TIPS-JIM Meeting
16 September 2004, 10am, Auditorium
1.
JWST NIRCam Calibration
Peter McCullough
2.
STIS Failure and Upcoming Tests
Paul Goudfrooij
3.
New Programs for Cycle 13
Duccio Macchetto
Next TIPS Meeting will be held on 21 October 2004.
JWST NIRCam Calibration
Peter McCullough,
Don Figer,
James Rhoads
16 September 2004
9/16/2004
NIRCam Calibration, STScI TIPS
1
Presentation Outline
• NIRCam Timeline
• NIRCam Optical Layout
• Three viewpoints
– Requirements Trace
– Analysis pipelines: CalNIRCamA, B
– Comparison to NICMOS Goals & Plan for
Commissioning
• Plan Outline: from ETU tests to JWST’s EOL
• Astronomical Sources for Photometry, Astrometry
• Summary
9/16/2004
NIRCam Calibration, STScI TIPS
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Not Addressed Here
• Cross-calibrations (to JWST’s NIRSPEC,
FGS; HST; Spitzer)
• WFS, WaveFront Sensing Requirements
– Because only recently completed
– TBR, To Be Reviewed
9/16/2004
NIRCam Calibration, STScI TIPS
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NIRCam Timeline
Oct 20-21, 2004
NIRCam PDR
NIRCam CDR
Oct 13, 2005
2007
2008
2009
2010
Deliver
GSW-01
GSW-02
Oct 20, 2005
Begin ETU I&T
Sep 22, 2006
Begin FM I&T
Launch
2011
Commissioning
completed
6 months after launch
PDR is Preliminary Design Review
CDR is Critical Design Review
GSW-01 defines reduction algorithms
GSW-02 defines reference files and their format
ETU is the Engineering Test Unit for NIRCam
FM is the Flight Model for NIRCam
9/16/2004
NIRCam Calibration, STScI TIPS
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Optical Layout
From OTE
3
9
10
11
12
4
5
6
2
1
7
14
1
Pick-Off Mirror Assembly
2
Coronagraph
3
First Fold Mirror
4
Collimator Lens Group
5
Dichroic Beamsplitter
6
Long Wave Filter Wheel Assembly
7
Long Wave Camera Lens Group
8
Long Wave Focal Plane Housing
9
Short Wave Filter Wheel Assembly
13 10
8
15
Short Wave Camera Lens Group
11
Short Wave Fold Mirror
12
Pupil Imaging Lens
13
Short Wave Focal Plane Housing
14
ICE Interface Panel
15
FPE Interface Panel
Light source
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NIRCam Calibration, STScI TIPS
NIRCam Optics & Mounts PDR, September 8, 2004
5
Flat Field Sources are in Pupil Wheel
Pupil Wheel
Pinhole Integrating
Cavity Assembly
Thermal
Radiant Source
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NIRCam Calibration, STScI TIPS
NIRCam Optics & Mounts PDR, September 8, 2004
6
Flat Field Sources Design Concept
Optical Integrating Cavity located on Pupil Wheel
Radiant Source – Fixed to Bench
Pinhole Aperture
9/16/2004
NIRCam Calibration, STScI TIPS
NIRCam Optics & Mounts PDR, September 8, 2004
7
Pinhole Integrating Cavity
Pinhole aperture (1 shown)
Exiting light paths
Incident light
from radiant source
9/16/2004
NIRCam Calibration, STScI TIPS
NIRCam Optics & Mounts PDR, September 8, 2004
8
Lyot Coronagraph Occulting Masks &
Pinhole Sources
Occulting Mask
Substrate
LED Source
Calibration pinhole
9/16/2004
NIRCam Calibration, STScI TIPS
NIRCam Optics & Mounts PDR, September 8, 2004
9
Three Viewpoints
to Calibration Plan
1. JWST+NIRCam Requirements
2. Software Pipeline (IDTL, Calnica, …)
3. Prior Calibration Experience (NICMOS, WFC3, …)
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Requirements Trace to
Calibration Plan
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NIRCam Calibration, STScI TIPS
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Requirements: detector
3.7.3.10 Pixel Operability
3.7.3.11 SCA noise
3.7.3.12 Read noise
Electrical crosstalk
3.7.3.13 between pixels
3.7.3.14 Radiometric Stability
Latent or Residual
3.7.3.15 Images
3.7.3.16 Radiation immunity
9/16/2004
While simultaneously meeting all requirements,
the SCA operability shall be > 98%
The total noise per pixel shall be < 9 e- (rms) in an
integration period of 1000secs. This will be
measured with two groups of 8 samples or
Frames,
The read noise for a single read shall be < 15 e(rms)
The electrical crosstalk between pixels shall be <
5%
The radiometric stability over 1000seconds shall be
< 1%
Latent or residual images when measured at the
same integration time as was use for the near
saturation image shall be <0.1% after the 2nd read
following an exposure of > 80% of full well
No more than 4% of the pixels will be degraded
from their original performance after 5.5 years at
L2 within NIRCam. This may be verified with
analysis and agreed upon assumptions of TID at
L2.
