HST
MOSES
SMOV4 PROJECT REVIEW
12 OCTOBER 2007
1
SMOV4 REQUIREMENTS
REVIEW – 12Oct07
DRAFT AGENDA
ITEM
LEAD
HST
MOSES
TIME (min)
PAGE
=======
=====
=======
====================
Intro
Carl Biagetti, Rick Burley
10
2
PCS
Dan Smith
10
14
TCS
Joe Mandi
5
24
EPS
Stan Kroll
10
26
OTA/FGS
Ed Nelan
15
28
WFC3
John MacKenty
25
47
COS
Tony Keyes
25
68
ACS
Kailash Sahu
25
99
STIS
Charles Proffitt
25
110
NICMOS/NCS
Tommy Wiklind
20
128
ERO
Carl Biagetti (for Keith Noll)
5
144
Closing
Carl Biagetti, Rick Burley
5
152
=======
3h00m
2
HST
MOSES
SMOV PROJECT REVIEW
- INTRODUCTION Carl Biagetti
3
SMOV4 Planning Schedule
for Aug 2008 Launch
Start
======
Oct06
End
======
Mar07
21Mar07
Mar07
Jun08
Activity
========== ============================
Requirements Update
Oct07
SMOV Planning
- Activity Summaries
- Special Commanding Development
- Integrated plan
SMOV Project Review
Aug08
Aug08
SMOV Implementation Phase
- Proposal generation/iteration
- ERO program
- Operations planning
Test Calendar/SMS generation
Jul08
GSFC Launch Readiness (FRR)
Jul08
STScI SM4/SMOV Readiness Review
07Aug08
15Aug08
Feb09
MOSES
SMOV Requirements Review
12Oct07
Oct07
HST
SM4 Launch
~Dec08
SMOV4
SMOV4 Closure Review
4
SMOV4 INTRODUCTION
- ASSUMPTIONS-
HST
MOSES
• New gyros
• New batteries
• Two new Science Instruments (SIs)
– COS in place of COSTAR
– WFC3 in place of WFPC2
• 2 Restored SIs
– STIS
– ACS
• Refurbished FGS
– FGS2R2 in place of FGS2R
• Other effects
– NICMOS “warming up” for 8-10 days
5
SMOV4 INTRODUCTION
- ASSUMPTIONS, cont’d-
HST
MOSES
• Bright Earth Avoidance (BEA)
– 21 days from Release
• BE exposure allowances
– Week 2 = 2 hours
– Week 3 = 4 hours (not contiguous)
• Week 4 – No “prolonged” anti-sun pointing
– Variant of 28-day SMB recommendation of
31May07
6
SMOV4 INTRODUCTION
-APPROACH-
HST
MOSES
• Proceed with commissioning of existing SIs while new
ones outgass
• Use ACS SBC for End-BEA Check
– BEA allowance
• Perform the “long” VDT early in BEA period
• FGS2R2 – Start commissioning prerequisites early using
BEA-compatible targets and BEA allowances
– Allows relief to FGS3 guiding asap
• STIS – Use BEA-compatible targets for early
commissioning activities
• Start NCS early for NICMOS cool-down
– 2-week cooldown assumed for planning purposes
7
SMOV4 INTRODUCTION
-SCHEDULE-
HST
MOSES
• WEEK1 –
–
–
–
–
–
–
PCS -- Recover PCS/guiding control, VDT2
FGS2R – Begin S-Curves
ACS – Initial activation
COS - FUV door open (Pressure = 100 uTorr)
STIS eng activation and initial optical verification
NICMOS – Begin NCS dewar cooldown
8
HST
MOSES
• WEEK 2 –
–
–
–
–
FGS2R – Continue S-Curves
WFC3 – Mem and SDB checks, outgassing
ACS – Engineering C/Os
COS – Engineering C/O, NUV HV ramp-up (pressure
= 10 uTorr)
– STIS – FUV HV recovery, BEA-compliant cals
– NICMOS – Cooling down
9
HST
MOSES
• WEEK 3
–
–
–
–
–
–
–
PCS Gyro/FHST alignment
FGS2R – Complete S-Curves, miniOFAD, alignment
WFC3 – Outgassing
COS – FUV HV ramp-up, detector functionals
ACS - End-BEA check
STIS – NUV HV recovery, BEA-compliant cals
NICMOS – activation & engineering C/Os, filter Wheel
Test
– BEA complete
10
SMOV EXTERNAL ORBITS
BY SI/SS
HST
MOSES
BEA EXTERNAL ORBITS
PCS VDT
5 orbits after 36 Hrs @ +V3
ACS
2 orbits -- BEA WINDOW
FGS
6 orbits -- BEA WINDOW
20 orbits -- BEA COMPLIANT
STIS
8 orbits -- BEA COMPLIANT
POST-BEA EXTERNAL ORBITS
PCS
WFC3
COS
STIS
ACS
NICMOS
FGS
10 (VDT)
124*
171*
25*
34*
55*
6
425 TOTAL
* Includes ERO guestimates
11
SMOV4 INTRODUCTION
HST
-EXTERNAL ORBIT ESTIMATES-
MOSES
POST-BEA EXTERNAL ORBITS
90
ORBITS
80
70
PCS
60
NICMOS
50
STIS
40
ACS
30
COS
WFC3
20
10
0
1
2
3
4
5
6
7
8
9
10
11
12
13
14
POST-BEA WEEK
12
SMOV4 SCHEDULE
MOSES
21-DAY BEA PERIOD
ID
1
2
3
4
5
6
7
8
9
10
11
38
39
40
41
42
43
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
36
37
gust 2008
September 2008
October 2008
November 2008
December 2008
4 7 10 13 16 19 22 25 28 31 3 6 9 12 15 18 21 24 27 30 3 6 9 12 15 18 21 24 27 30 2 5 8 11 14 17 20 23 26 29 2 5 8 11 14
Task Name
Start
SM4
HST RELEASE
BEA PERIOD
PCS COMMISSIONING
Thu 8/7/0
Fri 8/15/0
Fri 8/15/0
Mon 8/18/0
Fri 8/15/0
Fri 9/5/0
Sat 9/6/0
Sat 9/6/0
Thu 8/21/0
Thu 8/21/0
Sun 8/31/0
Sat 9/6/0
Fri 9/26/0
Fri 9/26/0
Mon 8/18/0
Mon 8/18/0
Thu 8/21/0
Fri 8/22/0
Sat 9/6/0
Sun 9/7/0
Tue 8/19/0
Tue 8/19/0
Sat 9/6/0
Sat 9/6/0
Sun 9/14/0
Sun 9/14/0
Mon 10/6/0
Sun 8/17/0
Sun 8/17/0
Sun 8/17/0
Sat 9/6/0
Sat 9/13/0
Sun 9/14/0
Sat 10/4/0
Mon 8/18/0
Mon 8/18/0
Wed 9/10/0
Tue 9/9/0
Fri 9/19/0
Thu 10/2/0
Tue 8/19/0
Tue 8/19/0
Sat 9/6/0
Thu 9/11/0
Mon 12/1/0
Wed 12/10/0
Sat 9/6/0
Sat 9/6/0
Fri 9/26/0
Sun 8/31/0
Thu 9/4/0
Sat 9/6/0
Fri 9/26/0
Fri 9/26/0
Tue 9/30/0
Fri 9/5/0
Tue 9/30/0
Tue 9/30/0
Sat 9/6/0
Sun 9/7/0
Wed 10/8/0
Wed 8/27/0
Sat 9/13/0
Wed 10/8/0
Sun 9/14/0
Sun 9/14/0
Mon 10/6/0
Fri 10/31/0
Sun 8/31/0
Wed 9/3/0
Sun 10/5/0
Fri 10/31/0
Sun 9/14/0
Sat 10/4/0
Sun 10/12/0
Sat 9/13/0
Sat 9/27/0
Sun 10/12/0
Fri 9/19/0
Thu 10/2/0
Sat 12/13/0
Wed 9/10/0
Sat 11/22/0
Sat 12/13/0
Mon 12/1/0
Wed 12/10/0
GYRO CALS COMPLETE
FGS SMOV
AMA ADJUST COMPLETE
OFADs & ALIGNMENTS
FGS1R SCIENCE ENABLED
FGS2R GS ACQ VERIFICATION
FGS2R ENABLED FOR GUIDING
STIS SMOV
ENGINEERING ACTIVATION
OPTICAL VERIFICATION
SCIENCE CALIBRATIONS
CCD SCIENCE ENABLED
MAMA SCIENCE ENABLED
ACS SMOV
ENGINEERING ACTIVATION
ALIGNMENT & FOCUS
SCIENCE CALS
CCD SCIENCE ENABLED
SBC SCIENCE ENABLED
CORONOGRAPHIC SCIENCE ENABLED
NICMOS SMOV
COOLDOWN
ENGINEERING ACTIVATION
OPTICAL ALIGNMENT & FOCUS
SCIENCE CALS
CAMERA SCIENCE ENABLED
CORONOGRAPHIC SCIENCE ENABLED
WFC3 SMOV
ENGINEERING ACTIVATION
OPTICAL ALIGNMENT
SCIENCE CALS
UVIS SCIENCE ENABLED
IR SCIENCE ENABLED
COS SMOV
ENGINEERING ACTIVATION
ALIGNMENT & FOCUS
SCIENCE CALS
NUV SCIENCE ENABLED
FUV SCIENCE ENABLED
Finish
HST
8/15
9/6
9/6
9/6
9/26
9/26
9/6
9/7
9/14
9/14
10/6
9/14
10/4
9/19
10/2
12/1
13
12/10
HST
MOSES
Pointing Control System
SMOV4 PLAN
14
HST
PCS Activities
MOSES
Objective: To return HST Normal Science Operations
h Initialize Fine Attitude
h Remove initial gyro rate bias error
h Verify the FHST/FHST alignments and update if
necessary
h Determine and correct RGA/FHST alignment errors
h Determine and correct FHST/FGS alignment errors
h Characterize disturbance sources and determine jitter
15
HST
PCS Activities
MOSES
Activity Summary #
Observatory
Verification Activity
Related SMOV
Requirement
Execution Method
Duration
(HH:MM)
PCS-1
FHST FOV Check
L.10.4.8.1
R/T Command
3:00
PCS-2
Fine Attitude
Determination
L.10.4.8.1
R/T Command
PCS-3
Gyro Rate Bias
Correction
L.10.4.8.1
R/T Command
PCS-4
FHST/FHST
Alignment
L.10.4.8.2
R/T Command
PCS-6
Gyro/FHST
Alignment
L.10.4.8.2
PCS-7
FHST/FGS
Alignment
L.10.4.8.3
PCS-8
Vehicle Disturbance
Test (VDT)
L.10.4.8.6
1:00
3:00
31:00
SMS
56:00
SMS
75:00
SPC/SMS
24:00
16
HST
PCS-1 FHST FOV Check
MOSES
Purpose: Verifies that the FHSTs are mapping normally
and that the observations can be used for attitude
determination (Req. J.10.4.8.1).
Description: FHSTs will be commanded in real time to
perform maps of their full FOV and the observations will
be analyzed to determine if the FHST performance is
adequate for subsequent activities (initial attitude and
gyro bias determination, attitude initialization and RGA to
FHST calibration). This activity is expected to last three
hours.
17
PCS-2 Fine Attitude
Determination
HST
MOSES
• Purpose: Determine the vehicle attitude using FHST
observations and update the On Board quaternion. This
activity is needed to return to normal operations (Req.
J.10.4.8.1).
• Description: The FHSTs will be commanded in real
time to perform a full FOV map. The observations will be
used to compute an Attitude Reference that is uplinked
to FSW. The duration for this activity is about one hour.
18
PCS-3 Initial Gyro Rate
Bias Corrections
HST
MOSES
Purpose: Compute the initial low mode gyro
uncompensated rate bias to reduce the vehicle low
mode rate error to less than .014 arcseconds per
second. This will allow a return to normal vehicle
operations (Req. J.10.4.8.1).
Description: FHST maps are used to measure the vehicle
attitude drift due to uncompensated gyro rate bias.
Attitude change while holding on gyros will be used to
determine the low mode rate bias. This real time map
activity is expected to last two hours. An additional
hour is needed for data processing, data validation, and
Table Load generation.
19
PCS-4 FHST/FHST
Alignment Check
HST
MOSES
Purpose: Verify the FHST/FHST alignment prior to using
the FHSTs for vehicle attitude updates (Req.
J.10.4.8.2).
Description: With the vehicle at a constant attitude each
pair of FHSTs will be commanded in real time to perform
a full FOV map. The observations from these maps will
be used to compute an FHST/FHST alignment. This
alignment will be compared to the pre-Servicing Mission
alignment. If there is a change of 20 arcseconds or
greater in the pitch or yaw components, a new
alignment will be uplinked to the vehicle. This activity
requires seven hours of data collection, and 24 hours of
analysis time.
