Telescope and Instrument Performance
Summary (TIPS)
16 May 2002
AGENDA
1.
2.
3.
4.
NISD Perspective
NICMOS Update
STIS Update
FGS Update
Ralph Bohlin
Torsten Boeker
Charles Proffitt
Ed Nelan
Next TIPS Meeting: 20 June 2002
NISD PERSPECTIVE
02MAY16
R. Bohlin
SMOV - Carl
Biagetti
• As of May 5, 64 of 93 SMOV 3B activities have been
executed for a total completion rate of 70%. Nominal
end is Jul-Aug.
• 02Aug-Sep, SMOV 4 planning starts for 04 Feb launch
of COS and WFC3.
COS - Tony
•
•
•
•
•
Keyes
Front end ground system software (commanding/TRANS
/scheduling/APT) is ~2/3 done. Finish ~03Jan.
CALCOS pipeline data processing ~2/3done.
Finish ~03Jan.
Science ground cal (thermal vac) at Ball 03Jan.
Delivery to GSFC 03Feb
SMGT 03May-Jun
WFC3 - John
•
•
•
•
•
MacKenty
Front end is ~half done.
Pipeline data processing on schedule. First
UVIS test images received.
Delivery to GSFC 02Aug
Science ground cal (thermal vac) at GSFC
March-May 2003.
SMGT 03Jul-Aug
News/status:
There are no showstoppers.
• GSFC has taken over WFC3 flight software coding
from Ball.
• Rockwell is characterizing additional WFC3
IR detectors. QE problem is solved. There still
are concerns with readnoise and stability
of dark current.
• Berkeley is requalifying QE grids for the COS
FUV detector.
Torsten Böker
TIPS
May 16, 2002
Instrument status
1) Final temperature adjustment
2) Fine Optical Alignment
3) Remaining SMOV timeline
Thermal stability
Mounting cup A/D limit
Compressor margin
NICMOS Fine Optical Alignment
NICMOS focus sweep
Encircled Energy measurements (G. Schneider)
Focus history
NIC2 Focus vs. Time
NIC1
NIC3 Focus vs. Time
73
4
7
0
72
3
72
3
71
6
70
9
69
6
68
2
66
61
4
0
54
3
51
7
44
8
39
5
36
9
33
30
7
7
26
1
9
23
20
2
18
14
15
3
6
9
13
2
12
6
12
8
11
4.5
3.5
-2
10
95
78
63
54
0
3.5
2.5
-6
Cycles 7 Focus Moniter Data
Cycle 7 Focus Moniter Data
NIC3 nominal PAM position
3
2
-8
Current NIC1 nominal Pam Position
2.5
1.5
-10
2
Current NIC2 Nominal PAM position
1
-12
1.5
SMOV datum
(no breathing
correction applied)
2
4
6
19
66
61
0
52
49
73
7
0
72
3
0
51
4
SMOV datum
(no breathing
correction applied)
41
7
39
7
37
1
5
3
9
8
36
35
33
32
5
Days since Jan. 1,
1,199
199
9977
Days since Jan. 1,199
97
30
29
7
26
1
25
7
23
9
5
22
1
5
20
19
18
8
0
0
16
14
14
3
13
6
12
9
11
3
11
5
10
95
87
78
-1
-20
71
-0.5
-18
0
71
3
70
6
69
68
9
6
66
2
61
52
0
4
41
7
37
1
35
32
3
5
29
1
25
5
22
5
19
0
16
0
14
12
6
3
11
95
Cycle 7 Focus Moniter Data
78
63
0
-16
0.5
SMOV datum
(no breathing
correction
applied)
72
0.5
-14
1
63
Foucs
(mm
of of
PAM
space)
Focus
(mm
PAM
space)
Focus
(mm
PAM
space)
4
3
-4
Y-tilt
Coma correction: NIC1 PAM tilt grid
Similar datasets for NIC2
and NIC3 will be obtained
within a few weeks…..
X-tilt
Remaining issues and NICMOS SMOV timeline
- currently investigating impact of SAA-persistence and possible scheduling
constraints for certain GO programs
5/08 Wed
Final temperature set point (TBD)
5/10 Sat
8893 & 9013
8985, 9269
EROs begin
Calibration flats, thermal background monitor begins
5/13 Mon
8975
Detector read noise & shading profiles
5/16 Thu
8977
Final NIC1 tilt update, GO science enabled
5/17 Fri
8981
Aperture locations
5/22 Wed
8982
Plate scale
5/23 Thu
8988
Astronomical persistence
5/24 Fri
8991
Grism calibration
5/19 Sun
8893 & 9013
EROs completed
5/26 Sun
8987
SAA Impact & CR persistence
Torsten Böker
TIPS
May 16, 2002
Summary
- GO science (except coronagraphy) is enabled
- ERO release on June 5 at AAS
- all is well….