NIRCam Calibration, STScI TIPS
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Requirements: coronagraphy
2.3 Coronagraphy
2.3.1 General
Characteristics
Little
or no influence
BTG2004
3.3.1.2.1
NSRD
page 2
3.3.2.2.1 Coronagraph Capability
2.4.3 Coronagraphic Science
We assume that the coronagraph will be allowed to
have little or no influence on the design or
operation of the telescope and minimal impact on
design of NIRCAM.
NIRCam shall provide a coronagraph capability in
all four of the imaging channels. This will be
enabled by the placement of coronagraph image
masks at the edge of the telescope focal surface
and selection of a coronagraph wedge in each of
the filter wh
NIRCam should be able to detect objects
as small as 1 MJ located outside 10-20 AU of the
star. For stars 5 Gyr old, Jupiter-mass objects
are detectable to ~5 pc.
10 AU at 5 pc is 2 arcsec
5 AU at 10 pc is 0.5 arcsec
MSRD
3.3.1.2.2
3.3.1.2.3
BTG2004
6.5 Coronagraphic Science
ND Filters on
3.3.2.2.2 Coronagraphic Slide
Coronagraphic mask
3.3.2.2.3 stability
Fig 15 Target Acquisition
On-board centroiding
3.8.1.2
Spacecraft Coarse Roll
Control
OBS-1621
Table 6-2 states that AB mag = 18, the bound
planet brightness is based on a 2-Jupiter mass
planet 5 AU from an M star 10 parsecs from Earth.
Neutral Density filters of density n = 3 (TBR) and
> 2arcseconds (TBR) diameter shall be utilized to
allow for centroiding bright sources.
Once NIRCam has reached it operating
temperature, the coronagraphic occulting mask
slide shall remain within 0.005 (TBR) arcseconds
of its nominal position relative to the pixels on the
FPAs over a timescale of 1 month (TBR).
to 0.010 (TBR) arcseconds 1-sigma each axis
To support coronagraphy, ISIM C&DH shall be
capable of positioning a point source on a
coronagraphic spot with an accuracy of 0.005 arcseconds (TBR).
During a science target observation, the Spacecraft
coarse roll control shall be less than or equal to 6.5
arcseconds RMS.
Software Pipeline Trace to
Calibration Plan
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NIRCam Calibration, STScI TIPS
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CalNIRCamA
Flowchart
p_udgjcdpmk/QA?9
/pcqcrmdbcrcarmp9
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Dj_eqqcr_qDGRQ
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sqcb`wngncjglc
K?QIAMPP
?nnjwK_qi
K?QIDGJC
PCDAMPP
PCDAMPPRWNC
PcdNgvcjAmppcar
LMGQA?JA
A_jasj_rcLmgqc
LMGQDGJC
@BAMPP
Qs`@g_q-B_pi
@G?QB?PIDGJC
LJGLAMPP
Lml+jglAmppcar
LJGLDGJC
APGB
APGbclrgdw
QJMNCDGR
QjmncDgr
DJ?RAMPP
Dj_rAmppcar
DJ?RDGJC
NFMRA?JA
A_jasj_rcNfmr
NFMRR?@
A_jg`p_rcb
Gk_ecqcr
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NIRCam Calibration, STScI TIPS
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HST Heritage Trace to
Calibration Plan
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NIRCam Calibration, STScI TIPS
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Trail Blazers
NICMOS
WFC3
NIRCam
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NIRCam Calibration, STScI TIPS
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NICMOS Calibration Goals
NIRCam will have
similar goals, except
no polarization and
no grism,
except WFS grism
in the Dispersed
Hartmann Sensor,
which is only used
in commissioning.
