTE which is most
significant for faint stars.
The rms deviation from the
median is ~0.05 pixels
(excluding CTE effects) as
illustrated in the top panel.
Faintest
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
190
ACS: Calibration
Requirements L.10.4.3.4.2
SM4
WFC Sensitivity versus Time
exptime
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
191
ACS: Calibration
Requirements L.10.4.3.4.2
2009 Internal Lamp Flat
2009/2006 Flat Ratio
Scale (0.90-1.10)
Scale (0.98-1.02)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
192
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.3 (WFC)
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
The stability of the WFC flats is verified using internal tungsten lamp observations with the
standard filter subset (F435W, F625W, F814W, & F850LP). After applying the new relative
gain values for each amp, the images are normalized by the median value. The SMOV
images are then ratioed with those obtained in August 2006 (after the WFC temperature
change) and histograms are created for each filter. A Gaussian fit to the histogram is used to
determine the peak and fwhm to determine the number of pixels deviating by more than 3sigma.
DESCRIPTION OF RESULTS
–
•
ACS11 (11374) - CCD Internal Flat Field Stability
DESCRIPTION OF METHODS
–
•
Variations in the ACS detectors’ sensitivity on a pixel-to-pixel scale shall be measured through
observations with the internal lamps
Status = MET
The F435W, F625W, F814W, & F850LP filter ratios indicate that the P-flats are extremely
stable, where only 1.6%, 0.9%, 0.5%, & 0.4% of pixels show ratios beyond the 3 sigma limits.
SUPPORTING DOCUMENTATION
–
See the following figure.
SMOV4 CLOSURE REVIEW
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193
ACS: Calibration
Requirements L.10.4.3.4
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
194
ACS: Calibration
Requirements L.10.4.3.4
•
SMOV4 REQUIREMENT: L.10.4.3.4.3 (SBC)
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Six internal flats are obtained with the SBC using the deuterium lamp, one in each UV filter.
As the SBC P-flat is known to be wavelength independent, the five broadband images are
averaged and compared to a sum of 37 F125LP internal flat field images obtained prior to
SM4.
DESCRIPTION OF RESULTS
–
•
ACS20 (11398) - UV Sensitivity, Geometric Distortion, and Flat Fields
DESCRIPTION OF METHODS
–
•
Variations in the ACS detectors’ sensitivity on a pixel-to-pixel scale shall be measured
through observations with the internal lamps
Status = MET
The comparison shows a stability in the L-flat of better than 0.1%, while the the P-flat shows
changes of 1-2%. The intensity of the lamp continues to degrade, as expected.
SUPPORTING DOCUMENTATION
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
195
Cross-SI Light
Leak Test
•
SMOV4 REQUIREMENT: L.10.4.16.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
COS37 (11515)
DESCRIPTION OF METHODS
–
•
SMOV4 Light-Leak test
Status = MET
a set of external exposures designed to determine whether a particular SI is susceptible to
light leaks resulting from photons escaping from the calibration system of another SI. For a
specific combination of SIs, the SI assumed to be the light source carries out a calibration
activity while, in parallel, the other SI performs an external exposure.
DESCRIPTION OF RESULTS
–
Test carried out on Aug. 7, 2009, 219/1615 – 1923
•
–
–
•
Data analyzed by ACS, WFC3, COS Teams
Initial positive detections in ACS and WFC3 all proved to be unrelated to a light leak from
another SI. For ACS, stray light leak streak in F814W seen regardless of whether COS or
WFC3 lamps are on or off.
Streak also seen in pre-SM4 images and is caused by scattering from CCD surface and
reflection from window and beveled edges of camera housing.
SUPPORTING DOCUMENTATION
–
See SMOV Meeting Notes, ACS Update of Sep. 3, 2009
•
–
“Review of ACS-R Performance During SMOV4”
Following figure
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196
Cross-SI Light
Leak Test
Comparison between WFC and WFC3 Glints
ACS/WFC F814W
SMOV Day 219
WFC3/UVIS Thermal Vac
ISR 2007-21
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197
STIS
Charles R. Proffitt
STIS SMOV4
REQUIREMENTS MATRIX
RELEVANT ACTIVITY
SMOV4 RQMT
PROPOSAL ID
TITLE
Status
N/A
N/A
N/A
11347
11348
11349
11383
11399
N/A
11382
11350, 11351
N/A
Instrument States
Detector States
Data Interface
Memory Dumps
CS Buffer RAM Test
Mechanism Functional
Calibration Lamps
CCD Annealing
Temperature Monintoring
CCD Mini-functional
MAMA Recovery Procedures
Wait 3 Weeks for Deuterium/Krypton Lamp Use
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
11384
11388, 11401
STIS-to-FGS Alignment
ACQ and ACQ/PEAK Tests
MET
MET
11386
11383
11385,11391, 11392
11388, 11393, 11394
11389, 11395
STIS Focus Check
Aperture Wheel Repeatability
MSM Optical Format Verification
Spectroscopic Image Quality
Pointing Stability Tests
MET
MET
MET
MET
MET
11404, 11390, 11402
11400
11401, 11403
Dark Rate Measurements
CTI Check
Throughput Check
MET
MET
MET
Engineering Activities
L.10.4.5.1.1
L.10.4.5.1.2
L.10.4.5.1.3
L.10.4.5.1.4
L.10.4.5.1.5
L.10.4.5.1.6
L.10.4.5.1.7
L.10.4.5.1.8
L.10.4.5.1.9
L.10.4.5.1.10
L.10.4.5.1.11
L.10.4.5.1.12
STIS01
STIS01
STIS01
STIS02
STIS03
STIS04
STIS08
STIS05
engineering telemetry
STIS06
STIS17/18
N/A
Acquisition Activities
L.10.4.5.2.1
L.10.4.5.2.2
STIS09
STIS13, 15
Alignment Activities
L.10.4.5.3.1
L.10.4.5.3.2
L.10.4.5.3.3
L.10.4.5.3.4
L.10.4.5.3.5
STIS11
STIS08
STIS10, 21, 22
STIS13, 23, 24
STIS16, 26
Calibration Activities
L.10.4.5.4.1
L10.4.5.4.2
L.10.4.5.4.3
STIS07, 19, 20
STIS14
STIS15, 25
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Instrument States
L.10.4.5.1.1
•
SMOV4 REQUIREMENT: L.10.4.5.1.1
– STIS entry into each of the four instrument states (Boot, Hold, Operate,
Observer) shall be demonstrated
•
•
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– No proposal number per se. Instead, SUs (Scheduling Units) OSAFE01 – 05
•
DESCRIPTION OF METHODS
– Transition STIS from Safe mode through Observe using standard stored
commanding SUs.
•
DESCRIPTION OF RESULTS
– Scheduling Units OSAFE01 – 05 started execution at 2009.147:12:00:02.
Engineering telemetry was received from all modes. The telemetry was
examined for correct relay states, voltages, temperatures, currents, and logical
values, positions, and memory monitor values. Relay configurations were also
validated with CCS software tool MON CALC. The formal monitoring was done
by the FOT (Flight Ops Team). All transitions were successful.
•
SUPPORTING DOCUMENTATION
– N/A
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Detector States
L.10.4.5.1.2
•
•
SMOV4 REQUIREMENT: L.10.4.5.1.2
–
STIS entry into each of the defined detector states shall be demonstrated.
–
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
–
–
•
DESCRIPTION OF METHODS
–
–
•
Objectives met during recovery and routine operation of detectors
MAMA recovery activities provided detailed engineering data for all modes, including MAMA
time-tag observations
DESCRIPTION OF RESULTS
–
•
FUV STIS17 (11350)
NUV STIS18 (11351)
CCD STIS06 (11382)
No problems were encountered with uses of defined detector states. Note that the CCD
protect mode, although mentioned in preliminary versions of this requirement, was removed
from the allowed detector states early in the life of STIS as it was determined that it was not
useful.
SUPPORTING DOCUMENTATION
–
See also requirement L.10.4.5.1.11
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Interfaces/Memory
L.10.4.5.1.3, L.10.4.5.1.4
•
SMOV4 REQUIREMENT: L.10.4.5.1.3 & L.10.4.5.1.4
– L.10.4.5.1.3 STIS command and engineering data interface via the RIU and
science data transmission via the Science Data Formatter (SDF) shall be verified
by monitoring of normal configuration and science activities.