1
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
STIS Status Report, 16 May, 2002
•STIS Calibration Plan for Cycle 11
•MAMA Dark Current since SMOV3B
2
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
STIS Calibration Plans for Cycle 11.
Considerations for Cycle 11
• Approved STIS GO orbits are down significantly for cycle 11 (1040 prime GO
orbits rather than the 1800 to 1900 orbits in cycles 7 through 10). In particular,
STIS imaging now accounts for only 2.7% of HST science.
• Most detector modes are now well understood, so the frequency of some
external monitors can be decreased without affecting the quality of calibration.
• There are some uncertainties in the absolute and relative flux calibration of the
E1 positions now supported for 1st order spectra near row 900 of the CCD.
• Monitor programs run for 13 months (Sep 1 2002 to Sep 30 2003) to give
more flexibility for Cycle 12 planning.
• Fewer special calibration programs.
3
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Orbit Allocations by Cycle
Cycle
Prime
GO
STIS/Cal STIS/
Prime
Cal Par.
STIS/Cal
Internal
7
1829
300
526
2244
8
1919
135
182
1761
9
1925
84
232
1658
10
1814
108
220
1503
11
1040
70
232
1700
Above numbers do not include side-2 recommissioning programs, contingency orbits,
or other additions not included in the calibration plans.
4
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
STIS Cycle 11 Calibration Plan
Estimated Time (orbits)
ID
Proposal Title
Frequency
“External” “Internal”
Prime
& Parallel
CCD Monitors
9604 CCD Performance Monitor
2 per year
42
9605 CCD Dark Monitor
9606
14 per week
760
9607 CCD Bias Monitor
9608
daily
395
9609 CCD Read Noise Monitor
monthly
26
9612 CCD Hot Pixel Annealing
monthly
168a
9613 CCD Spectroscopic Flats
monthly
68
9614 CCD Imaging Flats
monthly
17
9617 CCD Spectroscopic Dispersion Monitor
annually
7
9620 CCD Sparse Field CTE Internal
annually
96a
9621 CCD Sparse Field CTE External
annually
12
9622 CCD Full-Field Sensitivity Monitor
annually
1
9626 Slit Wheel Repeatability
annually
9627 CCD Spectroscopic Sensitivity Monitor
4 per year
1
8
5
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Estimated Time (orbits)
ID
Proposal Title
Frequency
“External” “Internal”
Prime
& Parallel
MAMA Monitors
9618 MAMA Dispersion Solutions
annually
36
9623 MAMA Full-field Sensitivity
annually
3
9628 MAMA Sensitivity & Focus Monitor
bi-monthly
16
9615 MAMA Dark Monitor
twice weekly
226
9629 MAMA Fold distribution
2 per year
4
9624 MAMA FUV flats
annually
10
9625 MAMA NUV flats
annually
10
9630 MAMA FUV/NUV Anomalous Recovery
As needed
N/A
Special Calibration Programs
9616 E1 Pseudo-Aperture Sensitivity and Throughputs once
4
9610 Spectroscopic PSF
once
3
9611 CCD Side-2 Gain Ratio Test
once
2
9631 Faint Standards Extension (FASTEX)
once
19
9619 Echelle Blaze Shift vs. MSM Monthly Offset
once
2
2
6
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Changes to Monitoring Programs
• Decreased frequency of MAMA spectroscopic sensitivity monitors. L modes
reduced from 12 to 6 times per year, and M modes from 6 to 4 times per year,
saving a total of 8 prime orbits/year.
• Decreased frequency of full field sensitivity monitors. Will only do once per
year, rather than twice, saving 4 prime orbits.
• Add annual NUV-PRISM observations to MAMA spectroscopic sensitivity
monitor. Prism sensitivity was last measured in 2000, but had significant usage
in cycles 10/11 (2 extra orbits this year, 1 per year continuing).
7
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Added Support for E1 Positions
• E1 aperture positions were defined to allow spectroscopy to be done closer to
the CCD readout, thereby reducing charge transfers and CTI effects by a factor of ~ 5. CCD sensitivity at this position differs by a few percent, and focus
and PSF differences may alter relative throughputs of narrow slits.
