TIPS/JIM
November 17, 2011
Agenda:
INS Division News (Danny Lennon)
JWST Status (Massimo Stiavelli)!
The New WFC3/UVIS Flats (Jennifer Mack)!
The COS FUV Lifetime Adjustment Plan (Alessandra Aloisi)!
Bias and Dark Calibration of ACS/WFC Data Post-SM4 Automated
Pipeline (Pey-Lian Lim)!
!
Next TIPS/JIM: December 15, 2011
INS News Staffing:
John Debes (ESA/AURA) has joined the COS/STIS team.
Miscellaneous:
The INS picnic will be held on Saturday, October 15th at Oregon Ridge Park
HST:
Instrument teams are in the process of seeking MO approval for C19 calibration proposals.
...and in reviewing C19 proposals. Planning windows are out.
SSR1 anomaly - corrected - no data lost!
JWST:
Webinar set for Sep 21st at 2pm. Access for STScI staff available in the auditorium.
..see Massimo's talk.
TIPS/JIM
November 17, 2011
Agenda:
INS Division News (Danny Lennon)
JWST Status (Massimo Stiavelli)!
The New WFC3/UVIS Flats (Jennifer Mack)!
The COS FUV Lifetime Adjustment Plan (Alessandra Aloisi)!
Bias and Dark Calibration of ACS/WFC Data Post-SM4 Automated
Pipeline (Pey-Lian Lim)!
!
Next TIPS/JIM: December 15, 2011
JWST Status
Massimo Stiavelli, November 17th,
2011
Space Telescope Science Institute
Agenda




Health chart
Mission Progress
STScI Progress
Funding Status
J
A S
STScI Health chart for JWST activities – October 2011
Science Technical Schedule Budget
Modes proposal negotiations were completed and the contract modification approved.
This modification brings the Science and Operations Contract baseline in line with a June
2014 Launch Readiness Date. Actual expenditures in FY11 did under-run the budget by
slightly resulting from difficulty filling new vacancies, caused in part by the Congressional
action of zeroing out the FY12 budget.
The staffing challenge is so far having a minor impact on the near term work but delays the
planned start on new functionality. Integration of the WFS&C system software was delayed
by slips in Ball deliveries but was ultimately completed ahead of schedule by assigning
additional resources. Delays in Science Instruments and ISIM flight software are
constraining on-board script completion but ISIM I&T has recognized the interdependency
of the on-board scripts and ISIM – rational schedule schedule discussion has ensued.
Continuing good technical progress. MIRI On-Board Scripts were released for a dry run of
MIRI/ISIM tests. The Wave Front Executive passed its internal acceptance test and was
successfully integrated with the Ball WFS&C software. The Proposal and Planning
Subsystem successfully completed its 3rd System Design Review (SDR) at the end of
October. Data Management Subsystem is preparing for their SDR 1, and designing their
initial prototype processing pipeline.
Hosted Science Working Group Meeting at STScI, incl. presentation on the I&T archive.
Developed plan for revising science white papers including authors outside the SWG.
Continued to track Science System Engineering issues – created or participated in ad hoc
groups as required.
Note – Budget and Schedule reflect expectation that a budget profile consistent with the
Launch Readiness Date October 2018 will be formalized. nominal
moderate problem, action plan identified
major problem, no solution yet
risk decreasing
no change
risk increasing
Schedule Milestones 
Completed three HQ tracked Project milestones
Milestone
Due Completed
Prototype Exposure Time
Calculators
June 2011
May 9, 2011*
WaveFront Software
Subsystem Integration
November 2011
September 27, 2011**
Proposal & Planning
Subsystem Design Review 3
November 2011
October 31- November 1
Data Management
Subsystem Design Review 1
December 2011
Planned for December 6
* Objective was to release in advance of the Frontier Science
Opportunities Workshop, June 6-8.
** Early completion resulted from mitigation actions to address a late
start to WAS, MCS & WEx integration. Mission Progress

Continuing verification of primary mirror segments.
Mission Progress


Continuing verification of primary mirror segments.
Continued progress on ground testing preparations.
Mission Progress



Continuing verification of primary mirror segments.
Continued progress on ground testing preparations.
Fine Guidance Image motion.


Compression


When it was found out that compression didnʼt work as planned a second
daily DSN contact was added to the plan. However, we were still hoping to
make compression work thanks to a workaround identified by John Isaacs.
This would have given extra margin on data volume, made it easier to
schedule high data volume observations such as transits and possibly
enabled science parallels. Unfortunately, a bug in the compression has
been identified that may make it unusable unless the boards are changed.
Fabrication continues (mostly) as planned. Some instrument
delays but ISIM has a lot of schedule margin.
Due to star tracker struts. Evaluating impacts and possible remedies.
Progress at STScI

Proposal Planning System 

Held and passed SDR3 review, last of the series.
Commanding

Continuing progress with script implementation
Script Implementation Status
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Progress at STScI

Proposal Planning System 

Commanding


Portable Spacecraft Simulator (PSS) installed
WIT




Continuing progress with script implementation
JWST I&T ramping up


Held and passed SDR3 review, last of the series.
Finalizing report on JWST overheads (Karl Gordon)
Completed report on MIRI dark current analysis (from FM)
FGS testing revealed some guide star acquisition issues
Telescope