20
PCS-6 Gyro/FHST
Alignment
HST
MOSES
Purpose: This activity is required to calibrate a new set of
gyros to maintain errors after a maneuver to less than
one arcsecond per degree of slew (Req. J.10.4.8.2).
Description: Six maneuvers are performed. Each
maneuver is about one of the vehicle axes with a slew
angle of + or - 90 degrees. Before and after each
maneuver the FHSTs perform a map of their full FOV.
This set of maneuvers is repeated approximately 24
hours later to verify the new calibration. This activity
requires about 56 hours to complete. The maneuvers
require 8 hours to execute. Approximately 24 hours are
required to process the data and uplink Table Loads.
Another 8 hours are needed for the verification slews
and about 16 hours to process the verification data. This
activity is implemented via an SMS proposal.
21
PCS-7 FHST/FGS
Alignment
HST
MOSES
Purpose: This is a contingency activity that allows the
FHSTs to be realigned to the FGS system. This is
needed to ensure that FHST updates following
maneuvers will result in successful FGS guide star
acquisitions. This activity will be performed if guide star
acquisitions are failing. (Req. J.10.4.8.3)
Description: FGS will map out its FOV using coarse track
astrometry observations while the FHSTs are mapping
their FOVs. The FHST/ FGS alignment will be computed
and Table Loads will be uplinked to the vehicle. The
duration for this activity is 75 hours. The data collection
requires 3 hours and the subsequent data processing
requires about 48 hours. An additional 24 hours is
needed to update the ground system and generate Table
Loads for uplink to the vehicle. This activity is
22
implemented via an SMS proposal.
HST
PCS-8 VDT
MOSES
Purpose: The purpose of the Vehicle Disturbance Test is
to characterize disturbances acting upon the HST during
normal operations. This activity was previously done
after Servicing Missions to establish a signature for
disturbance baseline of the vehicle. (Req. J.10.4.8.6)
Description: The test consists of 2 orbits in a +V3
sunpoint attitude while performing COS and WFC3
mechanism motion, 8 orbits of +V3 sunpoint after
achieving thermal equilibrium (3 orbits with RWA friction
compensation disabled) and 5 orbits in a –V1 sunpoint
(all or part with RWA friction compensation disabled).
The control law is commanded to use maneuver gains,
and the gyros are commanded to low mode. Nominal
gains are restored at the end of each test interval. The
+V3 sunpoint portion can be done during the BEA
23
period.
HST
MOSES
Thermal Control System (TCS)
SMOV4 PLAN
24
TCS
Engineering Activities
HST
MOSES
• TCS01 – NOBL Performance Verification
• Requirement
– L.10.4.13.1 Characterize the affect of NOBL
installation on SSM Bay 5, 7, and 8 equipment
temperatures
• Description of activity
– SSM Bay 5, 7, and 8 equipment temperatures will be
trended throughout SMOV and compared with
thermal model predictions as the observing schedule
permits
– No special observing attitudes or durations are
required
25
HST
MOSES
SMOV4 EPS
26
HST
EPS
MOSES
• L.10.4.14.1 Characterize the Replacement
Battery Performance.
– An AD for to verify this requirement does not exist.
This requirement will be verified during normal
operations, and reported to HST Project.
• L.10.4.14.2 Characterize the Science Instrument
and NCS Electrical Loads.
– An AD for to verify this requirement does not exist.
This requirement will be verified during normal
operations, and reported to HST Project.
27
HST
MOSES
Optical Telescope Assembly
and the
Fine Guidance Sensors
SMOV4 PLAN
E. Nelan, M. Lallo, A. Bradley, &
Abramowicz-Reed
L.
28
SMOV4 Activities for OTA
& FGS
Activity
Summary #
Observatory Verification Activity
Execution
Phase
OTA-01
Cross-SI & Observatory Focus
N/A
N/A
OTA-02
Positional Alignment of SI & FGS
SMS
N/A
OTA/FGS-03 Guide Star Acquisition
Verification
SMS
03:00
OTA/FGS-04 Optimize FGS2 S-curves
SMS
39:00
OTA/FGS-05 FGS2-to-FGS Alignment
SMS
07:30
OTA/FGS-06 FGS2 Plate Scale and Distortion
Calibration
SMS
07:30
OTA/FGS-07 FGS2 Guide Star Acquisition
Verification
SMS
03:00
OTA/FGS-08 Characterize FGS1, FGS2, & FGS3
pre-SM4 performance
SMS
06:00
OTA/FGS-09 Re-commission FGS1 and FGS3
SMS
06:00
OTA/FGS-10 Near Term Stability Check of FGS2
SMS
03:00
OTA/FGS-11 Calibrate FGS2 PMT Response
SMS
N/A
FGS/OTA-12 Map FGS2 Obscuration Zone
Ground
N/A
FGS/OTA-13 Calibrate FGS2 PMT Dark Count
AT & FT
N/A
HST
MOSES
Duration
Hr:min
29
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA-01 – Cross-SI & Observatory Focus
– Requirement L.10.4.7.1.1
– Intent was to use ACS to monitor HST focus before and after SM4.
• HRC has not been available to establish pre-SM4 baseline
• SBC found to not be a viable focus monitor (detector effects, UV PSF,
etc.)
• WFPC2 to be removed. NIC late to observe & not best OTA proxy.
• Thus little ability to accurately measure HST focus pre/post SM4
– Request waiver of requirement.
– Low risk:
• HST focus has not changed significantly across previous servicing mission
boundaries & current OTA focus maintanence will ensure entering SM4 at best
PC/OTA focus (to which STIS, NICMOS & ACS have been set earlier)
• COS & WFC3 will actively focus to within their SMOV requirements as planned.
30
OTA & FGS SMOV4
Activities
HST
MOSES
• OTA-02 – Alignment of SI & FGS
– Requirement L.10.4.7.2.1
– Confirm that the alignment of ACS, STIS, and NICMOS are
within 2” in (v2,V3) and 0.2 deg in orientation of their pre-SM4
locations.
– This requirement is to be verified by SMOV4 plan for each of the
affected instruments.
– We expect to enter SMOV4 with up to date alignment
calibrations for ACS/SBC & NICMOS relative to FGS1 & FGS3.
– Alignment data were acquired in Fall, 2006, updates to PDB are
being implemented. Alignments will be checked in Fall, 2007
(Cycle 16 OTA Calibration Plan).
31
OTA & FGS SMOV4
Activities
HST
MOSES
• OTA/FGS-03 – Guide Star Acquisition Verification
– Requirement L.10.4.7.3.1
– Guide star pair to be acquired in Finelock by FGS1 and FGS3.
• STScI will choose guide star pairs that have been successfully
acquired in the past.
• FGS1 and FGS3 will be used, in turn, as the primary and dominate
guider during the test.
• Test duration ~2 orbits
• Test executes in BEA, shortly after completion of the H&S SMS
(day 3 or 4 of SMOV)
32
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-04 – Optimize FGS2 S-curves
– Requirement L.10.4.7.3.2
– FGS2 observes a point source in Transfer mode to obtain
interferograms (S-curves) across the FGS FOV.
– The S-curve properties will inform the adjustment of the AMA to
optimize interferometric performance across the FGS2 FOV.
– Data analysis and AMA adjustments to be determined by Goodrich.
– Goodrich has requested three iterations.
– Observations will require 20 HST orbits over four visits spanning a 6day period (3POL, 3POL, 5 POL, 9POL).
– We are searching for BEA compliant targets.
33
HST
FGS2 On orbit, 1999
MOSES
34
HST
FGS2 Ground Alignment
MOSES
S-Curve(s) at Pickle Position(s) for FGS S/N 2004 X-Axis, Full Aperture
Pos= 7 P2P=1.19 Dec= 0.15
Pos=15 P2P=1.21 Dec= 0.19
Pos= 6 P2P=1.09 Dec= 0.17
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.2
-0.1
0.0
0.1
0.2
Pos= 4 P2P=1.20 Dec= 0.12
-0.1
0.0
0.1
0.2
Pos= 5 P2P=1.15 Dec= 0.15
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.0
0.1
0.2
Pos=12 P2P=1.14 Dec= 0.21
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.0
0.1
0.2
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.1
0.0
0.1
0.2
0.1
0.2
-0.1
0.0
0.1
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
Pos=13 P2P=1.14 Dec= 0.10
-0.2
-0.1
0.0
0.1
0.2
Pos= 2 P2P=1.08 Dec= 0.15
-0.1
0.0
0.1
0.2
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.2
-0.2
-0.1
0.0
0.1
0.2
-0.1
0.0
0.1
0.2
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.2
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.1
0.0
0.1
0.2
Pos= 1 P2P=1.08 Dec= 0.15
Pos=10 P2P=1.19 Dec= 0.06
-0.2
-0.2
-0.2
0.0
Pos= 8 P2P=1.19 Dec= 0.10
-0.1
Pos=11 P2P=1.19 Dec= 0.18
-0.1
-0.1
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.2
-0.2
-0.2
Pos=14 P2P=1.21 Dec= 0.10
Pos= 3 P2P=1.22 Dec= 0.13
-0.2
-0.2
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.2
-0.1
0.0
0.1
0.2
Pos= 9 P2P=1.14 Dec= 0.01
-0.2
-0.1
0.0
0.1
0.2
Decenter values are in mm
0.6
0.4
0.2
0.0
-0.2
-0.4
-0.6
-0.2
-0.1
0.0
0.1
0.2
Time range of data on graph: 2006:178:15:28:03 thru 2006:181:20:06:23
Graph generated by marilynn.chisholm on Wed Aug 09 08:07:09 2006 using PMatrix Version 1.1
35
FGS2r AMA Adjustments
(SMOV3A)
Pre-AMA
HST
MOSES
Post-AMA
36
HST
FGS2r, 2000 and 2002
March, 2000
MOSES
Jan, 2002
37
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-05 – FGS2 to FGS Alignment
– Requirement L.10.4.7.3.3
– FGS to FGS alignment must be known to an accuracy of ~100 mas.
• Alignment of FGS1 & FGS3 has been calibrated.
• Their post-SM4 alignment to be checked using data from other activities.
– The alignment of FGS2 to FGS1 & FGS3 must be calibrated.
• During FGS2r commissioning in SMOV3A, the initial alignment error was
approximately 20”!
– Calibration requires 5 HST orbits to observe astrometric stars in M35.
– GSFC performs analysis of the data and reports results to STScI for
database updates (OTA/FGS-06, distortion must be calibrated first).
– FGS2 preliminary alignment must first be updated using AMA test data
before these observations are made.
38
HST
FGS2 to FGS Alignment
MOSES
39
HST
FGS2 to FGS Alignment
MOSES
40
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-06 – FGS2 Distortion and Plate Scale Calibration
– Requirement L.10.4.7.3.4
– FGS2 optical distortion and plate scale are to be calibrated to 40 mas
and 2.7 x 10-5, respectively..
– This is accomplished by observing astrometric stars in M35..
– Calibration requires 5 HST orbits.
– GSFC performs analysis of the data and reports results to STScI for
database updates.
– Observations are to execute after completing the AMA S-curve
optimization, and after FGS2 alignment update (based upon AMA test
data).
41
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-07 – Verify FGS2 Guide Star Acquisition
– Requirement L.10.4.7.3.5
– Verify FGS2 as an HST guider. Specific guide star pairs that have been
successfully acquired in the past will be acquired by FGS2 and FGS3.
FGS1r will be used as an “astrometer” in Position mode measure HST
jitter with FGS2 in the guide loop.
– Calibration requires 2 HST orbit.
– Observations are to execute after completing the FGS2 to FGS
alignment and FGS Distortion and Plate Scale database updates
(L.10.4.7.3.3, L.10.4.7.3.4).
42
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-08 –Pre-SM4 characterization of FGS1,2,&3
– Requirement L.10.4.7.3.6
– Characterize the performance of FGS1, FGS2, and FGS3 pre-SM4 to
establish a pre-SM4 baseline.
• Acquire S-curves at the center of each FGS
• Observe the relative positions of stars in M35 distributed across each FGS FOV.
– FGS1r will use data from the Cycle 16 astrometry calibration program.
– Characterization of FGS2 and FGS3 distortions will use data from the
Cycle 16 alignment check (Fall, 2007).
– FGS2 & FGS3 S-curve characterization require one dedicated HST orbit
each.
– FGS2 is checked in the event that it is not replaced in SM4.
43
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-09 - Recommission FGS1 and FGS3
– Requirement L.10.4.7.3.7
– Compare post-SM4 S-curves and distortion & plate scale in FGS1 and
FGS3 to those from before SM4 (OTA/FGS-08).
• Acquire S-curves at the center of each FGS
• Observe the relative positions of stars in M35 distributed across each FGS
FOV.
– These data verify that the FGS calibration for guiding remains valid.