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NIRCam Calibration, STScI TIPS
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NIRCam Calibration Plan
duration in
NICMOS SMOV
NICMOS # NICMOS Name
1
2
3
4
SMR-2021/Rev A
MacKenty, J. 1997.01.31
to HOLD Mode
Internal parallel operation
memory load and dump
field offset mechanism
5 filter wheel mechanism
6 Electronic noise; SAA contour
7 Dewar heaters Setpoint
adjustment
8 Transfer function
9 Target Acquisition
10 NICMOS to FGS Astrometric
Calibration - aperture locations
11 Plate Scale and Astrometric
Calibration
12 Coarse Optical Alignment
13 Fine Optical Alignment
14 Point Spread Function
Characterization
15 Persistence
16 IntFlat Transfer and Stability
17 HST thermal background
18 Absolute photometry
19 Differential Photometry
20 Detector noise and Dark
characterization
Commissioning
Maintenance
CFT
0:02
3:00
1:30
10:00
CPT
A*
M
B,L
G
V1
ISIM Plum
A*
A*
E
B,C,G
F
H
H
H?
H
.
.
E,R
.
.
.
G
M
n
Y
J
L
Y
J
K
Y
A,B
n
B,C
B,I
Y
B
J
Y
N
F
C,O,R
C,S
C,S
.
Y
Y
Y
Y
D
Y
E
M
Y
D
A,H,R ?
I
P,Q
n
Y
n
.
I
6:00
24:00:00
0:05
0:40
5:00
5:00
1:30
J
11:00
J
16:00 E,F,H
,I
11:00
3:30
9:30
16:00
6:30
18:00
8:00
21 Coronagraphic Performance
verification
22 Limb avoidance Determination
23 Thermal Check on COSTAR
9:00
15:00
deploy
Grism Validation
Focus Monitor
Scattered Light Determination
SI Parallel Operations
10:00
16:30
1:30
9:00
4:30
24
25
26
SI-1
Ground test
Cycle 7
(hh:mm)
C
B
D
A
B
E
E
A
I
B
C
J
F
G
H,I
K
D
H
C,D
NIRCam Calibration Plan
Outline
Cold Functional Test (CFT) @ LMATC
Comprehensive Performance Test (CPT) @ LMATC
+V1 Down Test @ GSFC
ISIM Test @ GSFC
JWST Test @ Plum Brook or equivalent
On Orbit Commissioning @ L2
Maintenance Calibration @ L2
9/16/2004
NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
20
Cold Functional Test
A.
B.
C.
D.
E.
F.
G.
H.
I.
J.
BiasDark & Readnoise
Flats: lamp visible thru all filters
Coronagraphic emitters
PIL (Pupil Imaging Lens) – repeatability of PIL, PW
WFE using NOTES (NIRCam OTE Simulator)
WFE using Coronagraphic emitters
DHS rotation
FAM (Focus Adjust Mechanism, “pickoff mirror”)
Confocality of LW and SW FPAs
Alignment of LW and SW FPAs
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
21
Comprehensive Performance Test
(1 of 2)
A. Repeat CFT
B. Explore behavior by varying
1. integration time
2. Source brightness
3. Sampling
4. Co-adding
C. Subarrays
D. FAM calibration using NOTES
E. Linearity, Saturation, Latency
F. Thermal tests (SCAs and mechanisms)
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
22
Comprehensive Performance Test
(2 of 2)
G.
H.
I.
J.
K.
L.
M.
Flight-like scripts using SITS
Ghosts, Glints, & Diffuse scattered light using NOTES
Dark position is indeed dark
Coronagraphic slide survey (mapping)
DHS dispersion using NIRCam’s R=100 filters
Data rate & volume stress test
Fault protection test
9/16/2004
NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
23
+V1 Down Test
A. WFE using NOTES
B. Alignment of cubes (warm vs cold)
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
24
ISIM Test @ GSFC
A.
B.
C.
D.
E.
F.
G.
H.
Repeat CFT
Readnoise thru flight (or flight-like) wiring
EMI/EMC with parallel ops’ with FGS (& other SIs)
Stray light with parallel ops’..
Fault protection
Subarrays
Data rate and volume stress test
Flight-like scripts using ICDH
9/16/2004
NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
25
JWST Test @ Plumbrook
A.
B.
C.
D.
E.
F.
Repeat CFT
FAMs, confocality of modules
PIL: OTE pupil shear compensation using FAMs
WFS&C
Subarrays
Data rate & volume
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
26
On-Orbit Commissioning (1 of 2)
A.
B.
C.
D.
E.
F.
G.
H.
I.
J.
K.
Alignment
Pupil Shear
Radiometric Calibration
Dark current and read noise checks
Internal throughput checks
Flat field measurements
FPA tune-up – biases, offset voltages, etc.