Following actuator gear-motor rework.
Work on MIMF and alternative techniques.
Community Outreach
JWST Full Scale Model at Maryland Science Center (left)
A small Lego™ model of JWST (right), built by kids at the MSCʼs Education Tent (right).
 Also participation at DPS
Funding status




Mini-bus incl. full JWST funding passed by
Senate.
House Senate-Conference gone well
Waiting for full vote on conference bill by
House and Senate Update: this happened Thursday. Bill signed
by President on Friday
}$7.998 total construction cost
TIPS/JIM
November 17, 2011
Agenda:
INS Division News (Danny Lennon)
JWST Status (Massimo Stiavelli)!
The New WFC3/UVIS Flats (Jennifer Mack)!
The COS FUV Lifetime Adjustment Plan (Alessandra Aloisi)!
Bias and Dark Calibration of ACS/WFC Data Post-SM4 Automated
Pipeline (Pey-Lian Lim)!
!
Next TIPS/JIM: December 15, 2011
WFC3/UVIS Flats
(TIPS Nov 17, 2011)
J. Mack
http://www.stsci.edu/hst/wfc3/analysis/uvis_flats
KEY PLAYERS:
–  Elena Sabbi
–  Jennifer Mack
–  Tomas Dahlen
Other contributors:
Peter McCullough – UVIS window ghost model
Cheryl Pavlovsky – UVIS earth flats
Jason Kalirai –
Photometric Zeropoints
Abhijith Rajan –
Photometric Stepping
Alex Viana –
Aperture correction
Terminology
• LP-flat - detector response correction image, incl. both pix-to-pix sensitivity and low-freq modulations
  obtained from uniform illumination via the CASTLE stimulus during TV3
  high signal-to-noise gives pixel-to-pixel response
• L-flat - low-frequency correction to detector sensitivity, due to differences in-flight versus ground
  Stellar L-flat - residuals derived from stepping stars across detector
  Sky flat - residuals from many co-added observations of sparse fields with sources masked
  Earth flat - observations of the bright Earth limb
• Internal flat – flat fields obtained with the internal cal subsystem; used to monitor pixel-to-pixel changes
CASTLE Flats (TV3: 2008)
STIMULUS = D2
(λ < 300 nm)
Xe
(300 nm < λ < 531nm)
Xe, QTH
λ > 600 nm)
UV flats obtained warm (-49C vs -82C)
F225W
F438W
F606W
F814W
F850LP
F953N
L-flat Calibration
•  TV3 flats --> pixel-to-pixel sensitivity
•  In-flight, look for low-frequency residuals
by dithering sources across detector
•
•
•
9
dither
posi-ons,
40 steps
10
broadband
filters
Mul-ple
cycles