– L.10.4.5.1.4 Onboard memory will be checked by performing dumps of
EEPROM, PROM, EDAC RAM and Buffer RAM. (Special Commanding)
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– STIS02 (11347)
•
DESCRIPTION OF METHODS
– With the CS in Operate, dumps of the EDAC RAM, EEPROM, and CS PROM
memory areas were performed. With the DIB (and CS) in Operate, the MIE RAM
and MIE PROM was copied to the CS buffer RAM, and then dumped to the SSR.
•
DESCRIPTION OF RESULTS
– Code 582 flight software team at GSFC compared the dumped memory with the
ground reference image. No problems were found.
•
SUPPORTING DOCUMENTATION
– N/A
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CS Buffer Ram
L.10.4.5.1.5
•
SMOV4 REQUIREMENT: L.10.4.5.1.5
– L.10.4.5.1.5 Conduct a test of the ability to write to and read from the CS Buffer
RAM. (Special Commanding)
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– STIS03 11348 - Science Data Buffer Check with Self-Test
•
DESCRIPTION OF METHODS
– Using the set buffer memory macro, the CS Buffer RAM memory was zeroed
prior to SAA passages. Post passage, the buffer memory was dumped to the
SSR. This check was executed several times, spanning the SAA.
– The CS self test macro was used to conduct a pattern test of CS Buffer RAM and
the memory fail counter was monitored.
– DESCRIPTION OF RESULTS
– Code 582 flight software team at GSFC examined the zeroed-memory dumps –
no bit flips were found.
– The formal monitoring of the memory fail counter was done by the FOT (Flight
Ops Team) – the test passed.
•
SUPPORTING DOCUMENTATION
– N/A
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Mechanism Functional
L.10.4.5.1.6
•
SMOV4 REQUIREMENT: L.10.4.5.1.6
– L.10.4.5.1.6 Verify the proper functioning of all STIS mechanisms needed for
routine operations (the three MSM cylinders, the aperture wheel, CIM, echelle
blocker, CCD shutter, aperture door, & mode isolation shutter) over the full
ranges of motion needed for normal operations. Contingency: verification of the
corrector alignment mechanisms will be done only as part of any alignment or
focus adjustments. Movement of the corrector mechanisms should otherwise be
avoided.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– 11349 - Mechanism Mini-Functional
•
DESCRIPTION OF METHODS
– The mechanisms except the corrector were moved through the full range of
previous on-orbit motion. This verified operability and redistributed lubricant.
– Five telemetry samples of each mechanism's position were collected.
•
DESCRIPTION OF RESULTS
– All mechanism moves were verified successful by STIS instrument FSW (no ESB
messages) and via telemetry by STScI Engineering.
– No corrector movement was needed or performed.
•
SUPPORTING DOCUMENTATION
– N/A
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Lamp Function
L.10.4.5.1.7
•
SMOV4 REQUIREMENT: L.10.4.5.1.7
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)‫‏‬
–
•
STIS08 (11383, supplemental data from 11391 & 11392)
DESCRIPTION OF METHODS
–
•
Check the functioning of the calibrations lamps used for routine science and SMOV
operations (LINE, Tungsten, HITM1, & HITM2). If one or more of these lamps either shows
significantly degraded behavior or fails to function, make those changes which are necessary
to support science operations; these may include changes to the ground system and/or
onboard tables to allow substitution of one of the operable lamps for the critical functions of a
failed one. Verification of the Krypton and Deuterium lamps may be deferred until after
SMOV.
Status = MET
Obtain lamp images and compare intensities and wavelengths with results from previous
programs
DESCRIPTION OF RESULTS (Intensity Ratios)‫‏‬
–
•
All lamps functioned nominally with intensities in the optical and near-UV comparable to
those seen in 2004
– In the FUV, the LINE lamp flux at < 1350 Å shows significant declines, continuing trends
seen in pre-2004 data. Flux still appears to be minimally adequate for current wavecals.
SUPPORTING DOCUMENTATION
–
N/A
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CCD Annealing
L.10.4.5.1.8
•
SMOV4 REQUIREMENT: L.10.4.5.1.8
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Turn off CCD TEC and allow detector to warm to ambient for 12 hours. A standard sequence
of darks, biases, and flats is taken before and after the anneal to monitor the effects of the
anneal.
DESCRIPTION OF RESULTS
–
•
STIS-05 (11399)
DESCRIPTION OF METHODS
–
•
Description: The CCD shall be annealed to ameliorate hot pixels that have accumulated.
Status = MET
Anneal was successful, but did not eliminate all hot pixels that accumulated during the period
STIS was inoperative. The number of hot pixels is somewhat more than would be expected
from an extrapolation of pre-failure side-2 data.
SUPPORTING DOCUMENTATION
–
See plots on following page and STIS ISR 2009-02
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206
CCD Annealing
L.10.4.5.1.8
The number of pixels with a dark current > 0.1 e/s
as a function of observation date for before (red)
and after (black) each STIS CCD anneal. For all
values after the switch to side-2, the images are
rescaled to a CCD housing temperature of 18 C
before analysis.
The number of post-anneal hot pixels only at
various cut levels. All side-2 images were scaled to
a housing temperature of 18 C.
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Detector Temperature
Monitoring L.10.4.5.1.9
•
SMOV4 REQUIREMENT: L.10.4.5.1.9
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
N/A
DESCRIPTION OF METHODS
–
•
During the course of routine operations throughout SMOV, the temperature variations of
each detector will be monitored and compared to previous side-2 values. The ability of the
CCD TEC to cool that detector to the required operating temperature range will be evaluated.
Status = MET
Collection and examination of routine telemetry
DESCRIPTION OF RESULTS
–
Post-SMOV CCD housing temperature ~ 3 C higher than 2003
•
–
•
Results in higher dark rate and brighter hot pixels, but operations still feasible
Average MAMA Tube temperatures ~ 1.1 to 1.3 C higher than in 2003
SUPPORTING DOCUMENTATION
–
See following charts, STIS ISR 2009-02, and also the report on dark current
requirement 10.4.5.4.1 later in this package
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208
STIS L.10.4.5.1.9 MAMA Tube Temperatures
•
•
•
•
Above figures show MAMA Tube temperatures over the history of STIS.
Average values for the period between ~ 25 August & 16 September each year are also shown.
FUV MAMA OM1TUBET ~ 1.1 C warmer than in fall 2003
NUV MAMA OM2TUBET ~ 1.3 C warmer than in fall 2003
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STIS L.10.4.5.1.9
CCD Housing Temp.
•
On side-2 we can’t directly measure
CCD detector temperature, instead
use CCD housing temperature
(OCCDHT) as surrogate
–
–
–
–
•
Very sensitive to instrument state,
spacecraft attitude, and aft-shroud
temperature
Reached 24.5 C in August
~ 16 C when MAMA LVPSs were off
~ 22.1 during September 2009
OCCDHTAV averages
(excluding anneals)
–
–
–
–
22.1 C, 2009.65 - 2009.80
19.6 C, 2003.65 - 2003.80
19.5 C, 2002.65 - 2002.80
17.5 C, 2001.65 - 2001.80
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CCD Functional
L.10.4.5.1.10
•
SMOV4 REQUIREMENT: L.10.4.5.1.10
– Perform a mini-functional test of the STIS CCD
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– STIS06 (program 11382)
•
DESCRIPTION OF METHODS
– Measure baseline performance of CCD subsystem: Bias levels, read
noise, gain values, and charge transfer efficiency (CTE).
•
DESCRIPTION OF RESULTS
– Results are consistent with predictions based on extrapolations of
trends seen before STIS failure in August 2004.
– The CTE measurement indicates a dependence on CCD temperature,
to be determined and/or addressed later (when more data are available)
•
SUPPORTING DOCUMENTATION
– See STIS ISR 2009-02
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MAMA HV Recovery
L.10.4.5.1.11
•
SMOV4 REQUIREMENT: L.10.4.5.1.11
–
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
–
•
Verify the proper functioning of the MAMA detectors by following procedures similar to those
defined for MAMA anomalous recovery (STIS ISR 98-03). A MAMA detector should not be
otherwise used prior to completing this functional test. The high voltage for the STIS MAMA
detectors will not be activated until at least four days after release. (Special Commanding)
Meeting this also meets STIS SMOV4 Requirement L.10.4.5.1.2 for the MAMA detectors–
STIS entry into each of the defined detector states shall be demonstrated.