Observing mode checkouts
Focus confirmation on stellar sources
Point spread function characterization
Distortion mapping – confirming plate scales and distortions
across the field of view
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
27
On-Orbit Commissioning (2 of 2)
L. Focal plane survey – locations of the NIRCam fields of view
relative to FGS
M. Coronagraphic mode checkout – verifying emitters, ND spots,
offsets to the coronagraphic masks, algorithms for
centroiding, coronagraphic contrast
N. Latent image verification
O. Sensitivity/confusion limit checks
P. Off-axis glint checks
Q. Scattered light checks
R. Routine calibration activities
S. Checkout of candidate calibration sources
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NIRCam Calibration, STScI TIPS
Horner & Kelly, Jul 2004
28
On-orbit Maintenance
Programs for NIRcam, to date.
SODRM #
421
NIRCam Flat Field Monitoring
422
423
NIRCam Dark Monitoring
NIRCam Photometric Monitoring
424
NIRCam Short term Astrometric
Monitoring
NIRCam Long Term PSF
Monitoring
425
9/16/2004
Title
NIRCam Calibration, STScI TIPS
29
SODRM Program 423
Program No.: 423
As-of date: 2/23/04
Program title: NIRCam Photometric Monitoring
Synopsis: The goal of this proposal is to monitor the stability of NIRCam’s
photometric calibration. The observations will be carried out twice a year. It
is assumed that the photometric standard stars (or even better two secondary
calibrator fields) will have been observed during the commissioning.
Sample and sky coverage: Two standard stars suitably positioned.
Instruments and observing configurations: 60s in each filter.
Scheduling requirements or constraints: These are primary external
observations.
Visit scenarios: 2000s visit plus overheads
Total program time needed (days): 1
Program written by: Massimo Stiavelli and Peter McCullough
Date first written: 2/23/2004
9/16/2004
NIRCam Calibration, STScI TIPS
30
NIRCam Photometric Calibration
Clusters are chosen based upon suitability to solar-analog method
of calibration (Campins, Rieke, Lebofsky 1985):
–Solar
–Color, B-V0 = 0.6 to 0.7
–Age < 8 Gyr (so solar-temperature dwarfs still exist)
–Metallicity, Fe/H ~ 0
–Low extinction, E(B-V) < 0.2
–Rich and compact, in order to permit robust selection from
multiple candidates in NIRCam FOV
–Distance modulus, m-M > 11.7, d > 2200 pc presumes
– Sun’s Mv = 4.8; V-K = 1.5
– K=15 stars don’t saturate in quickest MULTIACCUM (TBR)
– Subarray use is TBD
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NIRCam Calibration, STScI TIPS
31
Stauffer, NIRCam Sci Team Meeting, May 2003
NIRCam cf. 2MASS
2MASS K-band image
(SNR=10 at K=15)
NGC 2420
NIRCam saturates at
K~15 unless subarray is
used.
= solar type star
= NIRCam FOV
(location is TBD)
Other open clusters that meet E(B-V), m-M, [Fe/H] criteria:
NGC 2506, 6791, 2266, 2243, Mel 66, Berk 39
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NIRCam Calibration, STScI TIPS
32
NIRCam Astrometric Calibration
We want to know how to do this: (x,y) (α,δ)
• HST observations of globular clusters are ideal
• A priori astrometry (easy way fewer NIRCam exposures)
• High density of stars within NIRCam FOV (2’x4’)
• 100,000 stars, not too bright (K > 15)
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NIRCam Calibration Summary
•
•
•
•
Requirements traced to plan
Heritage from NICMOS, WFC3, and ACS; IDTL
Basic calibration steps planned out
Calibration achievable on orbit
– Lamps are inside NIRCam, also dark slide
– Robust against changes to on-orbit environment
• Need to consider
–
–
–
–
WFS requirements
Cross-calibrations (to NIRSPEC, FGS, HST, Spitzer)
Saturation limit of NIRCam
Commissioning schedule for arbitrary launch date
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NIRCam Calibration, STScI TIPS
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Backup Slides
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NIRCam Calibration, STScI TIPS
35
NIRCam Cheat Sheet
Cheat
Sheet
Pixel Formats and Scales
Arm
Short
Long
λ-range
0.6 - 2.3µm
2.4 - 5.0µm
Pixel Format
4080x4080*
2040x2040
Pixel Scale
0.032“
0.065"
Long and short arms view same area on sky through a dichroic. Redundant A&B modules view adjacent areas on sky (separated by ~25")
*Has ~6" gaps between SCAs.