varying
roll
angles
SMOV (prop 11452) – 12 orbits (Kim-Quijano)
Cycle 17 (prop 11911) – 30 orbits (Sabbi)
Cycle 18 (prop 12339) – 14 orbits (Sabbi)
Matrix Solution Algorithm
Developed for ACS by R. van der Marel (ISR 2003-10)
•  Computes low-freq variations using apparent brightness vs position
•  Solution is an over-determined matrix equation with a unique min chi2 solution
•  Optimal order of fit determined by density of stars and # observations
2‐D
Legendre
Polynomials
Advantage:
Cohesive structures are well represented
Disadvantage: Cannot describe intermediate frequencies unless use high order
High order fits cause large excursions near detector edges
Chess
Board Basis
Func-ons
Advantage:
Detector is a pixelated version of the detector with indep soln’s
Disadvantage: Grid regions with few stars can lead to large fluctuations
TV3, Earth flat, and L-flat
Earth Flat
(flatcorr=OFF)
TV3 flat
F606W
Pavlovsky
& McCullough
Earth Flat
(flatcorr=ON)
1.000
0.9976
Residual = Lflat
(quad-dep gain)
Stellar Lflat inverse wedge
Wedge is a reflection ghost
1.0198
1.0124
  For sparse fields & local bkg subtraction, FLARE must be removed.
  For very bright extended sources, the FLARE should not be removed.
The UVIS Flare
We can model the FLARE with the matrix algorithm, however:
1) The edges of the flare are too sharp to be properly modeled;
2) The grid solution is smoothed to remove the pixelization.
Instead, use TV3 data to develop a geometric model…
Geometric Model
McCullough WFC3 ISR 2011-16
The flare in the TV3 flats is due to
4 ghost reflections between the
detector and the front and back
surfaces of the 2 detector windows.
The incident beam expands
to form 4 defocused ellipses
•  Sum of TV3 data with grid of sources in quad D
•  Geometric model of the 4 ghost reflections
•  Generates ghost ellipses in a wedge to the upper left.
•  Generated by projecting the 4 defocused ellipses created
from the reflections between the 2 glass windows
VIS Flats
Numerical Model of Window Ghosts (Peter)
VIS Flats
Numerical Model of Window Ghosts (Peter)
Alpha Release
March 2011
  7 filters available on WFC3 website
  Flare removed, 32x32 L-flat grid solutions (clipped, smoothed)
  Based on r=5 pixel aperture photometry (crowding)
  Flare Intensity with wavelength adjusted by eye
Blue means that the TV3 flats will make the stars too faint.
F336W
F390W
F438W
0.98
0.99
F555W
1.00
F606W
1.01
F775W
1.02
F814W
Verification
Cycle 17 Zerpoints CAL program (Kalirai)
  observed standards in the corners of Amp A & C
  measured chip-to-chip differences in TV3 vs alpha flats
F336W Spatial Stability Test (Kalirai & Rajan)
  stepping one standard in an 8x6 grid over the detector
  phot with r=10 gives +/-1% deviations
using alpha-release flats based on r=5 phot
F606W L-flat versus aperture
•
•
•
R=4
L-flat computed in variety of apertures in DRZ frames
Alpha-release r=5 pixels chosen to optimize S/N in crowded field
Larger aperture solutions get noisier but seem to converge at r=10
R=5
0.98
R=6
0.99
1.00
R=9
1.01
1.02
R= 10
(R=5 plus apcor)
PSF Variability
Bellini WFC3 code
(based on Anderson s ACS code)
Computed for each image in a 10x9 grid
(super-sampled x4)
R=5 to 10 Apcorr
F336W
-0.07 mag .. -0.04 mag
EE curves for all 90 regions
Variations are sub-1% beyond ~8 pixels
EE curves change from exposure to exposure
(different parts of the breathing curve)
F336W images in a sequence
APERTURE CORRECTION (R=5 to 10)
-0.04 mag
Focus Model
-0.05 mag
-0.06 mag
-0.07 mag
Time variability of MEDIAN ~0.3%
Alpha vs Pipeline Release
 Correcting photometry to 10 pixels reveals the wavelength dependence of L-flat
Blue indicates that the TV3 flats will make stars too faint.
R=5 L-flats (Alpha Release, Mar 2011)
F336W
F390W
F438W
F555W
F606W
F775W
R=‘10’ L-flats (Pipeline Release, Aug 2011)
0.98
0.99
1.00
1.01
1.02
F814W
Verification
2 images rotated 180 degrees
TV3
Alpha (r=5)
Pipeline (r= 10 )
Verification
F336W Spatial Stability Test (Rajan)
Accuracy is now sub-1%
Verification
Earth Flats (Pavlovsky)
F606W
R= 10
Lflat
Earth flat /
TV3 flat
Tricky Cases: UV Flats
(not yet in pipeline)
ISR 2008-46: Sabbi et al.
•  Count rates for Chip 1 (solid) and Chip 2 (dashed).
•  F218W, F225W, and F275W were obtained warm.
•  The QE offset decreases with increasing wavelength
F225W L-flat has residual QE offset ~1.5%
F225W
F225W (scaled)
F275W
Tricky Cases: F850LP
(not yet in pipeline)
Pivot wavelength 917nm
Detector becomes transparent at 1 micron
Black = glue = low QE in flat
32x32 grid may not fall along glue strips
Good Candidate for Spatial Scan
Tricky Cases: F850LP
(not yet in pipeline)
CASTLE QTH Mirror VISIR
INTFLAT Tungsten
Ratio
Color of the stimulus
causes the residuals in
the vertical 'glue' features
(~0.5-1.0%)
32x32
L-flat from Omega-Cen
Glue shows up as ~1% features
Stars are BLUER than the lamps
16x16
8x8
Ratio New Flats / TV3 Flats
Blue indicates that the TV3 flats will make stars too faint.
Peak-to-peak = 0.035-0.055 mag, rms = 0.006-0.013 mag
To ensure the accuracy of their flat fielding,
users are STRONGLY encouraged
to apply local aperture corrections to 0.4
Max difference in photometry (mag)
F225W
F275W
F390W
F438W
0.99
F555W
F775W
F606W
0.98
F336W
1.00
1.01
F814W
1.02
1.03
1.04
Filter
Full
frame
Center
3K x 3K
F225W
0.030
0.027
F275W
0.042
0.037
F336W
0.029
0.013
F390W
0.034
0.019
F438W
0.041
0.019
F555W
0.032
0.024
F606W
0.036
0.026
F775W
0.037
0.022
F814W
0.037
0.031
F850LP
0.057
0.051
Summary
  New UVIS flat fields have been constructed for 10 broad band filters
  Solutions include 4 main components:




Geometric model of ghost reflection
Low frequency residuals from dithered observations of Omega Cen
Chip offsets (QE) and amp offsets (gain)
Spatially-varying aperture corrections
  Flats for remaining 32 full frame filters are constructed via wavelength interpolation
Strong wavelength dependence of the suggests that interpolation is a valid method
  Delivery to CDBS by the end of the month, pending final verification testing
  Zeropoints to be recomputed using new flats (Kalirai/Rajan)
  Additional verification in Cycle 19
Cycle 19 Flat field Programs
12706 - UVIS Window Ghosts
(Mack)
  Measure the relative strength of the window ghosts in ~20 filters
12707  - UVIS Spatial Sensitivity
(Rajan)
  Verify the L-flat by stepping a spectrophotometric standard across the detector (50 positions, 4 filters)
12709 - UVIS & IR Moonlit Flats
(Pavlovsky)
  Observe the moonlit earth to validate the L-flat correction at visible and IR wavelengths
12710 - UVIS Bright Earth Flats
(Mack)
  Observe the bright Earth to validate the L-flat correction for the UV filters
12713 - Spatial Scanned L-flat
(McCullough)
  Validate the L-flat correction by spatially scanning a star back and forth across the detector in 7 filters
UVIS Flare
Program 12706 – Executed Oct 21, 2011 (1 orbit)
Calibration Strategy:
Short narrowband exposure exposure to measure source brightness
Long (saturated) broadband exposure to measure strength of each ghost
Ghosts 3 & 4
Ghosts 1 & 2
5.) Structure appears sharper in narrower bandpasses
TIPS/JIM
November 17, 2011
Agenda:
INS Division News (Danny Lennon)
JWST Status (Massimo Stiavelli)!
The New WFC3/UVIS Flats (Jennifer Mack)!
The COS FUV Lifetime Adjustment Plan (Alessandra Aloisi)!
Bias and Dark Calibration of ACS/WFC Data Post-SM4 Automated
Pipeline (Pey-Lian Lim)!
!
Next TIPS/JIM: December 15, 2011
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&#%()5+''"#)*,)'#-#M-*()+&)f)M*((#$8*&'$)-*)
&*5+&%")8*$+N*&),*()$M+#&M#)*G$#(A%N*&$)
0-.#()A+$+G"#)$-(+8#)%(*9&')fg^IIL^_I),(*5)
$8#M-(%)*,)7%A#"#&O-.)M%"+G(%N*&)"%58)
R#(NM%")$-(+8#$),(*5)G(+O.-)O#*M*(*&%")KUh)"+&#$)
–  ),9""U)+58"#5#&-#')+&-*)-.#)8+8#"+&#)7+-.)0>Q1)
G9+"')HIDI;`)
Gain sag holes
•
•
–
Red: PHA = [4,30] Blue: PHA = [2,30]
BlueTD^I<2D_EE)'%-%),(*5)8(*O(%5)DH`H`))))))))))))))
! PHA=[2,30]
Red ! PHA=[4,30]
6$#&$+NA+-U)5*&+-*(+&OC)*G-%+&#'))
G160M/1577 data from program 12424, obtained on
*&):#M)HH=)HIDI)
Dec 22nd 2010.
–
–
$##&)+&)5%+&)$8#M-(%")(#O+*&=)G9-)%"$*)%G*A#)%&')
G#"*7)6-.#)"%@#(),(*5)-.#)%8#(-9(#=)>1!)*()a0!=)
-.%-)+$)&*-)+&)9$#),*()$M+#&M#)*G$#(A%N*&$C)
`)*&)$#O5#&-)!))6*&#),*()#%M.)*,)-.#)`)P>L>01)
$#i&O$)*,)TD`IK2DDI_C)
HI)*&)$#O5#&-)a)6*&#),*()#%M.)*,)-.#)`)P>L>01)
$#i&O$)*,)-.#)_)TDYI<)$#i&O$C)
%<>44F;,4H#<4,>6$;,<#C.>6$
•
>X!)G+&)
)
34>1)<##N&O)
Y)
;,4H#<4,>6$;,<#C.>6$
DD2DE2HIDD)
34>1)<##N&O)
`)
+>C9.>6$>-$0,<E8>?$+,6#4$-<>/$GPROS$'#T6E$$
>6$%&'$()*$'#E/#65$U$
S>198$G9,6$I4K$!,/#$,6$'#E/#65$U$
Higher HV, SMOV
Lower HV, SMOV
Feb 2011, before
HV increase
End Sep 2011
Mar 2011, after
HV increase