Status = MET
STIS17 (11350) – FUV MAMA HV Recovery
STIS18 (11351) – NUV MAMA HV Recovery
DESCRIPTION OF METHODS
–
–
These activities described in 11350 and 11351 verified the proper functioning of the MAMAs
and addressed concerns over Cesium migration from the photocathodes into the pores of the
microchannel plates.
The recovery consisted of four separate and unique visits per detector that were completed
in order. They were:
1. a signal processing electronics check
2. 1st high voltage ramp-up to an intermediate MCP voltage of -1500V with limits modifications and
voltage plateaus
3. 2nd high voltage ramp-up to an intermediate MCP voltage of 300V below the nominal MCP voltage
with limits modifications and voltage plateaus followed by a fold distribution test
4. a final high voltage ramp-up to the full operating voltage, again with limits modifications and voltage
plateaus, followed by a fold distribution test
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STIS
L.10.4.5.1.11 (Cont)
•
DESCRIPTION OF METHODS (cont)
–
•
DESCRIPTION OF RESULTS
–
–
•
During the 1st high voltage ramp-up, a time-tag exposure was performed followed by a dark
exposure. During the 2nd and 3rd high voltage ramp-ups, time-tag exposures were taken
followed by darks, flat field ACCUMs, and fold analysis tests.
Each detector successfully past each test. The final fold distribution test for each detector
was within family with both detectors showing a slight shift in the folds towards higher fold
numbers. This is consistent with aging MAMA detectors. The diagnostic exposures showed
no unusual or unexpected features.
The NUV detector exhibited dark counts 4-5 X higher than predicted. This was attributed to
increased window glow that had not been previously modeled. This led to a modification of
the NUV monitored voltage ramp yellow an red counter limits increasing them from 15,000 to
25,000 counts/sec. No modification was required to the normal 770,000 counts/sec.
observing limit. The window glow is decreasing.
SUPPORTING DOCUMENTATION
–
Excel workbook containing the Fold Analysis results available upon request.
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Deuterium/Krypton Lamp
Restrictions L.10.4.5.1.12
•
SMOV4 REQUIREMENT: L.10.4.5.1.12
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Monitor schedule to ensure lamps are not used too soon. No SMOV activity made use of
these lamps.
DESCRIPTION OF RESULTS
–
•
N/A
DESCRIPTION OF METHODS
–
•
The STIS Deuterium and Krypton lamps will not be operated until 3 weeks after release, as
required by a Constraints and Restrictions Document.
Status = MET
First post-SM4 use of STIS Deuterium and Krypton lamps were on 17-Aug-2009, about 3
months after release.
SUPPORTING DOCUMENTATION
–
N/A
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STIS-to-FGS Alignment
L.10.4.5.2.1
•
•
•
SMOV4 REQUIREMENT: L.10.4.5.2.1
–
The location of a reference STIS camera aperture shall be determined with respect to the FGS reference
frames to an accuracy of 1 arc second in V2-V3 coordinates and 10 arc minutes in aperture rotation angle.
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– STIS09 (11384)
DESCRIPTION OF METHODS
– Used stellar target & guides stars with UCAC-2 astrometric coordinates
– STIS 50CCD images & lamp images of 0.2X0.2 aperture interleaved;
•
•
allows both detector and aperture plane alignment to be measured.
– Target dithered over FOV to allow detector rotation to be measured.
DESCRIPTION OF RESULTS
– Measured offsets in (V2, V3) from expected SIAF values
•
•
–
–
–
–
Detector reference point (+0.231”, -0.062”)
Lamp image of reference aperture (+0.299”, +0.042”)
Accuracies limited by target/GS uncertainties of ~ 0.05”
Rotation measured within 1.1 arc-min of expected SIAF value
Plate scale measured differs by < 0.1% from SIAF value
Alignment more than good enough for SMOV and GO science
•
Any SIAF updates will be deferred until later in Cycle 17
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ACQ & ACQ/Peak Tests
L.10.4.5.2.2
•
SMOV4 REQUIREMENT: L.10.4.5.2.2
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
ACQ and ACQ/PEAK exposures were performed as parts of routine calibration observations
DESCRIPTION OF RESULTS
–
•
STIS13 (11388), STIS15 (11401), among others
DESCRIPTION OF METHODS
–
•
The ability to acquire and properly center targets with standard ACQs and the ability to
center targets in small apertures with ACQ/PEAK exposures will be demonstrated for both
standard and E1 aperture positions.
Status = MET
12 ACQ exposures and 19 ACQ/Peak exposures were performed as part of STIS/SMOV
programs. ACQ Peaks included 2 exposures using the 52X0.1E1 aperture position, and one
at the 52X0.1D1 position. Subsequent spectroscopic exposures confirmed that required
centering accuracy was obtained.
SUPPORTING DOCUMENTATION
–
N/A
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STIS Focus Check
L.10.4.5.3.1
•
SMOV4 REQUIREMENT: L.10.4.5.3.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Performed dispersed light G230LB peakup of a hot standard star in the 0.1X0.09 aperture and compared
aperture throughput with historical trends. F28X50OII narrowband images were also taken to check relative
focus.
DESCRIPTION OF RESULTS
–
–
–
–
•
STIS11 (11386)
DESCRIPTION OF METHODS
–
•
An aperture throughput test using an external target shall be used to assess STIS focus. The slit plane
encircled energy vs. wavelength shall also be measured using this external target. Contingency: if
throughput is down by more than 3 sigma (7%), relative to the expected mean after correction for expected
secular sensitivity changes, additional tests and perhaps a STIS corrector alignment and/or focus
adjustment shall be done.
Status = MET
Peakup throughput measurements between 94% and 97% of expected values
Ratio of small to large aperture throughputs consistent with 1997 focus confirmation spectra
O II phase retrieval focus results also consistent with historical range
Conclude STIS focus has not changed.
SUPPORTING DOCUMENTATION
–
See following chart
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STIS L.10.4.5.3.1
Focus
•
Fraction of predicted count rate observed
with STIS G230LB & 0.1X0.09 aperture
inACQ/PEAK exposures (before ~ MJD
51500 ACQ/PEAK exposures clipped the
bias at too high a level causing
underestimates of the throughput).
•
The ratios of 0.1x0.09 to large
aperture net count rates as measured
with deep G230LB ACCUM spectra are
compared for data from 1997 (black)
and 2009 SMOV (color).
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STIS Aperture Wheel
L.10.4.5.3.2
•
SMOV4 REQUIREMENT: L.10.4.5.3.2
–
Positioning of the STIS slit wheel checked for a representative subset of STIS apertures, and
compared to the previous side-2 measurements. If operationally significant discrepancies are
found in the relative aperture positions, a full re-measurement of all aperture locations will be
done.
– Status = MET
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)‫‏‬
– STIS08 (11383)‫‏‬
•
DESCRIPTION OF METHODS
– Take 20 images with three narrow, long slits and in alternating sequence
– Measure shifts of spectral images between exposures
•
DESCRIPTION OF RESULTS
– After subtracting thermal trends, relative aperture positions are found to be within
typical random measurement errors of < 0.2 pixels
•
SUPPORTING DOCUMENTATION
– N/A
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Spectral Formats
L.10.4.5.3.3
•
SMOV4 REQUIREMENT: L.10.4.5.3.3
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)‫‏‬
–
•
–
Obtain spectral images with CCD, FUV MAMA and NUV MAMA, a narrow long slit, and in
low- and high-resolution and Echelle
Measure any shifts or rotation of spectral traces
DESCRIPTION OF RESULTS
–
–
–
•
STIS10,21,22 (11385, 11391, 11392)‫‏‬
DESCRIPTION OF METHODS
–
•
For each optical element in the MSM, (except for MAMA imaging modes), the location of a
lamp spectrum or slit image on the detector … shall be compared to previous side-2 values.
Operationally significant shifts shall be corrected by updating on-board mechanism
calibration tables. … MAMA imaging mode alignments may be deferred until after SMOV.
Status = MET
Shifts consistent with expected 1 - 2 pixel variations due to MSM non-repeatability and
thermal flexures.
All positions checked are range needed to support normal operations and calibrations.
All rotations < 0.3 pixels across detector width
SUPPORTING DOCUMENTATION
–
N/A
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Spectroscopic Image
Quality L.10.4.5.3.4
•
SMOV4 REQUIREMENT: L.10.4.5.3.4
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
With each detector a star was positioned at 3 different slit positions and dithered both along
and perpendicular to the aperture. Relative throughputs and cross dispersion profiles were
measured and compared to previous observations.