– FGS1r will use data from the Cycle 17 astrometry calibration program.
• This will also be used to verify FGS1r for astrometry science.
– FGS3 S-curve and distortion characterization require two dedicated
HST orbits.
44
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-10 - Near Term Stability of FGS2
– Requirement L.10.4.7.3.8
– FGS2 interferometric properties are expected to experience significant
changes over the course of FGS2’s first two years on orbit due to out
gassing.
– Monitor the performance of FGS2.
• Every 2 to 4 months, acquire S-curves at the center of FGS2
• Every 2 to 4 months, observe the relative positions of stars in M35
distributed across each FGS2 FOV.
– These data verify that the FGS2 calibration for guiding remains valid.
– These data are to be acquired as part of the Cycle 17 Calibration
Program. Request waiver of this requirement for SMOV4 as it will
become a requirement for routine operations.
45
OTA & FGS SMOV4
Activities
•
HST
MOSES
OTA/FGS-11 - FGS2 PMT Calibration
– Requirement L.10.4.7.3.9
– FGS2 photometric response is to be calibrated using data acquired from the
optical distortion calibration (OTA/FGS-06).
– PMT calibration is needed to commission FGS2 as a guider.
•
OTA/FGS-12 - FGS2 Obscuration Zone
– Requirement L.10.4.7.3.10
– The OCS aperture in the FGS FOV can not be used to observe astronomical
objects. Its location in the FOV must be known by the ground system.
– Its location in the FOV is to be measured on orbit using the ITS. Goodrich will
analyze these data and provide the results to STScI.
•
OTA/FGS-13 - FGS2 Dark Count Rate
– Requirement L.10.4.7.3.11
– The FGS dark count rate must be known to support the PMT calibration. These
data are to be acquired from the Aliveness Test and Functionality Test.
46
HST
MOSES
Wide Field Camera 3
SMOV4 PLAN
John MacKenty & Margaret Turnbull
47
HST
Approach
MOSES
• WFC3 schedule constrained by 21 day detector
venting period prior to cooling detectors.
• Three phase approach (parallels requirements):
– Engineering Checks
– Optical Alignment
– Calibration
• Bifurcated SMOV4 design to avoid linkage
between UVIS and IR channels
– Each can proceed at its own pace
– Only linked test is the CSM check
48
HST
Notes
MOSES
• Requested external orbits = 132
• Additional requirement to assess IR
channel photometric stability (10 orbits)
– Result of TV2 – might be resolved by TV3
• SMOV does not
– Check UVIS or IR Grisms (unlike ACS)
– Optimize Earth limb restriction
49
HST
Requirements Matrix (1)
MOSES
Requirements
After
INT
1.1.1, 1.1.3
Release
Load and Dump On-board Memory
INT
1.1.4
Release
Petro
Science Data Buffer Check
INT
1.1.5
Release
WF04
MacKenty
UVIS CCD Activation
INT
1.1.2
21 days
WF05
MacKenty
IR Detector Activation
INT
1.1.2
21 days
WF06
Baggett
UVIS Detector Functional test
INT
1.1.8
WF04
WF07
McCullough
IR Detector Functional test
INT
1.1.9
WF05
WF08
Bushouse
Channel Select Mechanism Test
2
1.1.6
WF06, WF07
WF09
Baggett
SOFA and Tungsten Lamp test
INT
1.1.6, 1.1.7
WF06
WF10
Baggett
IR FSM and Tungsten Lamp Test
INT
1.1.6, 1.1.7
WF07
WF11
Hartig
UVIS Initial Alignment
6
1.2.1, 1.2.2
WF09
WF12
Hartig
IR Initial Alignment
6
1.2.1, 1.2.2
WF10
WF13
Turnbull
UVIS SMOV Contamination Monitor
20
1.1.12, 1.3.6
WF06
WF14
Hilbert
UVIS Shutter test
1
1.1.6
WF11
WF15
Baggett
D2 Calibration lamp test
INT
1.1.7
WF06, WF11
WF16
Petro
UVIS TEC Performance
INT
1.1.10
WF11
WF17
Petro
IR TEC Performance
INT
1.1.10
WF12
WF18
Baggett
UVIS Hot Pixel Anneal
INT
1.1.11
WF06-TBR
WF19
Kim
UVIS Internal Flats
INT
1.3.7, 1.1.6, 1.1.7
WF11
WF20
Hilbert
IR Internal Flats
INT
1.3.7, 1.1.6, 1.1.7
WF12
AD
PI
Title
WF01
Petro
Activation Test (FT)
WF02
Petro
WF03
Orbits
50
HST
Requirements Matrix (2)
MOSES
Requirements
After
6
1.2.1, 1.2.2
WF11
IR Fine Alignment
6
1.2.1, 1.2.2
WF12
Hartig
UVIS Image Quality
4
1.2.2
WF21
WF24
Hartig
IR Image Quality
4
1.2.2
WF22
WF25
Hartig
UVIS PSF Wings
5
1.2.4
WF21
WF26
Hartig
IR PSF Wings
5
1.2.4
WF22
WF27
Brown
UVIS Pointing Stability
6
1.2.3
WF21
WF28
Brown
IR Pointing Stability
6
1.2.3
WF22
WF29
Dressel
FGS-UVIS Alignment
1
1.3.2
WF21
WF30
Dressel
FGS-IR Alignment
1
1.3.2
WF22
WF31
Dressel
UVIS Plate Scale
4
1.3.1
WF21
WF32
Dressel
IR Plate Scale
4
1.3.1
WF22
WF33
Baggett
UVIS Dark current, read-noise, CTE
INT
1.3.3
WF16
WF34
McCullough
IR Dark current, read-noise, background
6
1.3.3
WF17
WF35
Martel
UVIS SAA Passage Behavior
INT
1.3.5
WF16
WF36
Martel
IR SAA Passage Behavior
INT
1.3.5
WF17
WF37
Brown
UVIS Photometric Zero Points
10
1.3.6
WF21
WF38
Brown/Riess
IR Photometric Zero Points
8
1.3.6
WF22
WF39
Kim
UVIS Flat Field uniformity
12
1.3.7
WF21
WF40
Hilbert
IR Flat Field Uniformity
9
1.3.7
WF22
AD
PI
Title
WF21
Hartig
UVIS Fine Alignment
WF22
Hartig
WF23
Orbits
51
WFC3
Engineering Activities
HST
MOSES
• WF01 – Activation Test
– Re-run of SM4 FT to confirm basic function and
stability of instrument.
– Can be done prior to detector cool-downs.
• WF02 – Load and Dump On-board Memory
– Derived from SMOV3B-ACS-02.
– Can be done prior to detector cool-downs.
– Requires special commanding.
• WF03 – Science Data Buffer Check
– Derived from SMOV3B-ACS-03.
– Can be done prior to detector cool-downs.
52
WFC3
Engineering Activities
HST
MOSES
• WF04 – UVIS CCD Activation
– Verify that detector temperature is stable as desired set point.
– Follows 21 day detector venting period.
• WF05 – IR Detector Activation
– Verify that detector is temperature is stable as desired set point.
– Follows 21 day detector venting period.
• WF06 – UVIS Detector Functional test
– Verify detector readout operation, noise level, and gain.
– Obtain series of darks and internal flat fields.
• WF07 – IR Detector Functional test
– Verify detector readout operation, noise level, and gain.
– Obtain series of darks and internal flat fields.
53
WFC3
Engineering Activities
HST
MOSES
• WF08 – Channel Select Mechanism Test
– Verify proper positioning of CSM IR fold mirror and IR diffuse
paddle. Verify unobstructed UVIS beam.
• WF09 – SOFA and Tungsten Lamp test
– Verify operation of all SOFA filter wheels. Verify operation of at
least 2 Tungsten lamps.
– Obtain internal flat fields in one filter from each wheel.
– Establishes an initial baseline over a broad wavelength range.
• WF10 – IR FSM and Tungsten Lamp Test
– Verify operation of FSM. Verify operation of at least 2 Tungsten
lamps.
– Establishes an initial baseline for all IR filter elements.
54
WFC3
Engineering Activities
•
HST
MOSES
WF13 – UVIS SMOV Contamination Monitor
– Derived from SMOV3B-ACS-10.
– Standard star observations in F218W, F225W, F275W, and F606W one
per week during SMOV at two locations (one per CCD chip) using
subarrays.
– With the inclusion of bias, dark, and internal flats in F225W and F606W,
this activity also serves as the UVIS stability monitor during SMOV.
•
WF14 – UVIS Shutter test
– Verify operation and timing of the UVIS shutter mechanism.
– Obtain internal flat fields over a range of exposure times to verify shutter
shading is unchanged from ground testing.
– Obtain observations of a standard star at 0.5, 0.7, 1.0, 1.5, and 2.0
seconds at four locations within the FOV using subarrays.
•
WF15 – D2 Calibration lamp test
– Verify operation of D2 lamp via UV filter internal flat fields.
– Establishes an initial baseline for UV filter elements.
– Determine on-orbit range of D2 lamp “turn-on” times.
55
WFC3
Engineering Activities
•
HST
MOSES
WF16 – UVIS TEC Performance
– Derived from SMOV3B-ACS-06.
– Monitor UVIS TEC performance over a range of S/C pointings and over
orbit phase.
– Adjust detector temperature setpoint if analysis indicates inability to hold
nominal setpoint over Cycle 17.
•
WF17 – IR TEC Performance
– Derived from SMOV3B-ACS-06.
– Monitor IR TEC performance over a range of S/C pointings and over orbit
phase.
– Adjust detector temperature setpoint if analysis indicates inability to hold
nominal setpoint over Cycle 17.
•
WF18 – UVIS Hot Pixel Anneal
–
–
–
–
–
Derived from SMOV3B-ACS-31.
Demonstrate ability to performance UVIS anneal.
Obtain pre- and post-anneal series of ten 600 second dark images.
Note(1): perform within 30 days of initial cool-down of UVIS detector.
Note(2): succeeded by Cycle 17 UVIS Anneal proposal after successful
completion of two iterations of WF18.
56
WFC3
Alignment Activities
•
–
–
Derived from SMOV3B-ACS-13.
Obtain images of sparse star field (NGC 188) and position tip-tilt and piston corrector
mechanisms based on phase retrieval.
Requires two iteration opportunities.
WF21 – UVIS Fine Alignment
–
–
–
–
–
•
Derived from SMOV3B-ACS-13.
Obtain images of sparse star field (NGC 188) and position tip-tilt and piston corrector
mechanisms based on phase retrieval.
Requires two iteration opportunities.
WF12 – IR Initial Alignment
–
–
•
MOSES
WF11 – UVIS Initial Alignment
–
–
•
HST
Derived from SMOV3B-ACS-13.
Observe a sparse star field (NGC 188) over a 7 step internal focus sweep.
Update optimal focus (real-time uplink?)
Observe a sparse star field (NGC 188) over a 3x3 internal tip-tilt sweep.
Update optimal tip-tilt alignment position (real-time uplink?)
WF22 – IR Fine Alignment
–
–
–
–
–
Derived from SMOV3B-ACS-13.
Observe a sparse star field (NGC 188) over a 7 step internal focus sweep.
Update optimal focus (real-time uplink?)
Observe a sparse star field (NGC 188) over a 3x3 internal tip-tilt sweep.
Update optimal tip-tilt alignment position (real-time uplink?)
57
WFC3
Calibration Activities
HST
MOSES
• WF19 – UVIS Internal Flats
– Obtain internal flat fields using the D2 and Tungsten
lamps (as appropriate for each filter).
– At least 4 full-frame flat-field images are obtained for
each filter element.
• Ten images are obtained for all High priority (class 1) filters.
• Twenty images are obtained for all UV filters (D2 lamp only).
• Ten images are obtained for all ERO filters.
• WF20 – IR Internal Flats
– Obtain internal flat fields using the Tungsten lamps.
– At least 10 full-frame flat-field images are obtained for
each filter element.
• Twenty images are obtained for all High priority (class 1)
filters and for all ERO filters.
58
WFC3
Calibration Activities
HST
MOSES
• WF23– UVIS Image Quality
– Derived from SMOV3B-ACS-15.
– Detailed characterization of the achieved image quality using the
NGC 6681 or NGC 188 sparse star field.
– Four observations using a 2x2 dither pattern with 0.5 pixel steps
will be obtained at two pointings offset by 10 arc seconds.
– Observations will be obtained in the F275W and F631N filters.
• WF24 – IR Image Quality
– Derived from SMOV3B-ACS-15.
– Detailed characterization of the achieved image quality using the
NGC 188 sparse star field.
– Four observations using a 2x2 dither pattern with 0.5 pixel steps
will be obtained at two pointings offset by 10 arc seconds.
– Observations will be obtained in the F098M and F164N filters.