•  <*'%")O%+&)A$;)WL8+W#")8*$+N*&)*&)-.#)'#-#M-*()+&)%)DILGUL^)6+&)W)%&')UC)8+W#")7+'#)(#O+*&)7.#(#)$8#M-(%),%"")
•  :%-%),(*5)M959"%NA#)+5%O#$)%-)'+Z#(#&-)*8#(%N*&%")XR)A%"9#$)%&')#8*M.$)%(#)8(#$#&-#')
•  P+O9(#)(#8(#$#&-)(#$-(+M-#')U)%(#%)*&)'#-#M-*(=)5*'%")O%+&)'+$-(+G9N*&)A%(+#$)%"$*)7+-.)U)))
•  <*'%")O%+&)'(*8$)#A#(U7.#(#)7+-.)N5#)7.#(#)jM*&N&995k)*,)-.#)$8#M-(%),%""$)
•  <*'%")O%+&)'(*8$)#A#&)5*(#)+&)(#O+*&$)7.#(#)O#*M*(*&%")KUh),%""$)+&)TDYI<2TD`IK)$#i&O$=)-.#)$*LM%""#')j.*"#$k))
•  <*'%")O%+&)g)Y)6'*@#')"+&#C)+$)%)G#&M.5%(\),*()-.#)*&$#-)*,)$#A#(#)O%+&L$%O)#Z#M-$))
•  XR)+&M(#%$#')+&)1#O5#&-)a)6<%()HIDDCV)5*'%")O%+&)+&M(#%$#')GU)l)Y)>X!)G+&$)6l)D)U#%()*,)"+,#N5#)O%+&#'),*()-.#)$#O5#&-C)
•  P+($-)j.*"#k)(#"%-#')-*)O#*M*(*&%")KUh)*G$#(A%N*&$)+&)TDYI<2DHmD)%88#%(#')+&)n9")HIDD)
DD2DE2HIDD)
34>1)<##N&O)
_)
DD2DE2HIDD)
^)
$$%&'$()*$G9,6F'9E$VW#C54$
S>198$G9,6$I4K$!,/#$,6$'#E/#65$0$
•
Higher HV, SMOV
34>1)<##N&O)
0&M#)5*'%")O%+&)(#%M.#$)l)Y=),(%MN*&)*,)M*9&-$)"*$-)+$)l)_d)
–  M*58%(%G"#)-*)9&M#(-%+&N#$)+&)-.#)%G$*"9-#)o9W)M%"+G(%N*&)6l)YL_)dC)
–  M*58%(%G"#)-*)8+W#"L-*L8+W#")A%(+%N*&$)'9#)-*)o%-)b#"')6l)_dC)
Lower HV, SMOV
•
•
•
P(%MN*&)*,)"*$-)M*9&-$)+&M(#%$#$)#W8*&#&N%""U)%$)5*'%")O%+&)'#M(#%$#$)
DIId)"*$$)+$)(#%M.#')%(*9&')%)5*'%")O%+&)*,)l)D;_)
3.#)DIId)"*$$)+$)(#%M.#')*&)%)N5#$M%"#)-.%-)A%(+#$),(*5)*&#)(#O+*&)-*)-.#)*-.#()'#8#&'+&O)*&)
-.#)-*-%")M*9&-$)%MM959"%-#')%$)%),9&MN*&)*,)N5#)
–  +&)'##8#$-)KUh).*"#)-.+$)+$)(#%M.#')+&)YL`)5*&-.$)
–  +&)%)-U8+M%")M*&N&995)(#O+*&)-.+$)+$)(#%M.#')+&)^LE)5*&-.$)
S>198$E9,6$>-$R$,4$E>>1$=#6C"/9<X$-><$>64#5$>-$4#I#<#$E9,6$49E$#W#C54$961$C><<#C.I#$9C.>64$
/345$=#$59X#6$5>$H<#I#65$/>198$E9,6$-<>/$<#9C",6E$5",4$I983#$Y$
End Sep 2011
•  <*'%")O%+&)A$;)WL8+W#")8*$+N*&)*&)-.#)'#-#M-*()+&)%)DILGUL^)6+&)W)%&')UC)8+W#")7+'#)(#O+*&)7.#(#)$8#M-(%),%"")
•  :%-%),(*5)M959"%NA#)+5%O#$)%-)'+Z#(#&-)*8#(%N*&%")XR)A%"9#$)%&')#8*M.$)%(#)8(#$#&-#')
•  P+O9(#)(#8(#$#&-)(#$-(+M-#')U)%(#%)*&)'#-#M-*(=)5*'%")O%+&)'+$-(+G9N*&)A%(+#$)%"$*)7+-.)U)))
•  <*'%")O%+&)'(*8$)#A#(U7.#(#)7+-.)N5#)7.#(#)jM*&N&995k)*,)-.#)$8#M-(%),%""$)
)
)
•  <*'%")O%+&)'(*8$)#A#&)5*(#)+&)(#O+*&$)7.#(#)O#*M*(*&%")KUh),%""$)+&)TDYI<2TD`IK)$#i&O$=)-.#)$*LM%""#')j.*"#$k))
•  <*'%")O%+&)g)Y)6'*@#')"+&#C)+$)%)G#&M.5%(\),*()-.#)*&$#-)*,)$#A#(#)O%+&L$%O)#Z#M-$))
•  XR)&*-)+&M(#%$#')-*)*(+O+&%")1<0R)A%"9#$)+&)<%()HIDD)*&)1#O5#&-)!)
•  jX*"#$k)(#"%-#')-*)O#*M*(*&%")KUh)*G$#(A%N*&$)+&)TD`IK2DDI_)$9''#&"U)%88#%(#')+&)<%U2n9&#)HIDD)
DD2DE2HIDD)
34>1)<##N&O)
E)
DD2DE2HIDD)
Segment B near deepest +Z[$hole at ~ 9000 pixels in dispersion direction:
blue original operational HV
green increased HV
p)
G9,6F'9E$:>8#4$,6$'#E/#65$U$>-$%&'\()*$=Z$0H<$NOPN$$
!,/#8,6#$-><$%&'$()*$G9,6F'9E$VW#C54$
Segment
B
B
B
B
A
B
B
A
A
B
B
A
A
B
B
B
B
B
A
A
B
B
B
B
B
B
B
A
A
B
B
A
B
B
B
B
Cenwave
1291
1309
1327
1318
1105
1300
1327
1105
Continuum
Continuum
1327
Continuum
1105
1291
1291
1309
Continuum
1318
1105
Continuum
1327
1309
1318
Continuum
1318
1291
1309
Continuum
Continuum
1300
1300
Continuum
Continuum
1300
Continuum
Continuum
FP-POS
3
3
3
3
3
3
1
4
X=7000
X=1100