Note that CCD part of test was done before final July HST secondary move, but comparison
of focus test (11386) showed no significant change in image quality
DESCRIPTION OF RESULTS
–
•
STIS-13 (11388 CCD), STIS-24 (11394 NUV), STIS-23 (11393 FUV)
DESCRIPTION OF METHODS
–
•
The spectroscopic image quality and cross dispersion PSF at each detector will be measured
as a function of position and wavelength using an external point source target. This test is
dependent on the settings of the HST secondary mirror positions and of the STIS corrector
mechanism, which must have been first set to their nominal values.
Status = MET
All scans across aperture well centered, cross dispersion profiles show no change in image
quality except for charge transfer inefficiency (CTI)
SUPPORTING DOCUMENTATION
–
See following charts
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221
STIS Calibration
L.10.4.5.3.4 (CCD)
•Centering along slit good for all 8 positions
•Cross dispersion profiles compared for 2009 & 2002
•CTI has increased (expected)
•
(
(pixels; 0.0506”/pixel)
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STIS
L.10.4.5.3.4 (NUV MAMA), cont.
• Cross-dispersion profiles from July 2002 and
Aug 2009 identical (integrated from 1593 to
3093A for G140L)
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STIS
L.10.4.5.3.4 (FUV MAMA part)
• Cross-dispersion profiles from July 2002 and
Aug 2009 identical (integrated from 1350 to
1650A for G140L)
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STIS Image Stability
(CCD Part) L.10.4.5.3.5
•
SMOV4 REQUIREMENT: 10.4.5.3.5
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
–
Monitored a star field for two consecutive orbits after a large attitude change, interleaved with
lamp images. Measured drifts in stellar positions & rotations.
Also interleaved MAMA dark and lamp observations to measure MAMA detector stability.
DESCRIPTION OF RESULTS
–
–
•
STIS-16 (11389)
DESCRIPTION OF METHODS
–
•
To measure image drifts in the typical post-SM4 thermal environment, the pointing and PSF
stability of the OTA-STIS CCD combination when observing an external target shall be
monitored over a single orbit immediately following an attitude change that is expected to
produce a significant thermal change in STIS.
Status = MET
In all tests, image drifts were within previously encountered range.
Note that CCD tests were done while MAMA LVPSs powered off. This may have reduced
effectiveness of test.
SUPPORTING DOCUMENTATION
–
See following charts
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STIS
L.10.4.5.3.5 (CCD part), cont.
• Variations during these two orbits small. . .
•
– MAMA LVPSs were off during this test
Majority of motion within STIS
– (Large symbols: cal lamp; small symbols stars)
Shifts in X (disp)
Shift in Y (Cross-disp)
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STIS
L.10.4.5.3.5 (MAMA part), cont.
MAMA Thermal Stability
Image drifts of lamp
spectra on each
detector over time.
DX FUV
DX NUV
Left: FUV MAMA
Right: NUV MAMA
DY NUV
DY FUV
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Detector Darks
CCD Part of L.10.4.5.4.1
•
SMOV4 REQUIREMENT: L.10.4.5.4.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Measure dark and read noise and produce bias and dark reference files, all using preexisting scripts
DESCRIPTION OF RESULTS
–
–
–
•
STIS07 (program 11404)
DESCRIPTION OF METHODS
–
•
The dark rate for each detector shall be measured at normal operating temperatures. For the
CCD, bias and read-noise measurements will also be made. Sufficient CCD dark and bias
measurements will be done to allow proper calibration of other STIS SMOV and ERO data…
Status = MET
Results are marginally consistent with predictions based on extrapolations of trends seen
before STIS failure in August 2004. Proper weekly superbias and superdark reference files
were created, tested, and delivered to CDBS.
Bias levels systematically 0.2 - 0.3 e higher than in 2004
Full sets of super-bias and super-dark reference files delivered for pipeline use
SUPPORTING DOCUMENTATION
–
See STIS ISR 2009-02, and following chart
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L.10.4.5.4.1 CCD Darks
• CCD dark current varies
across detector
– ~ 63% lower dark current
close to readout
• Increases ~ 7% /degree
of housing temperature
• Increasing with time
– Too soon to establish slope
of new trend over time
•
Dark current at center and near the
readout for STIS CCD with side-2
electronics. All results are scaled to a
CCD housing temperature of 22 C.
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Detector Darks: MAMA
part of L.10.4.5.4.1
•
SMOV4 REQUIREMENT: L.10.4.5.4.1
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Take dark exposures and monitor global rate counters in telemetry
For FUV take grouped exposures over a single SAA free period
DESCRIPTION OF RESULTS
–
–
•
STIS07 (program 11404)
DESCRIPTION OF METHODS
–
–
•
Description:
• The dark rate for each detector shall be measured at normal operating temperatures ...
Sufficient NUV MAMA dark measurements will be taken to ensure that the
phosphorescent window glow has declined to a level that will allow routine
observations. The FUV MAMA dark rate will be monitored over at least one 5 orbit
interval ...
Status = MET
FUV behavior and dark current values in 2009 similar to 2004 behavior
NUV dark current about 10X larger than expected, but the excess dark rate seems to be
declining with ~ 100 day e-folding time.
SUPPORTING DOCUMENTATION
– See following charts
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NUV MAMA Dark rate
•
Orange curve shows prediction of pre-SM4 dark current model
– Short term fluctuations are due to daily temperature cycling
•
•
•
Symbols show STIS NUV MAMA dark current measurements
Pre-SM4 prediction + Ae(E/kT)e(t/), with  =100 days (red) and  =  (blue)
If current trend holds, will return to expected range by start of Cycle 18
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FUV MAMA Dark Rate
•
FUV MAMA dark current is lowest immediately after HV turn-on and
increases as a function of turn-on time. Initial dark rate after SM4, was lower
than during 2004, but this has increased to a comparable level.
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STIS CCD Charge Transfer
Efficiency L.10.4.5.4.2
•
SMOV4 REQUIREMENT: L.10.4.5.4.2
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Measure Charge Transfer Inefficiency of CCD using the previously documented “Internal
Sparse Field” method, albeit using fewer intensity levels than the usual annual calibration
monitoring visits.
DESCRIPTION OF RESULTS
–
–
•
STIS14 (program 11400; observations redone as part of program 11850)
DESCRIPTION OF METHODS
–
•
Description: A test to check predictions for CTI losses on the STIS CCD detector shall be
done. Results will be evaluated for any impact on planned GO observations.
Status = MET
Analysis of program 11400 was impossible due to the faulty amp B. Observations redone
with amps A & C by early execution of visits 1-32 and 65-74 of (revamped) Cycle 17
calibration program 11850.
Results are consistent with predictions based on extrapolations of trends seen before STIS
failure in August 2004. The only change made during SMOV was a slight change of the time
constant of the CTI (from 0.218 to 0.216 %/yr). This was incorporated in a CCDTAB
reference file update.
SUPPORTING DOCUMENTATION
–
See STIS ISR 2009-02
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STIS Spectroscopic
Throughputs L.10.4.5.4.3
•
SMOV4 REQUIREMENT: L.10.4.5.4.3
–
–
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
STIS-15 (11401), STIS-25 (11403)
DESCRIPTION OF METHODS
–
•
For one wavelength setting of each STIS grating the throughput will be checked using an
external calibration target.
Status = MET
(11401) exposures in G230LB, G430L, G750L using 52x2 slit at nominal and E1 position; exposures in
G230MB, G430M, G750M at nominal and E1 slit, 2 grating settings per mode (11403) exposures in G140L,
G230L using 52x2 slit at nominal target position; exposures in G140M, G230M using 52x2 slit at 1173,
1567, 2818 Å central wavelengths; E140M (1425 Å), E140H (1416 Å), E230M (1978, 2707 Å), E230H (2263
Å) with 0.2x0.2 slit
DESCRIPTION OF RESULTS
–
–
Sensitivities measured; see following plots
Most gratings fit extrapolations of previous trends.
•
•
Exception: E140H throughput appears to be 10-20% low, cause not yet understood
SUPPORTING DOCUMENTATION
–
See following charts
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1st-order modes
•
Throughput relative to 1997 for sensitivity monitor observations from
2004 (dotted lines) and 2009 (solid lines) are shown for all STIS low
resolution gratings (left) and selected 1st order medium resolution
gratings (right).