59
WFC3
Calibration Activities
•
HST
MOSES
WF25 – UVIS PSF Wings
– Observations of a moderately bright star (TBD) over a factor of 128 in exposure
time will be obtained to characterize the wings of the PSF.
– Observations will be obtained in the F275W and F621M filters (TBR).
– A series of 8 images (multiples in exposure time of 1,2,4,8,16,32,64,128) will be
obtained near the center of the FOV with the first image at ~2/3 full well.
– Four additional images at ~100x full well will be obtained at positions ~20 arc
seconds in from each corner of the FOV.
•
WF26 – IR PSF Wings
– Observations of a moderately bright star (TBD) over a factor of 128 in exposure
time will be obtained to characterize the wings of the PSF.
– Observations will be obtained in the F098M and F153M filters (TBR).
– A series of 8 images (multiples in exposure time of 1,2,4,8,16,32,64,128) will be
obtained near the center of the FOV with the first image at ~2/3 full well.
– Four additional images at ~100x full well will be obtained at positions ~20 arc
seconds in from each corner of the FOV.
– These data will also serve to characterize the persistence in the IR detector.
60
WFC3
Calibration Activities
•
HST
MOSES
WF27 – UVIS Pointing Stability
– Derived from SMOV3B-ACS-17.
– Measure UVIS line of sight pointing stability via observations of a dense
star field.
– Requires a series of ~300 second exposures over 2 orbits.
– Perform three times:
• When HST has been in a constant attitude for 10 orbits.
• Immediately following a slew from hot to cold attitude.
• Immediately following a slew from cold to hot attitude.
•
WF28 – IR Pointing Stability
– Derived from SMOV3B-ACS-17.
– Measure IR line of sight pointing stability via observations of a dense
star field.
– Requires a series of ~300 second exposures over 2 orbits.
– Perform three times:
• When HST has been in a constant attitude for 10 orbits.
• Immediately following a slew from hot to cold attitude.
• Immediately following a slew from cold to hot attitude.
61
WFC3
Calibration Activities
•
HST
MOSES
WF29 – FGS-UVIS Alignment
– Derived from SMOV3B-ACS-11.
– Observations of NGC 188 at three positions separated to at least 10 arc
seconds and moving in orthogonal directions will be obtained.
•
WF30 – FGS-IR Alignment
– Derived from SMOV3B-ACS-11.
– Observations of NGC 188 at three positions separated to at least 10 arc
seconds and moving in orthogonal directions will be obtained.
•
WF31 – UVIS Plate Scale
– Derived from SMOV3B-ACS-27 (smaller scope).
– Determine geometric scale factors and distortion from observations of a
dense star field (e.g. globular cluster field).
•
WF32 – IR Plate Scale
– Derived from SMOV3B-ACS-27 (smaller scope).
– Determine geometric scale factors and distortion from observations of a
dense star field (e.g. globular cluster field).
62
WFC3
Calibration Activities
HST
MOSES
• WF33 – UVIS Dark current, read-noise, CTE
– Measure and monitor UVIS detector:
• Dark Current
• Read-noise
• CTE
– Track development of warm, hot, and dead pixels.
• WF34 – IR Dark current, read-noise, background
– Measure and monitor IR detector:
• Dark Current
• Read-noise
• CTE
– Track development of warm, hot, and dead pixels.
– Determine non-detector background levels for each W&M filter.
• Limited to single (medium) zodiacal light level.
63
WFC3
Calibration Activities
HST
MOSES
• WF35 – UVIS SAA Passage Behavior
– Obtain series of dark frames within and for two orbits
following SAA passage.
– Demonstrate successful operation within SAA.
– Determine aftereffects of SAA exposure.
– Optimize WFC3/UVIS SAA contour.
• WF36 – IR SAA Passage Behavior
– Obtain series of dark frames within and for two orbits
following SAA passage.
– Demonstrate successful operation within SAA.
– Determine aftereffects of SAA exposure.
– Optimize WFC3/IR SAA contour
64
WFC3
Calibration Activities
HST
MOSES
• WF37 – UVIS Photometric Zero Points
– Derived from SMOV3B-ACS-20.
– Photometric standard star will be observed in each
Priority 1, 2, and ERO filter using sub-arrays.
– Key subset (~6 filters) will be re-observed on time
scales of 1, 7, and 30 days.
• WF38 – IR Photometric Zero Points
– Derived from SMOV3B-ACS-20.
– Two photometric standard stars (red and blue) will be
observed in each filter.
– Key subset (~4 filters) will be re-observed on time
scales of 1, 7, and 30 days.
65
WFC3
Calibration Activities
HST
MOSES
• WF39 – UVIS Flat Field uniformity
– Derived from SMOV3B-ACS-18.
– Calibrated star field will be observed to assess quality
of low frequency flat fields.
– A 3x3 dither pattern will be obtained in 5 filters.
• WF40 – IR Flat Field uniformity
– Derived from SMOV3B-ACS-18.
– Calibrated star field will be observed to assess quality
of low frequency flat fields.
– A 3x3 dither pattern will be obtained in 4 filters.
66
WFC3
Calibration Activities
HST
MOSES
• WF41 – IR Detector Stability
– Monitor of IR detector to track:
• Photometric zero point (4 filters)
• Dark current
– Contingency activity
67
HST
MOSES
COSMIC ORIGINS SPECTROGRAPH
SMOV4 PLAN
68
68
HST
Agenda
MOSES
• COS Plan Overview
–
–
–
–
–
–
–
–
COS SMOV “Philosophy”
Changes since March Requirements Review
Specially commanded and Real-time activities
NUV at a glance
FUV at a glance
Requirements Verification Matrix
Activities and Orbit Allocation
Flow Charts
• Detailed Activity Review
69
COS Plan Overview
HST
COS SMOV “Philosophy”
MOSES
• Subsequent to HST release, SI activities:
– Recover from SAFE
– Check memory
– Check Science Data Buffer
• Commence detector-based activities
• NUV first (due to FUV pressure constraint)
• FUV commences before NUV finished
70
COS Plan Overview
Changes since Req Review
HST
MOSES
• Request Requirement be Deleted
– 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.
– This capability is NOT a science-requirement; QE grid
will be turned off ONLY in event of serious failure.
71
COS Plan Overview
“Special” Activities
HST
MOSES
• Special Commanding Activities
–
–
–
–
SI Memory Check (COS02)
Science Data Buffer Check (COS03)
NUV Initial Turn-on and HV Ramp-Up (COS04)*
NUV Foldtest (COS07)
• Verification lien: test against SI in Dec 2007
– FUV Initial Turn-on and HV Ramp-up (COS23)*
• Real-Time Activities
– FUV Door Open (COS22)
* Also contains real-time commanded action
72
COS Plan Overview
HST
NUV at a glance
MOSES
• NUV HV Ramp-up (COS04)
• NUV Darks, Functional, and Foldtest
(COS05-07)
• Commence Alignment Activities
– COS to FGS (COS08)
– Optical Alignment (COS09)
• Science-related activities (COS10 et seq
see flow chart)
73
COS Plan Overview
HST
FUV at a glance
MOSES
•
•
•
•
FUV door open (COS22)
FUV HV Ramp-up (COS23)
FUV darks and functional (COS24-25)
Commence FUV optical alignment
(COS26)
• Science-related activities (COS27 et seq
see flow chart)
74
COS Plan Overview
HST
Requirements Verification Matrix
Requiremen
t
Requirement
Activities
special
comm
02
03 04 07 23
real-time
04
22 23
1.1
01
s
1.3
04
normal
op
1.4
s
02
1.5
s
03
1.6
s,r
04
1.7
s
23
1.8
1.9
Activities
L10.4.2+
L10.4.2+
1.2
MOSES
06
delete
29 30 34 23 01
14 16 25 29 05 11 09 24 26 28 31
1.11
normal
op
normal
op
2.1
19
34
22 23 06
1.10
2.2
r
04
2.3
s
22
10 06 07
3.5.1
11
3.5.2
12
3.6.1
13
3.6.2
13
3.6.3
13
3.7.1
14
15
3.7.2
16
17
3.7.3
17
3.7.4
18
3.7.5
19
3.7.6
20
3.7.7
21
3.8
24
3.9
26
3.10
26
3.11.1
28
3.12.1
29
30
3.12.2
31
32
3.12.3
32
3.12.4
33
3.1
05
3.12.5
34
3.2
08
3.12.6
35
3.3
09
3.12.7
36
3.4
09
3.13
16
27 25 07
75
17 31 32 11 13
COS Plan Overview
HST
MOSES
COS Activities / Requirements
Activity No.
COS01
Title
Instrument States; Data Interface
and Data Transmission
Verification
Req
L10.4.2+
1.1
Activity No.
1.2
COS02
On-Board Memory Check
1.4
COS03
Science Data Buffer Check
1.5
COS04
NUV Detector Initial HV Turn
On & RampUp
COS05
NUV Detector Dark
COS06
NUV Detector Internal
Functionality and Operation
COS07
NUV Fold Test
1.2;
1.6
3.1
1.8
2.2
3.8
COS08
COS to FGS Alignment (NUV)
3.2
COS09
NUV Optics Alignment and
Focus
3.3
3.4
COS10
Internal NUV Wavelength
Measurement
3.1
COS11
NUV Imaging Acquisition
Algorithm Verification
3.5.1
3.13
COS12
NUV Dispersed-light Acquisition
Algorithm Verification
3.5.2
NUV Imaging Performance
3.6.1
3.6.2
3.6.3
3.13
3.7.1
1.8
COS13
COS14
COS15
COS16
NUV Internal/External
Wavelength Scales
Internal NUV Wavelength
Verification
NUV External Spectroscopic
Performance – Part 1
COS17
NUV External Spectroscopic
Performance – Part 2
COS18
NUV Flat Fields
3.1
NUV Sensitivity
3.7.5
COS20
NUV Structural and Thermal
Stability
3.7.6
COS21
NUV High S/N Verification
3.7.7
COS22
FUV Detector Door Open
COS23
FUV Detector Initial HV Turn
On
COS24
3.8
COS25
FUV Detector Functionality and
Operation
1.8
3.8
COS26
FUV Optics Alignment and
Focus
3.9
3.10
1.8
COS27
Internal FUV Wavelength
Measurement
FUV Target Acquisition
Algorithm Verification
3.8
3.11.1
1.8
FUV Internal/External
Wavelength Scales
1.2
1.8
3.12.1
COS30
Internal FUV Wavelength
Verification
1.2
3.12.1
COS31
FUV External Spectroscopic
Performance – Part 1
COS32
FUV External Spectroscopic
Performance – Part 2
COS33
FUV External Flat Fields
COS34
FUV Sensitivity
COS35
FUV Structural and Thermal
Stability
3.12.6
COS36
FUV High S/N Verification
3.12.7
1.8
3.13
2.2
COS29
3.7.1
3.7.2
3.13
3.7.2
3.7.3
3.7.4
2.3
FUV Detector Dark
COS28
1.8
2.2
2.1
1.2
1.7
1.8
3.1
1.8
Req
L10.4.2+
COS19
2.2
1.8
Title
1.8
3.13
3.12.2
3.12.3
3.12.4
1.2
2.1
3.12.2
3.13
3.12.5
76
COS Plan Overview
HST
MOSES
COS Activities / Orbit Allocation
Activity No.
COS01
Title
Instrument States; Data
Interface and Data
Transmission Verification
No. orbits No. orbits
external internal
0
0
Activity No.
Title
No. orbits No. orbits
external internal
COS22
FUV Detector Door Open
0
1
FUV Detector Initial HV Turn
On
0
6
FUV Detector Dark
0
10
FUV Detector Functionality and
Operation
FUV Optics Alignment and
Focus
Internal FUV Wavelength
Measurement
FUV Target Acquisition
Algorithm Verification
FUV Internal/External
Wavelength Scales
Internal FUV Wavelength
Verification
0
1
10
0
0
3
6
0
4
0
0
4
COS02
On-Board Memory Check
0
1
COS23
COS03
Science Data Buffer Check
0
7
COS24
3
10
COS25
COS04
NUV Detector Initial HV Turn
On & RampUp
COS05
NUV Detector Dark
0
0
COS06
NUV Detector Internal
Functionality and Operation
0
1
COS27
COS07
NUV Fold Test
0
5
1
0
COS28
NUV Optics Alignment and
Focus
Internal NUV Wavelength
Measurement
NUV Imaging Acquisition
Algorithm Verification
NUV Dispersed-light
Acquisition Algorithm
Verification
9
0
COS30
0
6
COS31
FUV External Spectroscopic
Performance – Part 1
8
0
3
0
COS32
FUV External Spectroscopic
Performance – Part 2
6
0
4
0
COS33
FUV External Flat Fields
COS34
FUV Sensitivity
0
0
0
NUV Imaging Performance
6
6
12
COS35
NUV Internal/External
Wavelength Scales
Internal NUV Wavelength
Verification
NUV External Spectroscopic
Performance – Part 1
NUV External Spectroscopic
Performance – Part 2
3
0
7
0
FUV Structural and Thermal
Stability
COS36
FUV High S/N Verification
0
10
6
0
9
0
8
0
0
15
6
12
36
0
0
0
COS08
COS09
COS10
COS11
COS12
COS13
COS14
COS15
COS16
COS17
COS to FGS Alignment (NUV)
COS18
NUV Flat Fields
COS19
NUV Sensitivity
COS20
NUV Structural and Thermal
Stability
COS21
NUV High S/N Verification
COS26
COS29
external
internal
NUV orbits
84
75
FUV orbits
61
25
Total Orbits
145
100
77
COS SMOV4 NUV Sequence
HST
HST release
Internal pressure
<20 micro-Torr
MAMA LV on
COS-01
Recovery from
SAFE
COS-06
NUV Internal
Functionality &
Operation
COS-02
Onboard
Memory Check
COS-03
Science Data
Buffer Check
COS-04
NUV Initial HV
Turn-on/Ramp-up
FUV SMOV
sequence
Rapid data
turnaround
required
COS-16
NUV Ext.