4
X=4500
1
1
4
1
X=3000
1
2
X=1500
2
4
4
X=4900
2
2
2
X=13000
X=11000
2
4
X=15000
X=8500
1
X=12000
X=14000
Days to PH=3
since 1/21/2011
161
208
292
372
425
428
441
446
495
519
536
540
547
575
577
591
601
618
624
628
636
653
671
690
711
719
748
764
787
800
826
826
830
907
1023
1240
G130M settings that will produce these holes
1327
Date
Jul-11
Aug-11
Nov-11
Jan-12
Mar-12
Mar-12
Apr-12
Apr-12
May-12
Jun-12
Jul-12
Jul-12
Jul-12
Aug-12
Aug-12
Sep-12
Sep-12
Sep-12
Oct-12
Oct-12
Oct-12
Nov-12
Nov-12
Dec-12
Jan-13
Jan-13
Feb-13
Feb-13
Mar-13
Apr-13
Apr-13
Apr-13
May-13
Jul-13
Nov-13
Jun-14
1
First gain sag hole
appears in segment B
Rest of 2011
2
1318
3
4
First gain sag hole
appears in segment A
2013
3
1309
4
1
2
3
1300
4
1
2
3
1291
4
1
2
3
4
Effects of Segment B gain sag holes on G160M observations
Continuum effects start
appearing in both segments
•  Table reports dates when
modal gain reaches 3 in
certain regions of the spectra
•  For Segment B estimates are
based on data obtained at
lower HV (before Mar 2011)
but trends at increased HV
are similar
•  For Segment A estimates are
based on data obtained at
current (lower) HV
•  Currently revising the
predictions of our models
based on additional data from
Cycles 18 and 19
2014
2
Detector active area in dispersion direction: ~ 14,000 pixels
Coverage of all G130M settings shown (light blue): ~ 5000 pixels
First half 2012
Second half 2012
1
G160M observations with FP-POS=1,2,3,4 (in wavelength space)
1
2
3
4
What happens to S/N of coadded G160M data on Seg B?
x1dsum with 1 FP-POS (3): S/N = 0 over 500 pix (3.5% of spectrum)
x1dsum with 2 FP-POS (3+4): S/N = 70% over 1000 pix (7% of spectrum)
x1dsum with 3 FP-POS (2+3+4): S/N = 57% over 100 pix and S/N = 81% over 1300 pix (10% of spectrum)
x1dsum with 4 FP-POS (1+2+3+4): S/N = 70% over 200 pix and S/N = 87% over 1600 pix (13% of spectrum)
m)
G9,6F'9EE#1$%>6.633/$,6$'#E/#65$0$$
>-$%&'\()*$=Z$]$^36\^38$NOPN)
VI>83.>6$>-$G9,6F'9EE#1$%>6.633/$$
,6$'#E/#65$0$>-$%&'\()*$
Detector active area in dispersion direction (red + light blue): ~ 14,000 pixels
Continuum area affected by gain sagged (red): ~ 4000 pixels (~ pix 4000 to 8000)
20
Effects of Seg A sagged continuum on G160M observations
•  SA*"9N*&)*,)KU%L$%OO#').*"#$)&*-)$.*7&))
•  >(#'+MN*&$)%$$95#)-(#&'$)%-)M9((#&-)6"*7#(C)XR))
:*$,6C<#94#$5>$><,E,698$'S&*$I983#4$?>381$988>?$34$5>$E9,6$]$P$Z#9<$-><$5",4$4#E/#65$
Segment A
2011-05-05
G160M observations with FP-POS=1,2,3,4 (in wavelength space)
!"#$%&'(%)(*+',(-$+*&.(/01'&+-&("0(23&(
1
2
3
4
0H<$NOPR$
(#=$NOPR$
S9<$NOPR$
S9Z$NOPN$
^38$NOPN$
10
&C5$NOPN$
What happens to S/N of coadded G160M data on Seg A?
x1dsum with 1 FP-POS (1): S/N = 0 over 4000 pix (29% of spectrum)
Modal Gain
15
x1dsum with 2 FP-POS (1+2): S/N = 0 over 3750 pix (27% of spectrum)
5
x1dsum with 3 FP-POS (1+2+3): S/N = 0 over 3500 pix (25% spectrum)
x1dsum with 4 FP-POS (1+2+3+4): S/N = 0 over 3250 pix (23% spectrum)
0
26-May-2011 17:10
DD2DE2HIDD)
5.0•103
X Pixel
34>1)<##N&O)
1.0•104
1.5•104
DH)
VI>83.>6$>-$G9,6F'9EE#1$%>6.633/$$
,6$'#E/#65$U$>-$%&'\()*$