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Echelle modes
•
Sensitivity monitor
observations show 3 out
of 4 echelle gratings
show differences smaller
than typical throughput
variations of 0.2X0.2
aperture
• E140H is systematically
low by 10-20%. Cause
still being investigated.
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STIS SMOV4
REQUIREMENTS MATRIX
RELEVANT ACTIVITY
SMOV4 RQMT
PROPOSAL ID
TITLE
Status
N/A
N/A
N/A
11347
11348
11349
11383
11399
N/A
11382
11350, 11351
N/A
Instrument States
Detector States
Data Interface
Memory Dumps
CS Buffer RAM Test
Mechanism Functional
Calibration Lamps
CCD Annealing
Temperature Monintoring
CCD Mini-functional
MAMA Recovery Procedures
Wait 3 Weeks for Deuterium/Krypton Lamp Use
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
MET
11384
11388, 11401
STIS-to-FGS Alignment
ACQ and ACQ/PEAK Tests
MET
MET
11386
11383
11385,11391, 11392
11388, 11393, 11394
11389, 11395
STIS Focus Check
Aperture Wheel Repeatability
MSM Optical Format Verification
Spectroscopic Image Quality
Pointing Stability Tests
MET
MET
MET
MET
MET
11404, 11390, 11402
11400
11401, 11403
Dark Rate Measurements
CTI Check
Throughput Check
MET
MET
MET
Engineering Activities
L.10.4.5.1.1
L.10.4.5.1.2
L.10.4.5.1.3
L.10.4.5.1.4
L.10.4.5.1.5
L.10.4.5.1.6
L.10.4.5.1.7
L.10.4.5.1.8
L.10.4.5.1.9
L.10.4.5.1.10
L.10.4.5.1.11
L.10.4.5.1.12
STIS01
STIS01
STIS01
STIS02
STIS03
STIS04
STIS08
STIS05
engineering telemetry
STIS06
STIS17/18
N/A
Acquisition Activities
L.10.4.5.2.1
L.10.4.5.2.2
STIS09
STIS13, 15
Alignment Activities
L.10.4.5.3.1
L.10.4.5.3.2
L.10.4.5.3.3
L.10.4.5.3.4
L.10.4.5.3.5
STIS11
STIS08
STIS10, 21, 22
STIS13, 23, 24
STIS16, 26
Calibration Activities
L.10.4.5.4.1
L10.4.5.4.2
L.10.4.5.4.3
STIS07, 19, 20
STIS14
STIS15, 25
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OTA & FGS Requirements
E. Nelan
M. Lallo
OTA & FGS Requirements
OTA L.10.4.7.1
•
SMOV4 REQUIREMENT: L.10.4.7.1 cross-SI / Observatory Focus (WAIVED)
– After HST release, its focus state shall be well-determined with sufficient ACS/SBC monitoring (from SMOV RR, Mar‘07)
– After HST release, its focus state shall be determined with sufficient ACS/HRC monitoring (from SMR-4029, Sep ‘08)
– Status = Met despite waiver*
*in pre-SM4 investigation, sbc uv images proved an insufficient indicator of focus, but ACS/WFC and STIS data provided focus determination
•
SMOV4 ACTIVITY / Proposal
– ACS17 (11397 & 11510), STIS11 (11386)
•
METHOD
– Phase retrieval image analysis of point sources, linear regression, curve-fitting, and application of best temperature
model corrections were used to estimate SMOV focus state.
•
RESULTS
– All analysis methods of data since 2003 (up to and including SMOV) agreed to within 1 micron, on an OTA focus
estimate of -2.5 microns (for August 1).
– COS & WFC3 foci were offset during their fine alignment by the equivalent of this -2.5 microns to optimize confocality for
all the SIs.
– A Secondary Mirror move of +3.0 microns was executed July 20th to leave the SI focii ~+0.5 microns
– ACS focus data obtained since the Secondary Mirror confirm positive focus, giving a mean of +1.3 microns
– Preliminary WFC3 phase retrieval results suggest confocality with ACS to within 1 micron.
•
SUPPORTING DOCUMENTATION
– ISR-TEL: HST Focus during SMOV4, in preparation
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OTA L.10.4.7.2
•
SMOV4 REQUIREMENT: L.10.4.7.2 cross-SI Positional Alignment
– Confirm that ACS, NIC, STIS post-SM4 V2V3 positions are within 2” and orientations within 0.2 deg of pre-SM4 values.
– Status = Met*
*NICMOS calibrations not yet completed. However, for ACS & STIS, this requirement was met when those SIs met
their own more stringent alignment requirements.
•
SMOV4 ACTIVITY / Proposal
– STIS09 (11384), ACS12/17 (11379)
•
METHOD
– Observations in large astrometric fields provide accurate (<0.1”) relative positions of target and guidestars. Fit of
guidestars RA,Dec and V2V3 give pointing solution used to calculated V2V3 of observed target(s) in SI, allowing the
determination of position and orientation in V-frame.
•
RESULTS
– STIS position found 0.25” and 0.016 deg from operational values, meeting requirements. No SIAF updated performed.
– ACS position found 0.67” from operational values (neglible angle change), meeting requirements. SIAF update
performed.
•
SUPPORTING DOCUMENTATION
– STScI PR-63200 “Update to ACS SIAF”, http://www.ess.stsci.edu/prsystem/servlet/prbrowse/pr.63200
– See Supporting Documentation section for STIS L.10.4.5.2.1
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OTA/FGS L.10.4.7.3.1
•
SMOV4 REQUIREMENT: L.10.4.7.3.1 Guide Star Acquisition Verification
– Verify capability of FGS1 and FGS3 to acquire guide stars in Fine Lock after SM4.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-03 (11457)
•
METHOD
– Acquire guide star pairs in FGS1R & FGS3, alternating which FGS is primary, secondary.
– Two sets of guide star pairs are used.
•
RESULTS
– All guide star acquisitions were successful. This also verifies that the FGS-FHST alignment remains within
tolerance.
•
SUPPORTING DOCUMENTATION
– OTA System Report for May 23, 2009 (Art Bradley), SMOV4 daily meeting
– Note: Art reported 6 successful guide star acquisitions in that 24 hour period (and no failures). The additional four
were from other proposals.
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OTA/FGS L.10.4.7.3.2
•
SMOV4 REQUIREMENT: L.10.4.7.3.2 Optimize FGS2R2 S-curves
– Adjust the FGS2R2 AMA to optimize the interferometric performance of the FGS across the instrument’s FOV.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-04 (11458)
•
METHOD
– Acquire S-curves of three bright stars (V<10) at five widely separated locations in the FGS2R2 FOV with F583W.
– The morphology and amplitude of the S-curves are used to inform the adjustment of the AMA.
– After three iterations to optimize the S-curves, a 15 “point-of-light” finale is performed on one of the three stars.
– These observations included F583W and PUPIL exposures (PUPIL is used for guiding).
•
RESULTS
– FGS2R2 S-curves were optimized across the instrument FOV.
– The observed PUPIL S-curves, Goodrich provided the optimal values for K-factors for guide star acquisition.
•
SUPPORTING DOCUMENTATION
– 15 POL after 3rd AMA move.ppt (Marilynn Chisholm, Linda A-Reed), SMOV4 daily meeting, June 11, 2009
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2/3 aperture X-axis S-Curves, 9.56 MV,
15 POL
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2/3 aperture Y-axis S-Curves, 9.56 MV,
15 POL
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OTA/FGS L.10.4.7.3.3
•
SMOV4 REQUIREMENT: L.10.4.7.3.3 FGS-FGS Alignment
– Determine the relative alignment of FGS2R2 w.r.t. FGS1R and FGS3 to an accuracy of ~100 mas.
– Status = Met*
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-05 (11458) ---- This is the AMA adjustment proposal
–
(11459)* --- This the SMOV4 FGS2R2 alignment proposal, it was withdrawn.
•
METHOD
– With the telescope pointing held at a fixed attitude for six orbits, FGS2R2 is used to observe seven stars
distributed across its FOV in Position mode using the PUPIL element.
– For each of these orbits, different guide star pairs will be used by FGS1r and FGS3.
– The astrometry stars and guide stars have ICRS positions from the UCAC-3 accurate to about 25 milliarcseconds.
– The HST observations and cataloged positions of these stars allows for a determination of FGS2R2 alignment
relative to FGS1R and FGS3.
•
RESULTS
– FGS2R2 alignment relative to FGS1R and FGS3 was determined to approximately 100 mas.