Spectr. Perf.
Part 1
Internal pressure
<10 micro-Torr
COS-07
NUV
Fold Test
COS-05
NUV
Dark Measure
Wavelength
Ranges OK
Enable NUV ERO
and Science
BEA Complete
COS-08
OTA to FGS
Alignment (NUV)
COS-10
Internal NUV
Wavelength Meas
Vis 2 – lamp 2
Update SIAF
Alignment
Not OK
COS-09
NUV Optical
Alignment /Focus
visit 1-3
COS-15
Internal NUV
Wavelength
Verify
COS-10
Internal NUV
Wavelength
Meas – Vis 1
Require
Wavelength
Scale Update
COS-17
NUV Ext.
Spectr. Perf.
Part 2
COS-19
NUV Spectr.
Sensitivty
Wavelength
Ranges
Not OK
Patchable Const. Update
MOSES
COS-21
NUV High S/N
Verification
COS-20
NUV Structural
& Thermal
Stability
COS-14
NUV Int/External
Wavelength Scales
Update SIAF
Special
Commanding
External Observations
COS-09
NUV Optical
Alignment vis 4-5
Real-time uplink;
Poss. update SIAF
May require wait
Alignment OK
10 October 2007
COS-11
NUV Imaging
Acq Verify
COS-12
NUV Dispersed
Acq Verify
COS-18
NUV
Flat Fields
COS-13
NUV Imaging
Performance
Do NOT
Require
Wavelength
Scale Update
78
COS SMOV4 FUV Sequence
Outgassing
Concern?
XDL at OPER
HST release
COS-01
Internal
Pressure
COS-02
COS-03
<100 microTorr
NUV
SMOV
sequence
COS-24
FUV
Dark Measure
COS-22
FUV Detector
Door Open
COS-09
NUV Optical
Alignment /Focus
COS-27
Internal FUV
Wavelength Meas
Vis 2 – lamp 2
COS-23
FUV Initial HV
Turn-on/Ramp-up
COS-26
FUV Optical
Alignment /Focus
visit 1
Real-time uplink
Special
Commanding
External Observations
COS-27
Internal FUV
Wavelength
Meas – Vis 1
Alignment OK
Rapid data
turnaround
required
COS-31
FUV Ext.
Spectr. Perf.
Part 1
Pressure Gauge OFF
Wavelength
Ranges OK
COS-30
Internal NUV
Wavelength
Verify
Wavelength
Ranges
Not OK
Patchable Const. Update
Update SIAF
May require wait
<10 microTorr
COS-25
FUV Internal
Functionality &
Operation
BEA Complete
Real-time
Commanding
Internal
Pressure
COS-29
FUV Int/External
Wavelength Scales
HST
Enable FUV ERO
and Science
COS-36
FUV High S/N
Verification
Require
Wavelength
Scale Update
MOSES
COS-32
FUV Ext.
Spectr. Perf.
Part 2
COS-33
FUV
Flat Fields
COS-34
FUV Spectr.
Sensitivty
COS-35
FUV Structural
& Thermal
Stability
COS-28
FUV Dispersed
Acq Verify
Does NOT Require
Wavelength Scale
Update
79
10 October 2007
Cosmic Origins Spectrograph
Engineering Activities
HST
MOSES
• COS01: COS Recover from SAFE
– Dependencies: AT/FT; HST release
• COS02: COS Onboard Memory Check
– Dependencies: COS01, MAMA LV on, XDL OPER
– Special Commanding required; 1 internal orbit
– Verify DCE, DIB copy, dump of CS memory
• COS03: COS Science Data Buffer Check
– Dependencies: COS02
– Special Commanding required; 7 internal orbits
– CS memory read/write, DIB tests in vicinity of SAA
80
Cosmic Origins Spectrograph
HST
NUV Detector Activities
MOSES
• COS04: Initial NUV HV Turn-on / Ramp-up
– Dependencies: COS03; P < 20 microTorr for 12 hours
– Ramp HV in 3 steps; 24-hour evaluation period between each
step; rapid data turnaround required
– Special and Real-time Commanding required; 3 internal orbits
over 48 hours
• COS05: COS NUV Dark Measurements
– Dependencies: no less than 2 days after COS04
– 10 internal orbits
– Verifies TIME-TAG operation; evaluate dark near SAA
81
Cosmic Origins Spectrograph
NUV Detector Activities
HST
MOSES
• COS06: NUV Internal Functionality/Operation
– Dependencies: no less than 2 days after COS04 and P < 10
microTorr (to operate lamps)
– Obtain TIME-TAG science exposures with both PtNe and D2; 1
internal orbit
• COS07: COS NUV Fold Test
– Dependencies: no less than 2 days after COS04 and P < 10
microTorr (to operate lamps)
– Special Commanding required; 1 internal orbit
– Diagnostic of MAMA performance; obtain count-rate as function
of fold or pulse size
82
Cosmic Origins Spectrograph
NUV Alignment Activities
HST
MOSES
• COS08: COS OTA to FGS Alignment (NUV)
– Dependencies: COS06; BEA complete
– Coarse focus and initial aperture location sweeps
– 5 external orbits; SIAF update follows (2w turnaround)
• COS09: COS NUV Optical Alignment/Focus
– Dependencies: COS08
– 9 orbits; 5 visits
– 3 epochs of fine-focus sweeps; each followed by real-time
uplinks (focus, astigmatism update: 2-3d) and SIAF update
(coma update: ~2w turnaround)
– 2 visits of PSF verification (real-time update may follow)
83
Cosmic Origins Spectrograph
HST
NUV Acquisition Activities
MOSES
• COS11: NUV Imaging Acquisition Verification
– Dependencies: COS09
– Verify ability of ACQ/IMAGE FSW to place an isolated point
source in center of aperture for PSA and BOA with MIRRORA
and MIRRORB; exercise target-centering options; for PSA
evaluate capability with nearby companion
– 3 external orbits; 3 visits
• COS12: NUV Dispersed-Light Acq Verification
– Dependencies: COS11
– Verify ability of ACQ/SEARCH, ACQ/PEAKXD, ACQ/PEAKD
FSW to place an isolated point source in center of PSA and BOA
using NUV dispersed light; exercise all centering options
– 4 external orbits; 3 visits
84
Cosmic Origins Spectrograph
NUV Image-related Activities
HST
MOSES
• COS13: NUV Imaging Performance Verification
– Dependencies: COS11
– Verify imaging mode for PSA and BOA; characterize PSF, plate
scale, imaging throughput for MIRRORA and MIRRORB; dense
grid patterns used for MIRRORA; MIRRORB at aperture-center
– 6 external orbits
• COS18: COS NUV Flat Fields
– Dependencies: COS09
– 36 internal orbits; 65 Ksec of data acquisition
– Use 3 λc with G185M; co-add data to yield flat sufficient to allow
flat fielding to a level of 30:1 per resolution element
85
Cosmic Origins Spectrograph
NUV Wavelength Activities
HST
MOSES
• COS10: NUV Internal Wavelength Measurement
–
–
–
–
Dependencies: COS09; visit 2 preferred before COS15
Visit 1: initial wavecal for default FP-POS of all λc
Visit 2: PtNe lamp 2 verification at one λc and FP-POS
6 internal orbits
• COS14: NUV Internal/External Wavelength Scales
– Dependencies: COS10 visit 1
– 7 external orbits, CVZ preferred
– Utilize TIME-TAG (FLASH=YES) observations of a radial velocity
standard at all λc to obtain zero-point offsets for wavelength scales
of all setups; adjust nominal ranges to desired values and update
corresponding focus settings via real-time uplink of patchable
constants
86
Cosmic Origins Spectrograph
HST
NUV Wavelength Activities
MOSES
• COS15: COS NUV Internal Wavelength Verification
– Dependencies: COS14 and uplink of zero-pt and focus real-time
patchable constant update
– Obtain wavecal at all FP-POS for all λc to verify wavelength
ranges and establish dispersion relations; evaluate drifts
– 10 internal orbits
– Subsequent to this verification, ERO and science operations can
commence
87
Cosmic Origins Spectrograph
NUV Characterization
HST
MOSES
• COS16: NUV External Spectroscopic Performance – Part 1
• COS17: NUV External Spectroscopic Performance – Part 2
– Dependencies: COS15 verification
– Part 1 characterizes absorption line spectral resolution at aperture
center and at typical offsets from center; Part 2 characterizes
spectrum and spatial resolution for each NUV grating in crossdispersion direction with PSA and on-center with BOA; most
exposures with FLASH=YES, also verify FLASH=NO and Doppler
correction for ACCUM
– 17 external orbits
• COS20: COS NUV Structural and Thermal Stability
– Dependencies: COS15 verification
– 6 external orbits; CVZ preferred
– Observe non-variable target with one λc and TAGFLASH; assess 88
positional and photometric stability, OSM drift, TAGFLASH utility
Cosmic Origins Spectrograph
HST
NUV Characterization
MOSES
• COS19: NUV Spectroscopic Sensitivity
– Dependencies: COS15 verification
– Confirm spectroscopic sensitivity versus wavelength over the
entire observable spectrum for all NUV gratings and λc settings;
observe HST flux standard stars.
– 15 external orbits
• COS21: COS NUV High S/N Verification
– Dependencies: COS15 verification
– 12 external orbits
– Collect TIME-TAG data for each NUV grating at multiple FPPOS to verify that spectra with S/N>30 can be obtained with
normal data acquisition and reduction techniques.
89
Cosmic Origins Spectrograph
HST
FUV Detector Activities
MOSES
• COS22: COS FUV Detector Door Open
– Dependencies: COS03; P < 100 microTorr for 12 hours;
– Real-time activity; open door so detector can begin to outgas
and light can reach microchannel plates
• COS23: Initial FUV HV Turn-on / Ramp-up
– Dependencies: COS22; P < 10 microTorr for 12 hours
– Ramp HV in multiple sequences; 24-hour evaluation period
between each sequence; rapid data turnaround required
– Special and Real-time Commanding required; 6 internal orbits –
one per day over six days
90
Cosmic Origins Spectrograph
FUV Detector Activities
HST
MOSES
• COS24: COS FUV Dark Measurements
– Dependencies: not less than 2 days after COS23; internal
pressure gauge OFF for this and all subsequent observations
– 10 internal orbits
– Verifies TIME-TAG operation for FUV; evaluate darks near SAA
• COS25: FUV Internal Functionality/Operation
– Dependencies: not less than 2 days after COS23; internal
pressure gauge OFF for this and all subsequent observations
– Obtain TIME-TAG science exposures with both PtNe and D2; 1
internal orbit
91
Cosmic Origins Spectrograph
FUV Alignment Activities
HST
MOSES
• COS26: COS FUV Optical Alignment/Focus
– Dependencies: COS09 and COS25
– 12 external orbits; 3 visits
– 3 sets of fine-focus sweep spectra – one set per grating – with
sharp-lined target; observations require high S/N and will be
taken with TIME-TAG FLASH=YES
– Update derived focus setting for each grating via real-time uplink
of patchable constants (2-3d turnaround)
92
Cosmic Origins Spectrograph
FUV Acquisition Activities
HST
MOSES
• COS28: FUV Dispersed-Light Acq Verification
– Dependencies: COS26
– Verify ability of ACQ/SEARCH, ACQ/PEAKXD, ACQ/PEAKD
FSW to place an isolated point source in center of PSA and BOA
using FUV dispersed light; exercise all centering options;
evaluate for all grating and λc combinations that may be affected
by airglow for which subarrays are utilized in the FSW
– Also verifies routine FUV detector subarray readout
– 6 external orbits; 2 visits
93
Cosmic Origins Spectrograph
FUV Wavelength Activities
HST
MOSES
• COS27: FUV Internal Wavelength Measurement
–
–
–
–
Dependencies: COS26; visit 2 preferred before COS30
Visit 1: initial wavecal for default FP-POS of all λc
Visit 2: PtNe lamp 2 verification at one λc and FP-POS
3 internal orbits
• COS29: FUV Internal/External Wavelength Scales
– Dependencies: COS27 visit 1
– 4 external orbits, CVZ preferred
– Utilize TIME-TAG (FLASH=YES) observations of a radial velocity
standard at all λc to obtain zero-point offsets for wavelength scales
of all setups; adjust nominal ranges to desired values and update
corresponding focus settings via real-time uplink of patchable
constants
94
Cosmic Origins Spectrograph
FUV Wavelength Activities
HST
MOSES
• COS30: COS FUV Internal Wavelength Verification
– Dependencies: COS29 and uplink of zero-pt and focus real-time
patchable constant update
– Obtain wavecal at all FP-POS for all λc to verify wavelength
ranges and establish dispersion relations; evaluate drifts
– 4 internal orbits
– Subsequent to this verification, ERO and science operations can
commence
95
Cosmic Origins Spectrograph
FUV Characterization
HST
MOSES
• COS31: FUV External Spectroscopic Performance – Part 1
• COS32: FUV External Spectroscopic Performance – Part 1
– Dependencies: COS30 verification
– Part 1 characterizes absorption line spectral resolution at aperture
center and at typical offsets from center; Part 2 characterizes
spectrum and spatial resolution for each FUV grating in crossdispersion direction with PSA and on-center with BOA; most
exposures with FLASH=YES, also verify FLASH=NO and Doppler
correction for ACCUM
– 14 external orbits
• COS35: COS NUV Structural and Thermal Stability
– Dependencies: COS30 verification
– 3 external orbits; CVZ preferred
– Observe non-variable target with one λc and TAGFLASH; assess 96
positional and photometric stability, OSM drift, TAGFLASH utility
Cosmic Origins Spectrograph
FUV Characterization
HST
MOSES
• COS33: COS FUV External Flat Fields
– Dependencies: COS30 verification
– Obtain TIME-TAG FLASH=YES spectra at ~6 positions along crossdispersion direction with multiple FP-POS; choose positions to
maximize coverage in cross-dispersion directions where science
spectra are recorded. Co-add to produce S/N=30 per resolution
element flat field.