Detector Performance Requirements
Total Read Noise
Single Read Noise
Dark Current
QE
Well depth
Min. exposure time
Pixel size
Detector Max Op T
≤ 9e- in 1,000 secs
~14 e≤ 0.01 e/sec
≥ 80%
~90,000 e10.6 sec (full frame)
10µsec x No. of pixels (sub-array)
18µm x 18µm
80K, short-λ,42K, long-λ
Flat field sources illuminate back half of NIRCam optical train only.
Coronagraphy uses focal plane masks moved into detector FOV using wedge mounted with pupil wheel mask.
Flux Conversion: 0.038 e-/sec/nJy for F200W
Sensitivity: F200W 10,000secs 10-σ = 10.4 nJy, F444W , 10,000secs 10-σ = 24.5 nJy
9/16/2004
NIRCam Calibration, STScI TIPS
Rieke, Feb 2004
36
Filters
Revised Filter Set for Each Imaging Module
(subject to further change)
Short - λ Arm
Long - λ Arm
Filter Wheel
Pupil Wheel
Filter Wheel
Pupil Wheel
F070W
Imaging pupil
F270W
Imaging pupil
F090W
Flat field source
F357W
Flat field source
F110W
Outward pinholes
F444W
Outward pinholes
F150W
Coronagraph pupil 1
F250M
Coronagraph pupil 1
F200W
Coronagraph pupil 2
F300M
Coronagraph pupil 2
F140M
WFS dispersive #1
F335M
F241N
F163M
WFS dispersive #2
F430M
F256N
F183M
WFS weak lens 1
F460M
F469N
F210M
WFS weak lens 2
F405N
TBD Filter
F164N
WFS weak lens 3
F480M
TBD Filter
F187N
F212N
F390M
TBD Filter
WFS Filter
F108N
F360M
TBD Filter
Filter Names: FXXXR XXX=Center λ in 100xµm R= (W for R=4, M for R~10, N for R=100)
9/16/2004
NIRCam Calibration, STScI TIPS
Rieke, Feb 2004
37
CalNIRCamB
Concepts
A_jg`p_rcb
Gk_ecqcr
DGRQfc_bcpicwumpbq
Pcdcpclacdgjcq8
?qrpmkcrpw
Xmbgkmbcj
NQD
A_jLGPA_k@
E_n+dpcc
Gk_ecqcr
Bcamltmjtcb
Gk_ecqcr
&gdpcosgpcbc,e,`wqrsai
qcekclr&q'mdNK'
A_r_jmemd
Qr_pq*E_j_vgcq*cra
9/16/2004
Not included
in current
contract of
S&OC.
NIRCam Calibration, STScI TIPS
38
Solar Analog Method
• Adopt V magnitude for Sun as V = -26.76 +/-0.02
(Hayes 1985; Campins et al 1985; Bessel et al 1998)
• Convolve filter/detector/telescope response curves for NIRCAM
with model (Kurucz) A0 star. Define colors of the A0 star to be
0.00.
• Above 2 steps yield fluxes for zero mag for all NIRCAM filters.
• Convolve filter/detector/telescope response curves for NIRCAM
with solar spectrum; yields predicted NIRCAM fluxes for solar
analogs (use Colina et al. 1996 solar spectrum)
• Obtain NIRCAM observations of solar analogs in open clusters
(e.g. NGC2420, NGC 6791)
• Do LS fit of predictions vs. observations for AV and distance. If
get good fit and small residuals, you are done. If not, attempt to
determine if problem is with assumptions or with stars.
9/16/2004
NIRCam Calibration, STScI TIPS
39
Stauffer, NIRCam Sci Team Meeting, May 2003
Problems for NIRCAM Usage of
Solar Analog Method
• NIRCAM saturation at K ~ 15 mag
• Traditional application of method relies on identifying (field)
stars with spectra (or Teff/log g) approx. identical to Sun,
using high resolution spectra and optical photometry.
• K > 15 limit precludes traditional selection method.
• Even with alternate selection technique, K > 15 limit very
likely means standards will have non-zero reddening, poorly
known distance and possibly poorly known metallicity
• Proposed solution = use Solar Analogs in Open Clusters
9/16/2004
NIRCam Calibration, STScI TIPS
40
Stauffer, NIRCam Sci Team Meeting, May 2003
SPACE
TELESCOPE
SCIENCE
INSTITUTE
Operated for NASA by AURA
The Aug 3rd STIS Failure and Upcoming Tests
Paul Goudfrooij
•
Disclaimer: Only ‘Public Domain’ info shown here
•
FRB presentation to HSTP will occur 1:30 – 3:30 today
–
•
STScI Members of FRB: Ron Pitts, Tom Wheeler;
Tony Keyes ex officio
Final info from FRB studies to be shown in later TIPS.