•
SUPPORTING DOCUMENTATION
– FGS-2R2 SMOV-4 Calibrations (Ed Kimmer) June 29, 2009
– http://www.sesd/stsci.edu/prd/sciopsdb/smov4/fgs2r_align
* The requirement was relaxed to 1”, with the final alignment deferred into the Cycle 17 FGS Calibration program
(when we could access M35 in late August). However, the 0.1” accuracy was achieved.
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astrometry
targets
G1
G2
G6
G4
G3
G5
guide star pairs,
by visit ID
SMOV4
FGS2r2-FGS alignment
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OTA/FGS L.10.4.7.3.4
•
SMOV4 REQUIREMENT: L.10.4.7.3.4 FGS2 Distortion and Plate Scale Calibration
– Determine the FGS2R2 plate scale and geometric distortion..
– Status = waived, requirement deferred to Cycle 17 FGS Calibration Program
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-06 (11458) ---- This is the AMA adjustment proposal
– OTA/FGS-06 (11460)* --- This the SMOV4 FGS2R2 Distortion and Plate Scale proposal, it was withdrawn.
•
METHOD
– The FGS2R2 is used to observe approximately 20 stars in an astrometric star field at five slightly different
pointings. At each pointing the stars are sequentially observed in Pos mode using the PUPIL element.
– This was the original plan.
•
RESULTS
– This SMOV4 requirement was migrated to the Cycle 17 FGS Calibration program.
• allows time for the FGS2R2 to stabilize
• access to the very accurate M35 astrometric catalog.
– However, the plate scale was calibrated to support the FGS2R2-FGS alignment calibration.
– Effective distortion errors are ~100 mas after plate scale calibration.
•
SUPPORTING DOCUMENTATION
– FGS-2R2 SMOV-4 Calibrations (Ed Kimmer) June 29, 2009
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OTA/FGS L.10.4.7.3.5
•
SMOV4 REQUIREMENT: L.10.4.7.3.5 Verify FGS2 Guide Star Acquisition
– After updating the FGS2 database with FGS2-FGS alignment and K-factor assignments, verify that FGS2R2 can
successfully acquire guide stars.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-07 (11457)
•
METHOD
– The FGS2R2 is used to acquire guide stars.
– This test used FGS2R2 to acquire three different guide stars in four different visits.
– Over the course of these tests FGS2R2 was used as both the primary and secondary FGS.
•
RESULTS
– The guide star acquisitions were all successful.
– The “miss distances” were small*, indicating good FGS2R2-FGS alignment and FGS2R2 scale calibration
– The photometric measurements were within ~0.1 magnitude of expected.
•
SUPPORTING DOCUMENTATION
– “FGS-2R2 SMOV Guide Star Acquisition Tests”, Morgan Van Arsdall OTA SMOV4 report July 1, 2009
* “There was no search radius seen when FGS2R2 was used as the secondary guider.” OTA SMOV4 report July 1,
2009
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OTA/FGS L.10.4.7.3.6
•
SMOV4 REQUIREMENT: L.10.4.7.3.6 Characterize FGS1, FGS2, and FGS3 pre-SM4
– Obtain S-curves at three locations in each FGS to baseline their pre-SM4 interferometric properties and
– Obtain Position mode observations of astrometric stars in M35 to baseline the pre-SM4 scale and distortion in
each FGS.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-08 (11462, 11315*, 11842*)
•
METHOD
– Each FGS is used to obtain S-curve measurements at three widely separated locations in its FOV with both the
F583W and PUPIL elements to establish their pre-SM4 interferometric performance.
–
In addition, the selected stars from the astrometric field in M35 are observed by each FGS in Position mode to
establish a baseline to measure changes in the plate scale and geometric distortions against similar
observations after SM4.
•
RESULTS
– All data were successfully acquired in the winter of 2007 (when M35 was available in two gyro mode, and SM4
was anticipated to be in the spring or summer of 2008).
•
SUPPORTING DOCUMENTATION
– ISR-TEL FGS Changes Across SM4, in preparation.
* part of the Cycle 16 & Cycle 17 FGS1R Calibration Plans
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OTA/FGS L.10.4.7.3.7
•
SMOV4 REQUIREMENT: L.10.4.7.3.7 Re-commission FGS1 and FGS3
– Obtain S-curves at three locations in FGS1 and FGS3 to measure their post-SM4 interferometric properties and
– Obtain Position mode observations of astrometric stars in M35 to measure the post-SM4 scale and distortion in
FGS1 and FGS3.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-09 (11463 - withdrawn)
(11871*)
•
METHOD
– FGS1 and FGS3 are used to obtain S-curve measurements at three widely separated locations in its FOV with
both the F583W and PUPIL elements to establish their post-SM4 interferometric performance.
–
In addition, the selected stars from the astrometric field in M35 are observed by FGS1 and FGS3 in Position
mode to be compared to baseline measurements obtained before SM4 to assess changes in the plate scale and
geometric distortions.
•
RESULTS
– All data were successfully acquired in the August, 2009. No substantial changes seen across the SM4 boundary.
•
SUPPORTING DOCUMENTATION
– ISR-TEL FGS Changes Across SM4, in preparation.
* part of the Cycle 17 FGS1R Calibration Plan
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OTA/FGS L.10.4.7.3.8
•
SMOV4 REQUIREMENT: L.10.4.7.3.8 Monitor Near Term Stability of FGS2R2.
–
–
Two and four months after commissioning obtain:
• S-curves at three locations in FGS2R2 to monitor changes
• Observe astrometric stars in M35 are to monitor changes in FGS2R2 scale and distortion.
Status = waived, requirements to be satisfied by Cycle 17 FGS Calibration Plan
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-04, 06 (11463 - withdrawn)
(11874, 11875*)
•
METHOD
– S-curve measurements at three widely separated locations in the FGS2R2 FOV with both the F583W and PUPIL
elements are obtained every three months.
–
Selected stars from the astrometric field in M35 are observed in Position mode to monitor changes in the
FGS2R2 plate scale, geometric distortion, and FGS2-FGS alignments.
•
RESULTS
– initial set of data were successfully acquired in August, 2009. Small changes seen in F583W S-curves.
•
SUPPORTING DOCUMENTATION
* part of the Cycle 17 FGS1R Calibration Plan
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OTA/FGS L.10.4.7.3.9
•
SMOV4 REQUIREMENT: L.10.4.7.3.9 FGS2 PMT Calibration
– Obtain Position mode measurements of stars in M35 to photometrically calibrate the FGS2R2 photomultiplier
tubes .
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-10 (11875*)
•
METHOD
– The photometric response of the FGS2R2 PMTs are calibrated from the observed photon counts of Position
mode exposures on selected stars in M35.
–
These stars have accurate magnitude determinations (to ~0.05) based upon observations obtained from the
photometrically well calibrated FGS1r and FGS3.
–
Saves HST observing time, no need to allocate an orbit to observe a photometric standard star.
•
RESULTS
– All data were successfully acquired in the August, 2009.
– Photometric response of FGS2R2 is consistent with the measurements of field stars obtained in the early
SMOV4 commissioning (AMA, FGS2R2-FGS alignment)
•
SUPPORTING DOCUMENTATION
– ISR-TEL FGS2R2 Photometric Calibration, in preparation.
* part of the Cycle 17 FGS Calibration Plan
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OTA/FGS L.10.4.7.3.10
•
SMOV4 REQUIREMENT: L.10.4.7.3.10 FGS2 Obscuration Zone
– Determine the location of the “obscured zone” which is used to observe the Internal Test Source (ITS). This
“zone” can not be used for acquisition and tracking of guide stars.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-11
•
METHOD
– The location of the obscured zone will be determined from Position mode measurements of the ITS.
– This will locate the ITS, and it will be assumed that the obscuration zone will be all regions within 40” of the ITS
source.
•
RESULTS
– FGS2R2 ITS measurements were obtained in SM4 and routinely since on a monthly basis.
– The location of the obscuration zone was determined by GSFC and provided to STScI.
•
SUPPORTING DOCUMENTATION
– Delivered FGS2R2 SIAF updates (from Ed Kimmer), see:
– http://www.sesd.stsci/prd/sciopsdb/smov4/fgs2r_alig/plot_smov4/ocsfgs_62931_61897_dif.txt
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FGS2R2
Obscuration zone
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OTA/FGS L.10.4.7.3.11
•
SMOV4 REQUIREMENT: L.10.4.7.3.11 FGS2 Dark Count Rate
– Determine the dark count rate of each photomultiplier tube in FGS2R2.