– 6 external orbits
97
Cosmic Origins Spectrograph
FUV Characterization
HST
MOSES
• COS34: FUV Spectroscopic Sensitivity
– Dependencies: COS30 verification
– Confirm spectroscopic sensitivity versus wavelength over the entire
observable spectrum for all FUV gratings and λc settings; observe
HST flux standard stars.
– 12 external orbits
• COS36: COS FUV High S/N Verification
– Dependencies: COS30 verification
– 6 external orbits
– Collect TIME-TAG data for each FUV grating at multiple FP-POS to
verify that spectra with S/N>30 can be obtained with normal data
acquisition and reduction techniques.
98
HST
MOSES
ADVANCED CAMERA FOR SURVEYS
(ACS)
SMOV4 PLAN
Kailash C. Sahu
STScI
99
HST
Introduction/Overview
•
MOSES
Basic Assumptions
– We assume a fully repaired ACS, where all the 3 ACS channels (WFC,
HRC and SBC) are functioning
– However, proposals are separate for different detectors so that they can
be easily implemented depending on which channels are available after
SMOV
•
Approach
– Success Oriented Approach in the current timeline
– Contingencies are not shown in the timeline, but preparatory work is
being done as appropriate
– Include the minimum set required for starting GO science. Where
possible, do the tests as part of the regular calibration procedure
•
Proposed changes since the last Mar. 21 RR
– Focus check will not be done using SBC since SBC is not ideal for this
activity. More details in presentation by Ed Nelan on OTA/FGS.
100
HST
ACS Activity Summary
MOSES
101
HST
ACS Re-Commissioning Sequence
MOSES
102
HST
MOSES
Initial Start-up and Engineering Checks
•
•
Test and verify ACS dump of CS memory (ACS01)
Check science data buffer (ACS03)
Initial CCD Activities
• Hot pixel annealing (ACS04, L10.4.3.1.1)
– Similar to the monthly annealing process but will last for 12 hours
– To assess the effectiveness of the annealing process, bias frames and
darks will be taken before and after for both WFC and HRC
• Determination of the CCD Temperature Set Point (ACS05, L10.4.3.1.2)
– Verify the stability of previously set temperatures for WFC and HRC over
24 hrs (in the unlikely case of instability, activate contingency part)
21 Mar. 2007
HST
Initial CCD Activities (contd.)
•
CCD functional test (ACS06, L.10.4.3.1.3)
- Take a series of bias, dark and flat field frames for all gains
and readout modes
- CTE will be measured as a function of signal level
•
CCD cross-talk check (ACS08, L10.4.3.1.3)
- Check cross talk between the four quadrants of WFC CCD,
using a bright external target since cross talk can affect most
science observations. This would require 2 orbits.
21 Mar. 2007
MOSES
HST
SBC Activities
MOSES
•
SBC turn-on and anomalous recovery test (ACS07, L.10.4.3.1.3)
- Perform initial turn-on of the ACS MAMA detector, and recovery test
after an anomalous shutdown, as might result from a bright object
violation or hardware problem. This is a standard four stage test, with
gradual increase of the voltage.
•
UV contamination check and monitoring (ACS09, L.10.4.3.1.4)
– First part (checking) will be carried out within BEA but closer to
expected end of BEA, using SBC. All filters will be checked against
prior observations. This will help determine end of BEA. Depending on
target suitability/availability, UV contamination check may be done by
using the small amount of time available to observe non-BEA targets
during BEA. Second (monitoring) part +1 and +3 weeks after end of
BEA. •
Dark Current Measurement (ACS10, L.10.4.3.1.3)
– Measured over a period of 6 hrs to quantify known steady increase
with time
105
Image Quality and Alignment
HST
MOSES
•
Image Quality (CCD) and PSF Measurement (ACS17, L.10.4.3.3.1)
– A series of images will be obtained to evaluate to measure point source
image quality for WFC and HRC, using NGC 188 as the likely target.
•
ACS to FGS Alignment (ACS12, L.10.4.3.2.1)
– Same observations taken for ACS17 will be used to map the ACS
detector coordinate frame to the FGS frame
•
Coarse and fine corrector alignments are contingency activities (ACS13,14;
L.10.4.3.3.2)
•
SBC PSF Measurement (ACS16, L.10.4.3.3.1)
– A series of images to evaluate the point source image quality over the
field of view of the ACS SBC channel, using NGC 6681 (18.7 h, -32 deg)
as the target.
21 Mar. 2007
HST
CCD verification - cont
MOSES
•
UV sensitivity, geometric distortion and flat field verifications (ACS20,
L.10.4.3.1.4/4.2/4.3)
– The performance of SBC and HRC in the UV will be checked using
standard targets, and pixel-to-pixel sensitivities will be measured using
flat fields
•
CCD sensitivity, geometric distortion and flat field stability (ACS11,
L.10.4.3.4.2/4.3)
– The performance of WFC and HRC in the optical will be checked using
the standard target 47 Tuc
– Flat field stability will be checked using tungsten lamps and multiple
dithered pointings of 47 Tuc
21 Mar. 2007
HST
HRC Coronagraph
MOSES
•
Coronagraphic Spot Location (ACS15, L.10.4.3.2.2)
– This activity will be achieved using four images of the Earth. This activity
can be done after the end of the BEA.
•
Coronagraphic Acquisition (ACS18, L.10.4.3.3.3)
– Acquisition of a point source on to the coronagraphic spots will be
tested using a bright isolated star
108
HST
Final Remarks
MOSES
•
Total Orbits have been reduced from 158 to 105. Total external orbits have
been reduced to 30 (excluding contingencies).
•
Cycle 17 calibration will overlap with SMOV activity
•
Cycle 17 will contain a new CCD optimization program that will be executed
promptly if the noise characteristics are not satisfactory
109
HST
MOSES
Space Telescope Imaging
Spectrograph
SMOV4 PLAN
110
HST
STIS SMOV4 Overview
MOSES
• Assumes repair success verified by AT & FT
• Success oriented schedule
– Unless there is a safety issue, don’t wait to analyze results
before proceeding to subsequent activity.
• Baseline plan assumes alignment intact
– Assume HST Focus is good
– Assume STIS-to-FGS alignment good enough for ACQs
• Will verify early and do final measurement later
– Focus and tip-tilt of corrector should be OK
• Will verify early.
• If a corrector adjustment is needed, this would require repeating or
deferring most subsequent external observations, and seriously
delay the latter half of the STIS SMOV schedule
111
HST
STIS SMOV4 Overview
MOSES
• Do as much as possible during BEA
– Provide multiple targets for several tests to cover BEA dates
• Keep channel verification (CCD, NUV-MAMA, FUVMAMA) independent where practical.
• Some SMOV activities will be implemented as part of
Cycle 17 calibration programs.
– Need to be sequenced during SMOV, but usually identical to
routine calibrations. Reduces duplication of work.
– Identified in this presentation by blue text.
112
HST
STIS SMOV4 Overview
MOSES
• Requirements compliance
– STIS optical alignment requirements 10.4.5.3.1 and 10.4.5.3.4
state that the tests specified in those requirements are “…
dependant on the setting of the HST secondary mirror position,
which must first have been set to nominal focus”.
– The lack of the ACS CCDs prior to SM4 leave no direct way to compare
focus just before SM4 with the focus during the early SMOV period.
– Unless there is clear evidence to the contrary, we will presume that the
HST secondary is still at the nominal focus it was set at prior to SM4.
– MAMA HV recovery procedures have been substantially revised,
(working group led by O. Lupie)
• Suggest that 10.4.5.1.11 be reworded to reference new procedure.
– Otherwise, the STIS SMOV activities are designed to meet all
STIS SMOV requirements.
113
HST
STIS SMOV4 Activities
Activity
Title
Req. # 10.4.5.
STIS-01
STIS-02
STIS-03
STIS-04
STIS-05
STIS-06
STIS-07
STIS-08
STIS-09
STIS-10
STIS-11
STIS-12
STIS-13
STIS-14
STIS-15
STIS-16
STIS-17
STIS-18
STIS-19
STIS-20
STIS-21
STIS-22
STIS-23
STIS-24
STIS-25
STIS-26
Modes and Data Interface Checks
Memory Load and Dump
Science Data Buffer Check with Self-Test
Mechanism Mini-Functional
CCD Anneal
CCD Functional
CCD Bias and Dark Monitor
Aperture Wheel and Lamp Functional Tests
STIS to FGS Alignment
CCD Spectral Format Verification
External Focus Check
Corrector and Focus Alignment
CCD External Spectroscopic Image Quality & ACQ Tests
CCD CTI Check
CCD Spectroscopic Throughputs
CCD Image and Pointing Stability
FUV MAMA HV Recovery
NUV MAMA HV Recovery
FUV MAMA Dark Measure
NUV Dark Monitor
FUV MAMA Optical Format Verification
NUV MAMA Optical Format Verification
FUV MAMA External Spectroscopic Image Quality
NUV MAMA External Spectroscopic Image Quality
MAMA Spectroscopic Throughputs
MAMA Image Stability
1.1, 1.2, 1.3, 1.11
1.4
1.5
1.6
1.8, 1.9
1.9, 1.10
4.1
1.7, 3.2, 3.3
2.1
3.3
3.1
3.1
2.2, 3.4
4.2
4.3
3.5
1.11
1.11
4.1
4.1
3.3
3.3
3.4
3.4
4.3
3.5
TOTAL
External
orbits
MOSES
Internal time
(minutes)
20
60
60
250 + 15h wait
360
90/day
133
2
30
3
16
2
30
3
2
350
366
300
120/wk
60
60
2
2
4
192
20+16
2271 +
~750/wk
114
STIS Re-commissioning Sequence
STIS Recovery
LVPSs & TEC
on
STIS-02
Memory Load
And Dump
8/18
8/16-8/18
STIS-05
CCD Anneal
Repeat 28d
STIS-06
CCD
Functional
8/18
STIS-19
FUV MAMA
Dark Measure
Visits 1-5
STIS-10
CCD Optical
Format Verify
8/24
STIS-18
NUV MAMA
HV Recovery
Visits 2-4
8/31-9/05
8/24-8/29
STIS-21
FUV Optical
Format Verify
8/21
Start STIS-20
NUV MAMA
Dark Monitor
Start 9/05…
STIS-22
NUV Optical
Format Verify
9/06
8/31
8/21
STIS-09
STIS to FGS
Alignment 1
1 orbit
8/21-8/22
STIS-12
Contingency
Corrector &
Focus Adjust
STIS-13
CCD Spectro
Image Qual
& ACQ tests
2 orbits
Rewrite schedule
Calibration
STIS-17
FUV MAMA
HV Recovery
Visits 2-4
8/29-8/30
Start 8/20…
MOSES
STIS-18
NUV MAMA
Visit 1
Sig. proc. check
8/20
8/19
STIS-08
Aper. Wheel
& Lamp tests
8/21
Approx. dates specified
assume 8/15 release.