FRB Charter
1.
2.
3.
4.
5.
6.
Review Data: Review telemetry of the failure, and the record of events in the
STIS microprocessor memory log, construct a detailed timeline/ reconfirm
and/or update what has been learned since the August 3rd event;
Identify Most Likely Cause: Develop a complete fault tree identifying potential
causes of the August 3rd anomalies; if possible identify the root cause;
Propose Test Plan/Establish if STIS can be returned to use: Develop a plan
for diagnostic tests that will further characterize the problem and/or establish
conclusively whether STIS can be returned to use or is unrecoverable; identify
the risks presented by each test;
Consider risk of identical failure in additional HST assets: Consider, and, if
needed recommend a set of actions for assessing the susceptibility of other
HST Science Instruments (SIs) to a similar root failure mechanism;
Review thoroughness of SI safing routines: Review the self-checks and safing
architectures of the other SIs for adequacy, and, if needed, recommend
changes having high merit;
Report findings and Recommendations: Document and report the Review
Board’s conclusions.
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
2
“Home” Mechanism Configuration
(situation prior to suspend event)
Mechanism
External Shutter
Corrector Mechanism (Not initialized)
Focus
U Tip/Tilt
V Tip/Tilt
Slit wheel *
Mode Select Mechanism
Mode Isolation Shutter
Echelle Blocker
Calibration Insertion Mechanism
CCD Shutter *
Mnemonic
OXSHP
Position
Closed
OKMFOCP
0.1837134 mm
OKUTILTP
-900.0 a-s
OKVTILTP
-900.0 a-s
OSWABSP
3824311 – 3824372#
(MIRVIS, CCD imaging)
OSMPOSX
Closed
OSEPOSX
Block2
OCMMPOSX
Insert
OSCSHUTX
Closed
* All motors are stepper motors with magnetic detents except the slit wheel and CCD shutter. The latter two are brushless
DC torque motors.
# The slit wheel does not normally move unless commanded to do so. The loss of the +5V mech converter voltage
affected the servo loop permitting drift. 3824311 was the value when the mech 5 V went to zero. 3824372 was the
value at the suspend at 2004.216:16:38:58.
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
3
Observables during Anomaly
•
No STIS stored commanding during anomalous events.
– OMBMC5V (STIS +5V Mechanism voltage) drops to 0V
ÿ No suspend reaction, since no lower bound in FSW limit check !
– Increase in Current & Total Power ~43 minutes after
OMBMC5V dropped to 0V
– MCE1 and MCE2 serial communication with MEB halts
resulting in execution of STIS suspend sequence
•
No evidence of outgassing or temp increase during event
– No temp sensor on LVPS2, but MEB temp sensors did not
show change between loss of +5V and suspend sequence
– No rise in pressure measured by ESM pressure sensor
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
4
STIS Current around Anomaly
NSSC-I
Safing
Limit set to
9.67 Amps
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
5
Overlay
Current
signatures taken
24 hours apart
TIPS Presentation
“normal”
Sep 16, 2004
Paul Goudfrooij
6
Main Bus
Current
During
Fault
Main Bus Current during fault
MAMAs, CEB, Mech and
Cal OFF within 500ms
77
No large current spike captured
at 100ms sample rate
76
MCE drops out
CLDBUSCP
75
16:38:22.841
1 Amp +/- 0.6 Amp
drop in current prior
to Suspend Sequence
Execution
74
73
16:38:21.341
72
SUSPEND sequence
Starts 16:38:22.000
71
16:38:23.041
70
08/03/2004
16:38:12.480
TIPS Presentation
08/03/2004
16:38:15.072
08/03/2004
16:38:17.664
08/03/2004
16:38:20.256
Sep 16, 2004
08/03/2004
16:38:22.848
08/03/2004
16:38:25.440
Paul Goudfrooij
08/03/2004
16:38:28.032
7
Cause & Effect Theory
1. Interpoint +5V converter (MFL2805S) internally fails (at bus voltage
< 28V) causing +5V output to fall to 0V
– No observed change in current at time of failure (< 100 mA)
2. At bus voltage >28V, MFL2805S current input becomes increasingly
exponential
3. Current in excess of 72 Amps in less than 40ms occurs, causing
STIS bus voltage to drop to or beyond point required to reset MAMA
electronics prior to fault clearing
4. Both MAMA electronics proceed through power on reset phase,
halting communications with MEB in process
5. MEB requests Suspend activity; meanwhile, exponential current rise
fault has already cleared in MFL2805S converter; likely component
failure within MFL2805S
6. STIS Suspend is executed; MFL2805S is inhibited
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
8
Proposed On-Orbit Tests
•
Test #1: STIS Checkout
–
•
Test #2: Attempt to Enable +5V Mechanism Converter
–
•
Purpose: Determine if failure still exists
Test #3: Attempt to reactivate Side-1 (“Hail Mary”)
–
•
Purpose: Verify health & viability of STIS and its detectors
Purpose: Determine whether short still exists
Estimated development time needed before tests #1
and/or #2 can be executed:
–
7-9 weeks after getting go-ahead
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
9
Test #1 (STIS Checkout)
•
Test #1 - STIS Checkout (verify health and viability)
–
–
–
–
–
–
Transition from Safe mode to hybrid Operate Mode (no
mechanism initialized)
Enable each detector separately and take series of DARKs (+
BIASes for CCD) to assess detector performance.