– Status = Met
•
SMOV4 ACTIVITY / Proposal
– OTA/FGS-12
•
METHOD
– The dark count rate of the FGS2R2 PMTs are determined from the on orbit Aliveness and Functionality tests (in
shuttle bay)
– and from intervals of time when the FGS high voltage is on and the FGS 5”x5” instantaneous field of view is
exposed to empty sky.
•
RESULTS
– FGS2R2 dark count rates have been measured from the in-shuttle AT/FT, and from dark sky measurements as
the FGS2R2 slews from star to star in calibration measurements.
•
SUPPORTING DOCUMENTATION
– FGS 2 Dark + Background Count Rate Determination, Art Bradley, in preparation
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ERO
Early Release Observations requirement was met.
• Observations were obtained using WFC3, COS, ACS, and
STIS.
• Observations occurred from 29 June - 31 Aug. 2009.
• Images and spectra were released on 9 Sep. 2009
ERO
Data acquisition, analysis and image processing went according
to plan with a few exceptions:
• Guide star failures required repeats for 11 orbits of WFC3
observations of Stephans’ quintet.
• The Jupiter-comet collision impacted SMOV observations and
OPO image processing team. HST press release occurred on 24
July 2009.
• COS observations of quasar line of sight repeated (4 orbits)
after discovery of out-of-focus status.
• A portion of COS observations of supernova remnant were
repeated following a guide star failure (2 orbits).
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
258
WFC3
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
COS
259
ACS
STIS
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
260
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
261
NICMOS
T. Wiklind
NICMOS SMOV4 History
• NICMOS/NCS inactive September 2008 – August 2009
Planned safing of NICMOS and NCS in September 2008
Subsequent re-start attempts unsuccessful due to circulator and compressor
failures (water ice contamination)
In April 2009 it was decided to defer NCS re-start to later in SMOV4
NCS successfully re-started in August 2009 followed by rapid cool-down
Low mass-flow in circulator loop forced a higher set-point than planned
SMOV impact through extended dark current monitoring (dark current level and
stability)
NICMOS SMOV started in September 2009
All main NICMOS SMOV activities finished when the SIC&DH unit safed on
October 22 2009. Some monitoring activities remained.
NCS and NICMOS safed and warmed up
System is currently in a warm state
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263
NICMOS SMOV4
REQUIREMENTS MATRIX
SMOV4 RQMT RELEVANT ACTIVITY
L.10.4.4.1.1
NIC03
L.10.4.4.1.2
NIC04, NIC05
L10.4.4.1.3
NIC03
L.10.4.4.2.1
NIC07
L.10.4.4.2.2
NIC10
L.10.4.4.3.1
NIC08
L.10.4.4.3.2
NIC05
L.10.4.4.3.3
NIC11
L.10.4.4.4.1
NIC12
L.10.4.4.4.2
NIC09
L.10.4.4.4.3
NIC14
L.10.4.4.4.4
NIC13
L.10.4.4.5.1
NIC01
L.10.4.4.5.2
NIC01
L.10.4.4.5.3
NIC01
L.10.4.4.6.1
NIC01
PROPOSAL ID
11406
11407, 11408
11406
11410
11413
11411
11408
11414
11415
11412
11417
11416
Š
Š
Š
Š
TITLE
DC Transfer Test
Filter Wheel test, Focus and PAM Grid Tilt Test
DC Transfer Test
NICMOS Aperture Locations
NICMOS Mode-2 Coronagraphic Target Acquisition
NICMOS Optical Plate Scale
NICMOS Focus and PAM Grid Tilt Test
NICMOS Optimum Coronagraphic Focus Determination
NICMOS Coronagraphic Performance Assessment
NICMOS Geometric Stability
Detector Read Noise and Dark Current
Themal Characterization
Verify the NCS set-point at 72Š73K
Verify detector temperature at 77 ± 1 K
Characterize the NCS Cool-down
Verify and monitor detector temperature
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
RQMT STATUS
MET
MET
MET
PARTIALLY MET
Waived
Waived
MET
Waived
Waived
Waived
PARTIALLY MET
PARTIALLY MET
NOT MET
NOT MET
MET
NOT MET
COMMENTS
Detailed analysis pending
Deferred
Withdrawn
Deferred
Deferred
Withdrawn
Not finished
Not finished
Set-point 75-77K
Detector temp ~82K
No available temp sensor
264
NICMOS
L.10.4.4.1
•
Engineering requirements
SMOV4 REQUIREMENT: L.10.4.4.1.1
– The ability to command NICMOS via the RIU, science data transmission via the
SDF, and the ability of NICMOS to transition between primary operational states
(HOLD, BOOT, SAA-OPER, OPERATE and OBSERVE) shall be verified.
•
•
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC03 (11406) DC Transfer Test
DESCRIPTION OF METHODS
– Activation and verification of Functionality and Operability of Detectors and
Readout Electronics Chains.
•
DESCRIPTION OF RESULTS
– All test objectives met
•
SUPPORTING DOCUMENTATION
– Draft report from IDT
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
265
NICMOS
L.10.4.4.1
•
•
•
SMOV4 REQUIREMENT: L.10.4.4.1.2
Operation of the NICMOS mechanisms (PAM, FOM, and filter wheels) shall be
tested. PAM motion over the range needed to assure focus in all three NICMOS
cameras (best achievable focus for NIC3). The ability to reposition the field offset
mirror (FOM) over the range needed to remove vignetting in NIC3 shall be
demonstrated. Filter wheel motion shall be verified for each camera.
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC04, NIC05, NIC06 (11407, 11408) NICMOS Filter Wheel Test, Focus and Tilt
Test
DESCRIPTION OF METHODS
–
–
–
•
Filter Wheel Test: Digital/analog data for first filter wheel moves, flats for all filter positions
Focus/Tilt: Focus test and Coma (PAM tilt) for all 3 cameras
FOM functional inferred from focus/tilt images (proposal 11409 withdrawn)
DESCRIPTION OF RESULTS
–
–
–
–
•
Engineering Requirements
All test objectives met
Filter Wheel Test: All 3 filter wheels fully functional
Focus/Tilt: PAM corrected +0.5mm for NIC1 and NIC2 (SM move in July 2009)
FOM: Inspection of NIC3 images show no warm vignetting (FOM moved repeatedly)
SUPPORTING DOCUMENTATION
–
Planned ISR
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
266
NICMOS
L.10.4.4.1
•
•
Engineering Requirements
SMOV4 REQUIREMENT: L.10.4.4.1.3
Verify the basic operating characteristics of the flight detectors through a series of
multiple non-destructive readouts as a function of bias voltage.
– Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC03 (11406) DC Transfer Test
•
•
•
DESCRIPTION OF METHODS
– Evaluate long term stability of the Bias Voltage at the FPA and its impact on
detector gains. Series of non-destructive read-outs.
DESCRIPTION OF RESULTS
– All detector and image data flow operations nominal
– No A-to-D zero point offset adjustments needed
– Bias voltage declined by 21mV at all 3 FPAs since March 2002 (seen as
deviation of Temp_from_Bias and Mounting Cup temperature – calibration issue)
SUPPORTING DOCUMENTATION
–
Draft report from IDT
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
267
NICMOS
L.10.4.4.2
•
•
•
SMOV4 REQUIREMENT: L.10.4.4.2.1
The location of each NICMOS camera aperture shall be determined with respect to
the FGS reference frames to an accuracy of +/-2 arcseconds in V2-V3 coordinates
and 7 arcminutes in aperture rotation angle for Camera 2 and 1 degree for cameras 1
and 3.
– Status = PARTIALLY MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC07, 11410 NICMOS Aperture Locations
DESCRIPTION OF METHODS
–
–
–
•
Astrometric field (NGC188)
Three astrometric stars for each camera
9-point dither pattern
DESCRIPTION OF RESULTS
–
–
–
•
Target Acquisition Requirements
NIC1 and NIC2 shows a shift of 2.2 arcsec in +Y, NIC3 shows no shift
Expected shift in NIC1 and NIC2 due to PAM relocation: +1.8 arcsec
Detailed analysis underway: Tie to V2-V3 coordinate system
SUPPORTING DOCUMENTATION
–
Planned ISR
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
268
NICMOS
L.10.4.4.2
•
•
•
SMOV4 REQUIREMENT: L.10.4.4.2.2
The Mode-2 coronagraphic target acquisition shall be characterized and measured
with a precision of ~1/10 of a pixel. Acquisition of the target and the coronagraphic
hole shall be shown to be repeatable, within the precision given, using the onboard
flight software.