• Added exposures using 52X2E1 to the usual G230LB, G430L, G750L sensitivity monitoring program. This can be done without extra orbits.
• Added two orbits to CCD sensitivity monitor to allow the standard G230MB,
G430M, and G750M monitoring at selected wavelengths to also be done at E1
positions.
• Added a special program to observe a white dwarf standard through
52X0.05E1, 52X0.1E1, 52X0.2E1, 52X0.5E1, and 52X2E1 apertures. Prior
aperture throughput tests at the E1 positions did not use a standard star, so
absolute flux results are less certain. Doing two visits of two orbits each, separated by a few months, will test small slit throughput repeatability.
8
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
MAMA Dispersion Solutions (36 Internal Orbits).
• Dispersion solutions for many central wavelengths never checked on-orbit.
Will take deep wavecals at all central wavelengths this cycle.
• This data will be valuable for future ECF recalibration efforts.
CCD Dispersion Solutions (11 Internal Orbits)
• Regular line lamp has very low signal-to-noise at E1 position.
• Use HITM1 instead of usual LINE lamp to better illuminate E1 positions.
9
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Special Calibrations
Faint Standards Extension (FASTEX), 19 prime orbits.
• Primarily driven by the need to provide more standard stars for other instruments and projects (ACS Sloan filters and prism, as well as COS).
• Observe two new faint WD standards (V = 16.5) and improve observations for
two more.
• Also observe primary Sloan standard with STIS CCD to cross-calibrate.
Echelle MSM Offset Test (2 prime orbits)
• The monthly spectral offsetting causes a misalignment of the wavelength scale
with echelle blaze function. This adversely affects the extracted fluxes.
• Don’t have a flux standard with multiple offsets at same CENWAVE.
• Will observe the WD flux standard HZ 43 with E230H using the 2513 Å setting at five different MSM offset positions.
• Data will allow improved test of software fix devised by Lindler & Bowers.
10
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Upper panel shows blaze function misalignment. Bottom shows Lindler’s fix.
1.5
Old
1.4
Flux 10−12 erg s−1 cm−2 Å−1)
1.3
1.2
1.1
1.0
1.5
1.4
Order 313
Order 312
Order 311
1.3
1.2
1.1
1.0
E230H / 2513 (o6hb30020)
2465
2470
Lindler Algorithm
2475
2480
Wavelength (Å)
2485
11
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Gain ratio test (two prime and two internal orbits)
•
•
•
•
Take high signal-to-noise spectra of external target in gain=1 and gain=4.
Will give better estimate of gain ratio (current estimate 4.08+/-0.08).
Also checks that use of the side 2 electronics hasn’t changed the gain ratio.
Also includes measurements of B amp gain and bias, which will be useful for
CTE tests done using both B and standard D amps to read out the CCD. This
will allow us to infer the impact of CTE loss on the derived gain ratio.
CCD Spectroscopic PSF Test (3 prime orbits)
• Step 52x0.1 and 52x0.2 slits across a star to measure off-axis and out of slit
PSFs using the G750L. Will do both regular and E1 positions.
• Relevant for numerous galactic and black hole dynamics programs, both current and archival, which depend heavily on the ability to model the STIS PSF
in the red and near IR.
12
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
MAMA Dark Current Since SMOV3B.
• NUV MAMA dark current due to phosphorescence of window impurities.
• A short term increase in the temperature, T, increases the rate at which metastable states depopulate, increasing the dark current by about 12% per ˚C. This
is seen during daily temperature cycling.
• However, a sustained increase in T also reduces the overall population of
excited meta-stable states, moderating the increase in the dark rate.
• Expected net increase of about 4% in NUV dark rate per ˚C.
• Extra heat input from new instruments after SMOV3B was expected to
increase aft-shroud T by a a few ˚C.
• STIS Heater Zone 3A (the one nearest the MAMA detectors) was stuck at max
power between Nov 30, 2001 and Feb 17, 2002.
13
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Daily average of OMTUBET temperatures during Side 2 operations.
14
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
Dark rates during 2 periods of Side-2 STIS operations.
Despite increase in mean T of NUV MAMA, mean dark values are similar.
15
SPACE TELESCOPE SCIENCE INSTITUTE
STIS Status
TIPS 16-May-2002
Charles R. Proffitt
FUV MAMA dark “glow” also tends to increase as temperature increases.
Limited data since SMOV3B indicates no new enhancement of the FUV glow.
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS
• Comparing Pre-SM3B and Post-SM3B FGS performance.