20
G9,6F'9E$VW#C54$>6$%&'$()*$'H#C5<9a$P$
•  SA*"9N*&)*,)KU%L$%OO#').*"#$)&*-)$.*7&))
•  >(#'+MN*&$)%$$95#)-(#&'$)%-)"*7#()XR)G9-)-(#&'$)%-)+&M(#%$#')XR)$+5+"%()
:*$,6C<#94#$5>$><,E,698$'S&*$I983#4$98<#91Z$H#<-></#1$,6$S9<C"$NOPP)
Segment B
•  T%+&)$%O)+&)PQR)'#-#M-*()"#%'$)-*V)
-  "*M%"+e#').*"#$)+&)$8#M-(%))
2011-05-05
•  8(*'9M#')GU)KUh)%+(O"*7)6l)DII)8+W#"$)7+'#)#%M.C)
•  5*$-"U)*&)1#O5#&-)a=)G9-)$*5#)$-%(N&O)-*)%88#%()*&)1#O5#&-)!)
•  5+NO%-#')*8#(%N*&%""U)GU)9$#)*,)59"N8"#)P>L>01)8*$+N*&$)
^36$NOP`$
_>I$NOPR$
S9Z$NOPR$
'#H$NOPN$
^36$NOPN$
Modal Gain
15
;#C$NOPN$
!"#$%&'(%)(*+',(-$+*&.(/01'&+-&("0(23&(
)4#$>-$988$`$(7F7&'$H>4,.>64$#6-><C#1$459<.6E$-<>/$%ZC8#$NO$
-  '#8(#$$+*&)*,)M*&N&995)+&)$*5#)%(#%$)*,)#%M.)$#O5#&-)M*58%(#')-*)*-.#()
&#%(GU)%(#%$)6'9#)-*)$.+[)*,)>X!)'+$-(+G9N*&)-*)"*7#()A%"9#$)7+-.)9$%O#C)
10
•  #Z#M-$)*&)M*&N&995).%(')-*)*A#(M*5#)*8#(%N*&%""U)7+-.)P>L>01)G#M%9$#)
+&A*"A+&O)%)"%(O#),(%MN*&)*,)8+W#"$))$
)
5
5.0•103
0
DD2DE2HIDD)
X Pixel
1.0•104
1.5•104
34>1)<##N&O)
26-May-2011 17:10
DY)
DD2DE2HIDD)
•  4,)-(#&'$),(*5)#%("+#()'%-%)6.+O.#()XR),*()1#O5#&-)aC)M*&N&9#)%&')&*),9(-.#()
%MN*&)+$)-%\#&=)#Z#M-$)*,)O%+&)$%O)'+?M9"-)-*)*A#(M*5#)7+-.+&)l)D)U#%()61#8)
HIDHC)#A#&)7.#&)9$+&O)$#A#(%")P>L>01)8*$+N*&$)
•
-  59"N8"#).*"#$)*&)G*-.)1#O5#&-$)GU)#%("U)!8()HIDH)
-  H_d)*,)M*&N&995)*&)1#O5#&-)!)$#A#(#"U)%Z#M-#')GU)#&')*,)n9&)HIDH))))))))))))
6G9-)M9((#&-"U)M*&$+'#(+&O)+&M(#%$+&O)-.#)XR)-*)+&+N%")*&L*(G+-)A%"9#$C)
&68Z$]$N$">3<4$>-$!*$5#4.6E$95$",E"#<$:*L$6>5$C3<<#658Z$H8966,6E$5>$E>$5",4$?9Z$Y)
•
-  D_d)*,)M*&N&995)*&)1#O5#&-)a)$#A#(#"U)%Z#M-#')GU)1#8)HIDH)
•  )q+-.)&*),9(-.#()%MN*&)-%\#&=)7.*"#)$M+#&M#)$8#M-(95)$#A#(#"U)M*58(*5+$#'))))
-  *&)1#O5#&-)!)7+-.+&)H)U#%($)6XR)+&M(#%$#)7*9"')O+A#)l)D)%''+N*&%")U#%(C)
T%+&L$%O)#Z#M-$)%-)M9((#&-)"+,#N5#)8*$+N*&)M%&)G#)5+NO%-#')GU)(%+$+&O)
*8#(%N*&%")XR)*,)H)/01)PQR)$#O5#&-$=)$+5+"%("U)-*)7.%-)'*&#),*()1#O5#&-)
a)+&)<%(M.)HIDDV)
–  /9((#&-"U)M*&$+'#(+&O)(%+$+&O)XR)+&)1#O5#&-)!)-*)A%"9#)+&+N%""U)9$#')+&)1<0R)))))))))))))))))))))))))))))))))
6-%(O#-)'%-#)P#G2<%()HIDHC)
–  4&A#$NO%-#')(%+$+&O)XR)*,)1#O5#&-)a)6%&')#A#&-9%""U)!C)-*)A%"9#$)O(#%-#()-.%&)
-.*$#)%"(#%'U)9$#')*&L*(G+-)
-  b($-).*"#)*&)1#O5#&-)a)%88#%(#')+&)n9")HIDD)
SZ#M-$)*,)O%+&)$%O)M%&)%"$*)G#)5+NO%-#')GU)5*A+&O)-*)&#7)"+,#N5#)8*$+N*&)
–  SW-#&$+A#)8(#8%(%-*(U)7*(\)+&)8(*O(#$$r)&##'$)-*)G#)M*58"#-#')7+-.+&)-.#)&#W-)))
l)^)5*&-.$)*()$*)-*)G#)%G"#)-*)5*A#)-*)%)&#7)"+,#N5#)8*$+N*&)GU)1955#()HIDH)
–  Q8)-*)l)DII)#W-#(&%")6SC)*(G+-$)%&')l)H_)+&-#(&%")64C)*(G+-$)5+O.-)G#)(#s9+(#';))))))))))))))))
3.#$#)*(G+-$).%A#)G##&)*()7+"")G#)9$#'),*(V)
•  8(#8%(%-*(U)7*(\)-*)M.%(%M-#(+e#)%"")&#7)PQR)"+,#N5#)8*$+N*&$)
•  q*(\)-*)#&%G"#2M%"+G(%-#)&#W-)PQR)"+,#N5#)8*$+N*&)-*)9$#),*()$M+#&M#)
•  7*(\)-*)#&%G"#2M%"+G(%-#)$M+#&M#)%-)FQR)*ZL&*5+&%")8*$+N*&$)6+,)&##'#'C)&*-)U#-)
+&M"9'#')6%''+N*&%")l)^I)S)%&')l)DI)4)*(G+-$C)
-  *&)1#O5#&-)a)7+-.+&)Y)U#%($)
06$9C.>6$>-$4>/#$X,61$,4$<#b3,<#1$5>$/,.E95#$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$
4#I#<#$E9,6F49E$#W#C54$?,5",6$5"#$6#c5$PO$/>65"4$A'#H$NOPNBY$