STIS-17
FUV MAMA
Visit 1
Sig. proc. check
STIS-04
Mechanism
Functional
Start STIS-07
CCD Dark
Bias Monitor
8/20-8/21
8/19-8/20
STIS-14
CCD CTI
Measurement
STIS-03
Science Data
Buffer Check
HST
STIS-11
STIS External
Focus Check
3 orbits
8/22
STIS-19
FUV MAMA
Dark Measure
Visits 6-10
9/30
External Observations
Contingency we hope not to need
5 days each including waits for data
analysis
STIS-09
STIS to FGS
Alignment 2
2 orbits
9/05-9/06
8/22
STIS-15
CCD Spectro
Throughputs
3 orbits
9/06-9/07
STIS-16
CCD Stability
STIS-23
FUV Spectro.
Image Quality
2 orbits
8/31
STIS-25
MAMA Spectro
Throughputs
4 orbits
9/07-9/08
STIS-24
NUV Spectro.
Image Quality
2 orbits
9/07
STIS-26
MAMA Stability
After BEA
2 orbits
9/05-9/06
9/08-9/09
115
STIS Engineering
Activities
HST
MOSES
Initial Engineering Activities start after STIS Recovery.
• STIS01 – Data Modes and Interfaces
– Requirements L.10.4.5.1.1, L.10.4.5.1.2, L10.4.5.1.3,
L10.4.5.1.11
– Verify modes and data interfaces during routine ops.
– No associated proposal - goals satisfied during other activities.
• STIS02 - Memory Load and Dump
– Requirement 10.4.5.1.4
– Dump and verify various sections of Control Section (CS)
Memory (including EEPROM, PROM, EDAC RAM, Buffer RAM,
MIE RAM) in OPERATE mode.
• STIS03 - Science Data Buffer Check with Self-Test.
– Requirement 10.4.5.1.5
– test science buffer across SAA
– CS ‘walking ones’ self test
116
STIS Engineering
Activities - Cont.
HST
MOSES
• STIS04 - Mechanism Mini-Functional
– Requirement: L10.4.5.1.6
– Execute after STIS03
– Move all STIS mechanisms (except focus/ corrector) through full
range needed for normal operations.
– Verify functioning and redistribute lubrication.
– Engineering telemetry used to verify motions.
• STIS05 - CCD Anneal
–
–
–
–
Requirement: L10.4.5.1.8, L.10.4.5.1.9 (CCD cooling)
Execute after STIS04 Mechanism Functional
Normal CCD anneal at +5 C, but at -5 C while safed.
Perform usual monthly anneal
• Includes usual pre-/post- anneal darks, biases, and flats
• Implement as part of Cycle 17 calibration program
117
STIS Engineering
Activities
HST
MOSES
• STIS06 - CCD Functional
– Requirements - L.10.4.5.1.9 (CCD cooling); L.10.4.5.1.10
– Execute after initial iteration of STIS06 CCD Anneal
– Measure baseline CCD performance, using dark, bias, and flat
exposures with different gains, amps, sub-arrays, and binning.
– More extensive than usual annual calibration program
• STIS08 - Aperture Wheel & Lamp Tests
–
–
–
–
–
Requirements - L.10.4.5…
Execute after STIS06, CCD Functional Test
Verify aperture wheel encoder positions … 3.2
Verify tungsten and PtCr/Ne lamp functioning … 1.7
Verify optical path & image locations for CCD imaging … 3.3
118
HST
MAMA HV recovery
•
•
MOSES
STIS17 FUV MAMA HV Recovery
STIS18 NUV MAMA HV Recovery
–
–
–
Requirement: 10.4.5.1.11
Careful recovery in case Cesium migration into MCP pores
during safing leads to large temporary increase in dark current.
Done in stages, one stage of stages 2-4 ~ every other day
1. Signal processing check (LV only) - any time after STIS04
2. 1st HV ramp-up to -1500V
•
4+ days after release; 3+ days after MAMA LVPSs on
3. 2nd HV ramp-up to -1950V/-1750V (FUV/NUV)
•
Follow with darks and fold test
4. 3rd HV ramp to full voltage
•
–
Follow with darks and fold test
NUV HV (steps 2-4) to follow full FUV recovery.
119
HST
STIS Target ACQ Activities
MOSES
• STIS09 - STIS to FGS Alignment
– Requirement: L10.4.5.2.1
• Accuracy req. 1” in V2-V3, 10’ in aperture rotation angle
–
–
–
–
Execute after CCD functional test (STIS06).
First external target to be observed with STIS.
1 orbit per visit, dither target to various positions in V2 & V3
Use targets and guide stars with good astrometry
• USNO CCD Astrograph Catalog 2 (UCAC2) or better.
– Done in two visits
• Initial visit done during BEA to verify alignment good enough for
SMOV, (i.e., ACQs will work). Need targets to cover all times.
• Second visit done using astrometric field with multiple stars to verify
rotation as well as offset, and provide best possible accuracy (0.3”).
– Assume that SMOV can proceed without waiting for any SIAF,
PDB, or other table updates. These will be done later.
120
HST
STIS Alignment Activities
MOSES
• STIS11 - External Focus Check
– 3 orbits (but may reduce to 1 or 2 orbits)
– After STIS09 (STIS to FGS Alignment)
– Requirement 10.4.5.3.1
• NUV throughput of 0.1x0.09 should ≥ 93% of expected
• Significant problem with focus would trigger STIS12
– Measure NUV PSF to verify STIS focus/alignment
• G230LB peakup on hot star with 0.1X0.09 aperture
– Similar to standard calibration focus monitor
• Relative throughputs of 0.1x0.09 & 52X2 apertures
• Narrow-band OII images (3740 Å)
– Use phase retrieval techniques
– Need sufficient targets to cover BEA period
• Could use WD targets defined for SMOV3B, but fainter of these
would require multiple orbits to do this test
• In process of selecting suitable brighter targets
121
HST
STIS Alignment Activities
MOSES
• STIS12 - Corrector and Focus Alignment
– Requirement: 10.4.5.3.1
– This contingency program will only be executed if
there is a problem with the focus
• Not included in baseline SMOV plan
• Corrector mechanism will only be moved if necessary
• Need to decide whether we want some visits to be in BEA
– Repeats procedure used during SMOV2
• Step tip/tilt and focus values
• Phase retrieval of OII images for coarse alignment
• Maximize throughput of 0.1x0.09 with G230LB during fine
alignment.
122
HST
STIS Alignment Activities
MOSES
• STIS10 - CCD Spectral Format Verification
• STIS21 - FUV MAMA Optical Format Verification
• STIS22 - NUV MAMA Optical Format Verification
–
–
–
–
Requirement: 10.4.5.3.3
Execute STIS10 after aperture wheel test (STIS08)
Execute STIS21/22 after MAMA Recovery
Take internal LINE or HITM1 PtCr/Ne lamp spectra
with all STIS spectral modes.
– Only one CENWAVE for each optical element.
– Verify spectra fall at expected locations on detector
• select settings to facilitate comparisons with previous data
– Verifies internal optical paths for all spectral modes
123
HST
STIS Alignment Activities
MOSES
Requirement 10.4.5.3.4 - External Image Quality
• STIS13 CCD Spectroscopic Quality & ACQ Tests
• STIS23 FUV MAMA Spectroscopic Image Quality
• STIS24 NUV MAMA Spectroscopic Image Quality
– 2 orbits per detector (external targets)
– Execute after corresponding format verification (STIS10,21,22)
and focus verification (STIS11).
– Check spectroscopic PSF for each detector at several locations
along long slit (more extensive than STIS11)
– Step targets perpendicular to narrow aperture at these locations
– CCD activity includes target ACQs and ACQ/Peak exposures at
central, E1, and D1 locations, -> ACQ requirement 10.4.5.2.2
– For FUV and CCD need sufficient BEA targets to cover all
possible dates; NUV activity expected to occur after BEA.
124
HST
STIS Calibration Activities
MOSES
Requirement L.10.4.5.4.1 (dark measurements)
Start after each channel recovered (STIS06,17,18 respectively)
• STIS07 - CCD Bias/Dark Monitor
– Routine daily darks and biases
– Implement as parts of cycle 17 cal programs.
•
STIS19 - FUV MAMA Dark Measure
– FUV dark current increases with time after daily HV turn-on
– Measure FUV dark over 5 orbit block during SAA free period
– Also depends on T, so do once right after HV recovery and later after all
heat sources to aft-shroud (e.g. COS) in operation.
•
STIS20 - NUV MAMA Dark Monitor
– NUV MAMA dark current mostly phosphorescent window glow
• Expected to be high after SM4, but decline over a few weeks
– Normal cal program does 2 darks per week
• Increase to 4 darks per week until window glow decays
– Implement as part of cycle 17 cal program.
125
HST
STIS Calibration Activities
•
MOSES
STIS14 - CCD CTI Check
–
–
–
–
Requirement 10.4.5.4.2
After CCD Functional (STIS06)
Internal tungsten lamp exposures using 0.05X31NDA slit
Read out from alternate amps to map CTI as a function of position and
exposure level
– Implement as part of Cycle 17 “Internal Sparse Field” Calibration
Program
Requirement 10.4.5.4.3 - Flux Calibration
• STIS15 - CCD Spectroscopic Throughputs
• STIS25 - MAMA Spectroscopic Throughputs
–
–
–
–
4 orbits for MAMA; 3 orbits for CCD; after BEA end.
Prefer standard high-latitude sensitivity monitor targets
Include all STIS gratings; may exclude NUV PRISM
Implement as parts of Cycle 17 calibration programs
126
HST
STIS Calibration Activities
MOSES
Requirement 10.4.5.3.5 - Image Stability
• STIS16 - CCD Image and Pointing Stability
– Two orbits immediately following an attitude change that is
expected to change heating of STIS bench
– Perform after BEA & after image quality checks (STIS13)
– Check relative stability of detector, aperture plane and sky.
– Interleave lamp exposures of standard aperture with external
exposures of star field
• STIS26 - MAMA Image Stability
– Two orbits per detector, immediately following an attitude
change that is expected to change heating of STIS bench
• May be done in parallel with another instrument’s stability test
– After MAMA External Image Quality checks (STIS23,24)
– Internal only. Interleave echelle LINE lamp exposures with darks
127
to minimize lamp useage.
HST
MOSES
SMOV4 NICMOS
128
HST
NICMOS
Approach
MOSES
SMOV4 PLAN
October 12 2007
–
Re-use as much as possible the NICMOS SMOV3b
requirements/proposals
–
Perform NICMOS SMOV4 to verify operation and ascertain
basic performance of the instrument
–
Move some SMOV3b verification requirements to regular
(extended) calibration programs to follow immediately after
SMOV4
–
NCS off–time minimized in order to minimize dewar re–
cooling
NICMOS SMOV4 activities partially based on recommendations from the
NICMOS group following the NCS/NICMOS safing in August2003 and
January 2007. Potential problems associated with the thermal cycling include
mechanical and optical misalignments and increased particulate matter (‘Grot’).
129
HST
NICMOS
Approach (cont’d)
MOSES
SMOV4 PLAN
October 12 2007
–
Estimated dewar temperature (measured at the NIC1
mounting cup) with NCS off and NICMOS in safe mode:
T = 176[1 - exp(-t/183)] + 80 K (t in hours)
–
Warm–up rates varies from event to event (Jan 2000/
Aug 2003/Jan 2007)
–
NCS off for 9 days ––> detector warm–up ∆T~120K. Final
temperature: ~200K unless NICMOS powered off (in which
case the temperature would be higher, possibly ~280K)
–
Cool–down rate uncertain, ~14 days is reasonable based on
previous safing events
130
HST
NICMOS
MOSES
Summary of Activities
NIC01 Dewar cool–down
NIC02 Activation Test
NIC03 DC Transfer Test*
NIC04 Filter Wheel Test*
NIC05 Focus Test*
NIC06 FOM Test
NIC07 Aperture Location
NIC08 Optical Plate Scale
NIC09 Geometric Stability
NIC10 Mode2 Coronagraphic Acquisition
NIC11 Coronagraphic Focus*
NIC12 Coronagraphic Performance
NIC13 Thermal Characterization
NIC14 Detector Read Noise/Dark Current
*
BEA period
Coronagraphy
Pure parallel
= Special Commanding
131
HST
NICMOS
MOSES
NIC01
NIC02
NIC03
BEA END
Basic Timeline
NIC04
NIC05
NIC06
NIC07
NICMOS Science Enabled
NIC13
NIC08
NIC09
NIC10
NIC11
NIC12
Coronagraphy Enabled
NIC14
132
HST
NICMOS
MOSES
Detailed Timeline
133
HST
NICMOS
MOSES
Detailed Timeline
134
HST
NICMOS
MOSES
Activities not included in the SMOV4
–
All photometric calibrations
–
All grism calibrations
–
Test of the Cold Mask Offset
To be done as part of the regular Cycle 17
calibration program. Some of these activities
will be required to schedule soon after
SMOV4
135
HST
NICMOS
MOSES
Activities
NIC01 NICMOS Dewar Cool–Down
NIC02 NICMOS Activation Test
Configure the NCS to re–cool the NICMOS dewar
and detectors. The goal is to reach the nominal
detector temperature less than or equal to 77.15K
by maintaining the Neon inlet- and outlettemperatures at a desired set-point. NICMOS will
be off during the re-cooling. The NICMOS
temperature will be characterized indirectly
through the NCS control-law. The stability
requirement will be assessed through temperature
monitoring during SMOV4.