• HST Jitter
• FGS1r Astrometric Performance; first parallax
• FGS1r BEA Science Update
1
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS SMOV3B
• FGS SMOV3B consists of:
– verify that S-curves have not changed in any FGS
– verify that distortions have not changed in any FGS.
• FGS observations of Upgren69 (our standard) show no appreciable changes in
S-curves across SM3B for any FGS.
– no need to update guide star and astrometry star acquisition parameters.
• Distortion monitoring observation were made during the epoch of high jitter.
However, recent astrometry science data indicates no change in distortion (in
FGS1r) at the sub-mas level.
2
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS2r S-curves Pre-Post SM3B
X-axis, F583W
3
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS2r S-curves Pre-Post SM3B
Y-Axis, F583W
4
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS2r S-curves SM3A-SM3B
Evolution of FGS2r X-axis, 1999 (dashed line) to 2002 (solid line).
5
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS2r S-curves Pre-Post SM3B
Evolution of FGS2r Y-axis, 1999 (dashed line) to 2002 (solid line).
6
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
FGS2r S-curves for Guiding
2/3 Pupil Restores FGS2r S-curves for guiding HST
7
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter
• New Solar panels reduced HST jitter, especially across Day/Night transitions.
• The (original) pointing control law, appropriate for new solar panels, was activated.
• FGS and STIS jitter measurements indicated the presence of a prominent
oscillation of HST with a period of 2 seconds (0.5 hz)
– but jitter was still within specification.
• The 0.5 hz was traced to a flaw in the pointing control law.
8
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter
• Gyro failure reduced control to 3-gyro configuration.
– jitter exceeded specification (> 0.007”)
• Flight software was updated to eliminate the control law error (late April).
• FGS jitter test was repeated on May 7, 2002.
– jitter within specification (~0.003”)
9
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter Power Spectrum
V2 jitter power spectrum as seen along FGS2r x-axis
10
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter Power Spectrum
V3 jitter power spectrum as seen along FGS2r y-axis
11
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter
Time series profile of jitter along V2 (as seen along FGS2r x-axis).
12
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Jitter
Close up time series profile of jitter along V2 (as seen along FGS2r x-axis).
13
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Astrometric Performance, FGS1r
• All post-SM3B FGS distortion measurements were made in 3-gyro mode with
flawed pointing control law.
• Data of reduced quality, but no significant degradation for guiding performance seen.
• What about for FGS Astrometry science? This requires sub-mas stability in
the geometric distortion (OFAD).
• First opportunity to assess FGS1r astrometric performance came from proposal 9240 (PI McGrath).
14
SPACE TELESCOPE SCIENCE INSTITUTE
TIPS
FGS
May 16, 2002
Ed Nelan
Astrometric Performance, FGS1r
• Comparison of data gathered on May & Nov., 2001 and May 2002 indicate
FGS1r’s astrometric performance is excellent! Analysis invokes
– OFAD calibration
– cross filter calibration
Parallax and Proper Motion of ρCancri
mas
Hipparcos
FGS1r
π
79.8 +/- 0.8
79.8 +/- 0.5
µα
-485.4 +/- 1.0
-483.4 +/- 0.7
µβ
-234.4 +/- 0.7
-236.9 +/- 0.5
15
MEMORANDUM
TO:
Distribution
DATE:
May 16, 2002
SUBJECT:
Questions and Answers from May 16, 2002 TIPS Meeting
NISD Perspective
Presenter – Ralph Bohlin
Q: Is there any change to the current SM4 launch date?
A: No, the current launch date is still February 2004.
FGS Update
Presenter – Ed Nelan
Q: Regarding the point source analysis of Eta Carinae, when nebulosity was added to the model, how was
it done? Was an uniform background used or were structures being incorporated into the nebulosity model?
A: An uniform background model was used, since the beam size for FGS is large and will integrate over all
background structure.
Q: Can the potential binary systems, separated by 30 mas, be resolved?
A: FGS will not be able to resolve this system.
NICMOS Update
Presenter – Torsten Boeker
Q: On the graph showing the mounting cup temperature, it seems to show a 24-hour period temperature
oscillation. Is that real?
A: We currently do not aware of any 24-hour period temperature oscillation. There are existing orbital
temperature variations, but the do not have a 24-hour period. It is possible that what is showing on the
graph reflects CCD housing temperature variation and/or self-heating from the detectors. Further study of
this will be needed.
STIS Update
Presenter – Charles Poffitt
No questions.
1