Enable each calibration lamp.
Place STIS back in Safe Mode, and start analyzing data &
telemetry
Estimated execution time ~24 hours, no impact to other SI
observing schedule
Note: STIS was already in similar mode (suspend) for 4 days after
failure without any noted anomalies. Hence extremely low risk of
clearing fuse.
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
10
Test #2: Enable +5V Mech
Converter
•
Test #2- Enable +5 volt Mechanism Converter
–
–
Transition from Safe mode to hybrid Operate Mode (no
mechanism initialized) in real-time commanding.
Enable Side-2 Mech Power (similar test to STIS Side-1 failure).
ÿ
ÿ
ÿ
ÿ
ÿ
ÿ
ÿ
–
Activate HST486 ACR to monitor PDU current (shut off if current
exceed expected value plus a delta).
Start high-rate telemetry collection.
Start internal STIS high rate diagnostic on +5volt, +30volt, +15volt,
and other telemetry (TBD) of SES collected items.
Enable STIS Side-2 mechanism relay
Start series of Mechanism moves (clear optical path to enable
observations).
Disable STIS Side-2 mechanism relay.
Dump diagnostic data and place STIS back in Safe Mode.
Note: If bus A/B fuse already stressed, fault might clear fuse,
leaving STIS unpowered.
(Fuse stress rendered unlikely)
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
11
Impact of Fuse Clearing
•
•
STIS Side 1 presently powered off at HOLD relay
– Side-1 Survival Heaters can not be utilized
If STIS Side-2 testing were to interrupt 20 Amp PDU#1 fuse
– Isolation to side-2 Bus-C Fuse would be major impact to HST
ÿ
ÿ
–
Following STIS items would be at high risk
ÿ
ÿ
ÿ
–
Other SIs would have to switch to side-2 as well, single-fused
Bus-C only 35 Amps of fusing to PCU instead of 70 Amps
MAMAs:
Optical Bench:
Mechanisms:
Survival Limit –5C
Survival Limit –10C
Survival Limit –10C
Hence any robotic STIS servicing may not be useful anymore
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
12
Test #3: Side-1 Reactivation
•
•
Same test as during June 2001: Close Hold Relay
(Fuses were replaced during SM3B)
Why?
– No comparable spectroscopic capability in space at present
– STIS offers unique capabilities that will not be replaced by COS
– HST is thinly instrumented now (before addition of WFC3 and
COS), with minimal spectroscopic capability;
– STIS was regularly scheduled for 25-30% of HST time
– STIS performance would be better now than after SM4:
ÿ
ÿ
ÿ
ÿ
Degradation of the CCD detector with radiation exposure
Increasing throughput losses in the UV due to contamination
Increases in the dark current levels of the MAMA detectors
NOTE: these effects should not be drastic; definitely still worth
repairing STIS in the robotic mission!!
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
13
Test Results Prediction
•
Test #1: STIS Side 2 except Mech power supply
–
–
•
Test #2: STIS Side 2 Mech supply
–
–
•
PDU fuse will remain intact
All STIS side-2 systems tested will be 100% functional
PDU fuse will remain intact
+5V Mech voltage will not be present; no mechanism
movement will be accomplished
Test #3: STIS Side 1 Test
–
PDU STIS Side-1 20 Amp fuse (connected to HST A/B bus)
will blow upon closure of STIS HOLD relay
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
14
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
15
Fusing Lay-Out
TIPS Presentation
Sep 16, 2004
Paul Goudfrooij
16
Duccio Macchetto
TIPS, September 2004
STIS PROGRAMS REVIEW
• If STIS cannot be recovered, STIS programs cannot be
executed. [!!!]