34>1)<##N&O)
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S,.E9.>6$>-$%&'$()*$G9,6F'9E$VW#C54$
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DD2DE2HIDD)
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%3<<#658Z$?><X,6E$5>?9<14$/>I,6E$5>$6#?$()*$8,-#./#$H>4,.>6$=Z$'3//#<$NOPN$Y$
DD2DE2HIDD)
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%>645<9,654$>6$_3/=#<$>-$$
0I9,89=8#$()*$+,-#./#$7>4,.>64$
%&'$()*$+,-#./#$012345/#65$e><X$
45678(+--93&-(7:;<=(33(>?@(+'1-&1A(-%&B-(C&%D&&0(EFG(H"I&23&(B)-"2)0-J(!"#$%$$$$
&"&%'$"!$($')!*+,*$-".)+"/.J(C9%(3"#$%(C&(0&1&--+'K(%)(1)0-"*&'(B)-"2)0-(3)'&()'(
H&--(1H)-&HK(-B+1&*($
F95G#()*,)%A%+"%G"#)"+,#N5#)8*$+N*&$)7+"")'#8#&')*&)$#A#(%"),%M-*($=)+&M"9'+&OV)
D;
–  3*)G#)M*58"#-#'))!1!>)+&)*('#()-*)$#"#M-)&#W-)8*$+N*&$
!"#4#$9C.I,.#4$?,88$=#$H#<-></#1$>6C#$
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<#M.%&+M%")"+5+-%N*&$)*,)%8#(-9(#)5#M.%&+$5),*()FQR)-%(O#-)%Ms9+$+N*&$))))))))))))))))))))))))
6+;#;=)&95G#()*,)M#(Nb#')%8#(-9(#)5*A#$C)
•  >%-.$)-.%-)%""*7)"%58)%&')#W-#(&%")"+O.-)-*)(#%M.)'#-#M-*()+&)+58(*8#()7%U$)))))))))))))))))))))))))
6#;O;=)%A*+'%&M#)*,)$%b&O)'#-#M-*()#A#&-$)$+5+"%("U)-*)7.%-).%88#&#')+&)8(*O(%5)DHIm^C)
•
•
•
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Bias and Dark Calibration of
ACS/WFC Data: Post-SM4
Automated Pipeline
P. L. Lim
TIPS/JIM, Nov 17, 2011
Before SM4
• ACS ISR 2004-07 (Mutchler et al.)
• ACS TIR 2007-04 (Lucas et al.)
After SM4
• WFC3 TIR 2008-01(Martel et al.; Borders) and
automated MAST retrieval (Viana et al. 2012; in
prep.)
• Refitted for ACS/WFC and manually executed
(Armstrong et al. 2012; in prep.)
• Automated since Sep 2011 (Lim et al. 2012; in
prep.)
New vs. Old
•
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•
Pros
Fast turnaround
New CALACS
No IRAF
Less clunky
Improved codes
Easier to adapt for
new mode or SI
•
•
•
•
Cons
No DSB support
No version control
Shared machine
Uses FTE and disk
space in AWT
Cron Jobs
• Nightly check for new RAW
– Every 2-3 days
• Weekly check for new anneal (Sun)
– 1-2 weeks after each monthly anneal
• Weekly check for the need to organize and create
new reference files (Thu)
– When new anneal is found
– Followed by manual inspection (Armstrong) and
CDBS delivery (McMaster)
Reference Files
• 2 superbias per anneal cycle
• 2 basedark per anneal cycle
• 1 daydark per DATE-OBS
• Basedark + daydark = 1 superdark per
DATE-OBS
Outputs
• Reference files to deliver
• Smoothed images to show underlying pattern
• Plots
– RAW stats by exposure
– Pixel distribution histograms
– Stats and flags over time
– Column profiles for amp jump (superdark only)
• Log files with miscellaneous info
• Error files (on failed execution only)
• Emails with CDBS delivery template
Smoothed Superbias
Smoothed Superdark
Superdark Flags Trends
Future Work
Add subarray superbias support
Publish ACS ISR (Lim et al. 2012; in prep.)
Start delivering DKC files
Maintain compatibility with new CALACS
(Hack et al. 2012; in prep.)
• Add support for CRDS (?)
•
•
•
•
Thank You