Verify 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, SAAOPER, OPERATE and OBSERVE)
Estimated time: 2 weeks
Science bits to SSR: 0
Estimated time: 1 internal orbit
Science bits to SSR:
Comments: NCS should be turned on as early as
possible to minimize the warm-up.
Comments: Can be done in BEA
SMOV Requirements: L10.4.4.5.1, L10.4.4.5.3
SMOV Requirements: L.10.4.4.1.1
136
HST
NICMOS
MOSES
Activities
NIC03 NICMOS DC Transfer
Function Test
NIC04 NICMOS Filter Wheel Test
Verify the basic operating characteristics of the
detectors through a series of multiple read-outs as
a function of bias voltage. This activity checks the
basic relation between the signal (in the dark
environment) and counts out in instrumental units
relative to a level set by the reference voltages.
Verify the mechanical integrity of the filter wheels,
their operability and electro-mechanical
calibration. This test is designed to obviate
concerns of possible deformation or breakage of
filter wheel “soda-straw” shafts due to excessive
rotational torque and/or bending motions that may
be imparted due to thermal cycling of the
NICMOS dewar. Analog and digital data are
sampled while each filter wheel is moved one slot
and back. Subsequent moves samples all filter
positions while taking lamp on/off exposures.
Estimated time: Internal orbits 4
Science bits to SSR: 375Mb
Comments: Special Commanding. Requires 2
orbits, with 2 spare orbits requested to allow for
potential bias adjustment and subsequent check
SMOV Requirements: L10.4.4.1.3
Estimated time: 6 internal orbit
Science bits to SSR: 940Mb
Comments: Can be done in BEA. Same program
executed in Feb 2007.
SMOV Requirements: L.10.4.4.1.2
137
HST
NICMOS
MOSES
Activities
NIC05 NICMOS Focus and PAM Grid
Tilt Test
NIC06 NICMOS FOM Functional
Test
Determine the best focus for all three cameras
through a series of iterative adjustments of the
PAM. The optimum PAM tilt will be derived after
the best focus is determined. The PAM position
and tilt may need to be updated.
Verify the basic mechanical operating
characteristics of the FOM by observing a
standard star in different locations on the NIC3
detector using the FOM to offset the star. A single
filter (F166N) will be used. A set of 3 additional
FOM positions will be obtained with the F222M
filter to test for vignetting.
Estimated time: External orbits 17
Science bits to SSR: 838Mb
Estimated time: External orbit 1
Science bits to SSR: 110Mb
Comments: Special Commanding. Based on
regular focus monitoring program. Outside BEA
period.
Comments: After NIC05 Focus and PAM Grid Tilt
Test
SMOV Requirements: L10.4.4.3.2
SMOV Requirements: L.10.4.4.1.2
138
HST
NICMOS
MOSES
Activities
NIC07 NICMOS Aperture Locations
NIC08 NICMOS Optical Plate Scale
Determine the location of each NICMOS camera
aperture with respect to the FGS reference
frames. Observations of 3 stars in a standard
astrometric field will be obtained. A series at offset
field pointings will be taken to determine the
location of the NICMOS apertures and to measure
the rotation angle of the apertures.
Measure the plate scale, field rotation and field
distortion for each NICMOS camera. The
intercamera astrometric solution will also be
obtained. A standard astrometric field will be
observed with a single filter (F160W). Each
camera will take 5 exposures, covering the 4
quadrants and the center position with the same
group of stars.
Estimated time: External orbits 6
Science bits to SSR: 1512Mb
Estimated time: External orbit 4
Science bits to SSR: 110Mb
Comments: May need SIAF update.
Comments: After NIC07
SMOV Requirements: L.10.4.4.2.1
SMOV Requirements: L.10.4.4.3.1
139
HST
NICMOS
MOSES
Activities
NIC09 NICMOS Geometric Stability
The geometric stability will be characterized by
measuring the lateral motion of the image in the
NIC2 focal plane. Exposure of a star field will be
obtained on a regular interval and the location of
each star will be measured as a function of time.
The geometric stability can be determined by
repeating the Optical Plate Scale test two
additional times during the SMOV using the same
target but only the NIC2 camera.
NIC10 NICMOS Mode-2
Coronagraphic Target Acquisition
Test
The mode-2 coronagraphic target acquisition will
be characterized and measured. Coronagraphic
observations are sensitive to small centering
errors and needs to be re-assessed following SM4
and re-cooling. The test will be done on 2 bright
stars of different characteristics (brightness and
environment). The test will be done in the domain
of saturation and under-exposure as well as for
optimally exposed targets.
Estimated time: External orbits 2
Science bits to SSR: 126Mb
Estimated time: External orbit 4
Science bits to SSR: 900Mb
Comments: Observations separated by ~10 days
Comments:
SMOV Requirements: L.10.4.4.4.2
SMOV Requirements: L.10.4.4.2.2
140
HST
NICMOS
MOSES
Activities
NIC11 NICMOS Optimum
Coronagraphic Focus Determination
NIC12 NICMOS Coronagraphic
Performance Assessment
Determine the optimum PAM position that
maximizes the coronagraphic image/background
contrast ratio. The coronagraphic hole is situated
at the f/24 focus and the detector at the re-imaged
f/45 focus. Due to the displacement of the optical
bench in the NICMOS dewar, these two foci are
no longer confocal. The PAM position and tilt can
be modified to optimize the focus for the
coronagraphic hole simultaneously with the
imaging.
This test defines a coherent program designed to
quantitatively measure and map out the diffractive
and scattered energy rejection of occulted targets.
The performance levels of the system will be
assessed while exploring the observational
parameter spaces and execution strategies.
Estimated time: External orbits 10
Science bits to SSR: 1779Mb
Estimated time: External orbit 6
Science bits to SSR: 1696Mb
Comments: If necessary the optimal parameters
will be updated in the FSW.
Comments:
SMOV Requirements: L.10.4.4.3.3
SMOV Requirements: L.10.4.4.4.1
141
HST
NICMOS
MOSES
Activities
NIC13 NICMOS Thermal
Characterization
NIC14 NICMOS Detector Read
Noise and Dark Current
Characterize the stability of the
HST+NCS+Instrument thermal emission as seen
by NICMOS on secular scales. The data will be
obtained using NIC3 and the F222M filter and will
run throughout the extent of SMOV4 activities as
a pure parallel program
The NICMOS detector characteristics will be
monitored during the extent of SMOV4 through a
series of dark exposures. This will also allow a
determination of the detector temperatures from
bias measurements. The data should be obtained
in SAA-free orbits, approximately every 24 hours.
In addition, the detector read noise and the
detector shading profiles will be measured
regularly.
Estimated time: Pure parallel orbits 100
Science bits to SSR: 126Mb per orbit. A total of
100 orbits and 12.6Gb
Estimated time: Internal orbit 30
Science bits to SSR: 5742Mb per week for the
duration of SMOV4. One dark per day (756Mb),
one Read Noise+Shading every 5 days (451Mb).
Comments:
Comments: Based on program from Feb 2007
SMOV Requirements: L.10.4.4.4.4
SMOV Requirements: L.10.4.4.6.1
142
HST
NICMOS
Ext.
orbits
Activity
Name
Int.
orbits
NIC01
NCS Cool-down
–
NIC02
Activation test
1
X
NIC03
DC Bias Test
4
X
375Mb
L.10.4.4.1.3
NIC04
Filter Wheel Test
6
X
940Mb
L.10.4.4.1.2
NIC05
Focus & Tilt
17
X
838Mb
L.10.4.4.3.2
NIC06
FOM Functional
1
110Mb
L.10.4.4.1.2
NIC07
Aperture Location
6
1312Mb
L.10.4.4.2.1
NIC08
Plate Scale
4
189Mb
L.10.4.4.3.1
NIC09
Geometric Stability
2
126Mb
L.10.4.4.4.2
NIC10
Mode-2 Coron Acq.
4
900Mb
L.10.4.4.2.2
NIC11
Coron. Focus
10
1779Mb
L.10.4.4.3.3
NIC12
Coron. Performance
6
1696Mb
L.10.4.4.4.1
Coron. enable
NIC13
Thermal Char.
(100)
12600Mb
L.10.4.4.4.4
Pure parallels
NIC14
Darks/Read Noise
30
5742Mb*
L.10.4.4.4.3
*Data per week
Total
35
56
SC
X
Science
bits
MOSES
Req.
Comment
L.10.4.4.5.1
~2 weeks
L.10.4.4.1.1
After BEA
Science enable
~44Gb
143
HST
MOSES
EARLY RELEASE OBSERVATIONS
SMOV4 PLAN
Keith Noll
SMOV Project Review
October 12, 2007
144
HST
ERO: Who’s Involved
MOSES
• Instrument-specific teams: WFC3 SOC, COS IDT,
ACS,STIS,NICMOS Instrument Science Teams +
community consultation
• GSFC: Leckrone, Niedner
• HQ: Stern, Morse, Mather, Hayes
• STScI: Noll, Reid, Sembach,
Biagetti,Mountain
• OPO: Livio, Villard, Gundy,
Estacion, Levay, Frattare
WFPC2 ERO from SM1.
145
HST
ERO: Philosophy
MOSES
• Images and other outreach products designed to produce
maximum positive news for Hubble project.
• Communicate excitement of astronomical enterprise to
the public.
• Inform scientific community of capabilities of new and
revived instrumentation.
• Demonstrate most capable,
instrument-laden Hubble ever.
• Stay on the forefront in outreach
as well as science with creative
approach to new media.
STIS ERO from SM2.
146
HST
ERO: Process
MOSES
Phase 1: Brainstorming
-
Instrument teams have developed multiple candidates
farthest along for WFC3 and COS, all teams active
consider unconventional media outlets: YouTube, iPhone, etc.
look for opportunities to leverage previous work, multiple instruments
Phase 2: Winnowing
-
downselect to ~2-4 targets per observing mode
use explicit criteria for downselect
rank recommendations
Phase 3: HQ Briefing and Selection
-
proposal package presented to HQ
HQ directly involved in selection
Phase 4: Implementation
-
generate final phase 2s
integrate final program into SMOV schedule
contingency plan
NICMOS ERO from SM2.
147
HST
ERO: Selection Criteria
MOSES
• Spectacular images - goal is front page, above the fold.
• Unique capabilities - highlight unique features of each
instrument, demonstrate inherent complementarity,
• Suitable for a broad audience from general public to
scientific community
• IMAX compatible - IMAX
digital resolution requires
5616x4096 pixels --> single
frames OK, mosaics enable
pan and zoom
• Practical - must be
schedulable and allow for
WFPC2 ERO from SM3A.
148
adequate processing time
HST
ERO: Schedule
Presentation to HQ: ~ February 2008 (TBD)
Execution on Spacecraft (all dates approximate, assume early Aug launch):
•
•
•
•
Instrument dependent
~mid September~early October
ERO Press release: ~ mid-late October 2008 (TBD)
•
•
Avoid US presidential election news cycle!
AAS
•
•
•
•
MOSES
Long Beach, CA 7-10 January 2009
Pasadena, CA 7-11 June 2009
IAU General Assembly
•
•
Rio de Janeiro, Brazil 3-14 August 2009
International Year of Astronomy 2009
WFPC2 ERO from SM3A.
149
ERO: GTO & Early Release
Science
•
HST
MOSES
GTO and Early Release Science programs provide additional
outreach opportunities
– Pre and post launch media
– Scientific meeting presentations
– Journal special issues
•
ERO will coordinate with
GTO/ERS to maximize outreach
with minimal cost.
ACS EROs from SM3B.
150
HST
ERO: Results
MOSES
• Progress is good
• No identifiable hurdles to
meeting expected goals
NGC 3603 (released Oct 4, 2007)
151
HST
MOSES
SMOV4 PROJECT REVIEW
CLOSING REMARKS
152