• We have reviewed all the STIS programs
– Can a substantial [~90%] fraction of the science as proposed
be accomplished with another instrument [typically ACS
imaging or grism spectroscopy]?
• Three different groups looked at the programs
– INS [Paul &Co]
– Rodger
– SPD [Bob, Mike, Claus, Neill & Duccio]
2
STIS PROGRAMS REVIEW
• The reviews were done independently
• We took a conservative approach but found only ~18
programs out of ~104 Cycle 10,11,12 &13 where, we
believe, a switch would be successful
3
STIS LETTERS
• Letters were sent to the affected PIs
– Says that program cannot be executed
– Tells PIs that they can request a change of SI if they can prove that the
original scientific objectives can be met
– The TTRB [suitably augmented] will review the change requests
• For those programs that we believe can be switched,
INS has sent an additional letter telling them to
formally request the change
• In all cases the burden of proof is with the Pis
• The TTRB will review the request and make the
recommendation in each case
• The overall procedure has been discussed with STUC,
STIC and TAC Chair
4
Replacement Programs
• TAC Selected proposals with the explicit
understanding that the scientific objectives were to be
substantially accomplished with the instrument [s]
identified in the proposal
• To ensure that we would have a pool of good
proposals to carry-out in case of an instrument
malfunction, the TAC was instructed to grade
proposals all the way down to the “triage’ line.
• They were also asked to identify a line below which
we should not implement proposals even if time was
available
5
Replacement Programs
• The STIS orbits that cannot be executed [Cycles 10-13]
are ~ 1100
– Assuming that ~200 orbits can be switched
• We have identified replacement Cycle 13 proposals
[non STIS] following the already defined Panels/TAC
ranking
• The list [~40-45 programs] is being discussed with the
TAC Chair
• Proposals selected are still ~in the top quartile
• Proposers will be informed by late September.
6
Original Cycle 13 Orbits by Sci Cat
SS
2%
SP
11%
AGN
6%
COS
14%
SF
10%
QAL
9%
ISM
10%
Final Mix of Proposals for Orbits by Sci Cat
HS
11%
CS
2%
SS
2%
GAL
25%
AGN
8%
SP
18%
COS
25%
SF
9%
ISM
7%
QAL
0%
HS
7%
7
CS
1%
GAL
23%
Institutional Acceptance Rate
100%
Cycle 13
90%
W/O STIS
New Props
80%
70%
60%
50%
40%
30%
20%
10%
0%
Yale
UCLA
U. of Washington
U. of Texas at Austin
U. of Pittsburgh
U. of Pennsylvania
U. of Michigan
U. of Kentucky
U. of Colorado at Boulder
Caltech
Carnegie Institution of Washington
JHU
JPL
Northwestern
Ohio State
Penn State
SAO
Southwest Research Institute
STScI
U. of Arizona
U. of California - Berkeley
U. of California - San Diego
8
Orbit Increase/Decrease from Original Cycle 13 Allocation
250%
200%
Yale
UCLA
U. of Washington
U. of Texas at Austin
U. of Pittsburgh
U. of Pennsylvania
U. of Michigan
U. of Kentucky
U. of Colorado at Boulder
U. of California - San Diego
U. of California - Berkeley
U. of Arizona
STScI
9
-100%
-56%
-56%
-100% -13%
Southwest Research Institute
SAO
Penn State
Ohio State
-56%
Caltech
Carnegie Institution of Washington
JHU
JPL
Northwestern
-53% -24%
0%
0%
0%
0%
8% 11%
-54%
-150%
78%
76%
-100%-100%
-100%
100%
100%
-40%
-50%
206%
191%
150%
50%
Final Mix of Proposals by Orbit Bins
70
60
Cycle 13 Original Mix
Gained Props
Final Props
59
53
# of Proposals
50
46
43
40
30
27
21
20
14
11
10
10
5
5
7
8
7
4
1
3
3
3
4
2
0
1 - 10
11 - 20
21 - 30
31 - 40
Orbit Bins
41 - 50
51 - 99
>=100
10
Final Mix of Proposals by Orbit Bins
1200
Cycle 13 Original Mix
Gained Orbits
Final Orbits
1000
Orbits
800
600
400
200
0
1 - 10
11 - 20
21 - 30
31 - 40
Orbit Bins
41 - 50
51 - 99
>=100
11