– Status = Waived
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC10, 11413 NICMOS Mode-2 Coronagraphic Target Acquisition
DESCRIPTION OF METHODS
–
–
•
Target acquisition with two different roll angles and slew maneuvers
Three different brightness and environment tested
DESCRIPTION OF RESULTS
–
•
Target Acquisition Requirements
Test deferred until demanded by allocated GO/DD program
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
269
NICMOS
L.10.4.4.3
•
Optical Requirements
SMOV4 REQUIREMENT: L.10.4.4.3.1
The optical plate scales at each of the detector focal planes shall be measured, with
a precision of better than 0.1% in each camera.
Status = Waived
•
•
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
– NIC08, 11411 NICMOS Optical Plate Scale
DESCRIPTION OF METHODS
–
–
•
DESCRIPTION OF RESULTS
–
•
Observation of standard astrometric field in a single filter for all 3 cameras
Five exposures with the same group of stars placed in each quadrant and center
Test withdrawn. Negligible corrections from SMOV2 to SMOV3b.
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
270
NICMOS
L.10.4.4.3
•
Optical Requirements
SMOV4 REQUIREMENT: L.10.4.4.3.2
PAM focus setting should be measured to establish the best focus focus for each
camera. The encircled energy within 100 mas (200 mas for camera 3) radius of an
unresolved point source shall be measured. In case the total wavefront error exceeds
/14 for NIC1 and NIC2 at 1.1 and 1.6 microns, respectively, a fine optical alignment
program will be implemented.
•
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
– NIC05, 11408 NICMOS Focus and PAM Grid Tilt Test
DESCRIPTION OF METHODS
–
•
DESCRIPTION OF RESULTS
–
•
See L10.4.4.1.2
PAM Focus for NIC1 and NIC2 changed by +0.5mm
SUPPORTING DOCUMENTATION
–
Planned ISR
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
271
NICMOS
L.10.4.4.3
•
Optical Requirements
SMOV4 REQUIREMENT: L.10.4.4.3.3
The best coronagraphic focus shall be determined. The purpose of this test is to
establish the PAM position to optimize the contrast in the coronagraphic image.
•
Status = Waived
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
– NIC11, 11414 NICMOS Optimum Coronagraphic Focus Determination
DESCRIPTION OF METHODS
–
•
•
Find the PAM position that maximizes the coronagraphic image/background ratio
DESCRIPTION OF RESULTS
– Test deferred until demanded by allocated GO/DD program
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
272
NICMOS
L.10.4.4.4
•
Calibration Requirements
SMOV4 REQUIREMENT: L.10.4.4.4.1
The performance of the NICMOS coronagraph shall be characterized. The goal is to
provide the best achievable target/background contrast ratio.
•
Status = Waived
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
– NIC12, 11415 NICMOS Coronagraphic Performance Assessment
DESCRIPTION OF METHODS
–
•
•
Quantitatively measure and map the diffractive and scattered energy rejection of occulted
targets
DESCRIPTION OF RESULTS
– Test deferred until demanded by allocated GO/DD program
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
273
NICMOS
L.10.4.4.4
•
Calibration Requirements
SMOV4 REQUIREMENT: L.10.4.4.4.2
NICMOS geometric stability will be characterized by measuring the lateral motion of
the image in the Camera 2 focal plane.
•
Status = Waived
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
•
– NIC09, 11412 NICMOS Geometric Stability
DESCRIPTION OF METHODS
–
•
•
Repeat of NICMOS Optical Plate Scale using NIC2. Time baseline ~2 months
DESCRIPTION OF RESULTS
– Test withdrawn. No initial Optical Plate Scale measurement. No GO program
demanding astrometric precision
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
274
NICMOS
L.10.4.4.4
•
Calibration Requirements
SMOV4 REQUIREMENT: L.10.4.4.4.3
Detector noise, read-noise and dark current shall be measured throughout the SMOV period
through a series of dark exposures.
•
Status = Partially MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
DESCRIPTION OF METHODS
–
•
Monitoring of detector characteristics. Daily for dark current, weekly for read noise
DESCRIPTION OF RESULTS
–
–
–
•
NIC14, 11417 (11947) NICMOS Detector Read Noise and Dark Current
Significant dark current measurements at three different neon set-points allowed
characterization of the dark current’s temperature dependence (75/76/77 K)
NIC3 showed a factor 5 increase in linear dark current at 77K, while NIC1 and NIC2
experienced a factor of 2 increase.
More stable dark current at a neon set-point of 76K
SUPPORTING DOCUMENTATION
–
Planned ISR
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
275
NICMOS
L.10.4.4.4
•
•
SMOV4 REQUIREMENT: L.10.4.4.4.4
HST+NICMOS thermal emission will be characterized in a subset of spectral
elements over the duration of SMOV.
Status = Partially MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Pure Parallel observations using NIC3 and the F222M filter
Characterize the background as a function of HST sun angle and other factors
DESCRIPTION OF RESULTS
–
•
NIC13, 11416 NICMOS Thermal Characterization
DESCRIPTION OF METHODS
–
–
•
Calibration Requirements
Program had just started when SIC&DH safed on October 22
SUPPORTING DOCUMENTATION
–
Planned ISR
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
276
NICMOS
L.10.4.4.5
•
•
SMOV4 REQUIREMENT: L.10.4.4.5.1
Configure the NCS to re-cool NICMOS detectors. The goal during SMOV is to verify
the capability to maintain the weighted average of the neon inlet and outlet
temperatures at a desired setpoint in the range 72-73 K.
Status = NOT MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Engineering activity following the start of cool-down
DESCRIPTION OF RESULTS
–
–
•
NIC01, None
DESCRIPTION OF METHODS
–
•
NCS Engineering Requirements
Unable to maintain dewar temperature with a neon set-point at 72–73K
The NCS was operated with a Neon set-point at 75, 76 and 77K while detector performance
was monitored through dark monitoring
SUPPORTING DOCUMENTATION
–
Planned ISR (dark measurements)
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
277
NICMOS
L.10.4.4.5
•
•
SMOV4 REQUIREMENT: L.10.4.4.5.2
Verify the capability of the NCS to achieve a NICMOS Cold Well temperature (as
measured by the 1-1 temperature sensor) of 77+/-1 degrees Kelvin (nominal 77.15K)
and maintain it within 0.1K.
Status = NOT MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Engineering activity following the start of cool-down
DESCRIPTION OF RESULTS
–
–
–
•
NIC01, None
DESCRIPTION OF METHODS
–
•
NCS Engineering Requirements
Unable to maintain dewar temperature at 77 ± 1 K
The higher set-points demanded by the reduced mass-flow in the circulator resulted in a
dewar temperature above the range of dewar temperature sensors (A/D conversion)
No direct measurements of the dewar or detector temperatures
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
278
NICMOS
L.10.4.4.5
•
•
SMOV4 REQUIREMENT: L.10.4.4.5.3
The NICMOS cooldown profile shall be characterized.
Status = MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
Engineering activity following the start of cool-down
DESCRIPTION OF RESULTS
–
–
–
•
NIC01, None
DESCRIPTION OF METHODS
–
•
NCS Engineering Requirements
Cool-down profile different from previous cool-downs
Rapid and effective cool-down
NICMOS is safe mode from the start of cool-down
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
279
NICMOS
L.10.4.4.6
NICMOS/NCS Calibration
and Performance Requirements
•
•
SMOV4 REQUIREMENT: L.10.4.4.6.1
The temperature of each NICMOS detector, along with its range of variation and the
timescale of variation, shall be determined. Detector temperature stability shall be
characterized over periods of 60 sec, 2000 sec, 24 hours and 30 days using available
temperature sensors and temperature from detector bias
Status = NOT MET
RELEVANT SMOV4 ACTIVITY (PROPOSAL NO.)
–
•
DESCRIPTION OF METHODS
–
•
Engineering activity following the start of cool-down
DESCRIPTION OF RESULTS
–
–
•
NIC01, None
Loss of mounting cup temperature sensors due to high Circulator neon set-point
Temperature from detector bias affected by variation in bias supply voltage
SUPPORTING DOCUMENTATION
–
None
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
280
NICMOS
SMOV4 CLOSURE REVIEW
Nov. 18, 2009
281