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NIRCam Status Marcia Rieke University of Arizona JWST Partner’s Workshop

JWST-PRES-012902. NIRCam Status Marcia Rieke University of Arizona JWST Partner’s Workshop Ottawa, Canada May 19, 2009. Read Noise with ASICs. A set consisted of 30 80-sample ramps. Data taken using development unit ASICs and Qual FPA. How to Use Subarrays.

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NIRCam Status Marcia Rieke University of Arizona JWST Partner’s Workshop

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  1. JWST-PRES-012902 NIRCam Status Marcia Rieke University of Arizona JWST Partner’s Workshop Ottawa, Canada May 19, 2009 JWST Partner's Workshop

  2. Read Noise with ASICs A set consisted of 30 80-sample ramps. Data taken using development unit ASICs and Qual FPA JWST Partner's Workshop

  3. How to Use Subarrays An open question in using the subarray readout mode is whether special calibrations are needed for each subarray location and size or whether data can be extracted from full frame data. • For 2-sample (CDS) data, we may recommend taking darks before the exposure • SCAs run from an ASIC may not have the reset anomaly that we see running in buffered mode w/ a Leach controller • Reference pixels do not provide any benefit. • Again need to be careful about possible ASIC vs Leach or buffered vs unbuffered mode caveats • Flats can be used from full frame data. • no ref pix corr • ref pix corr JWST Partner's Workshop

  4. Illuminated Subarrays NIRCam will use a subarray or “window” readout mode to extend dynamic range. It may be the principal mode for observing transits by extra-solar planets. A 128x128 subarray was used with four SCAs (two shown here) in our test dewar. Illumination was provided by 2micron LED, and a series of 2-sample ramps were taken. Arrays run simultaneously so LED variations are seen in all. JWST Partner's Workshop

  5. Subarray Flatfielding Gray scale and plot show the result of ratioing subarray to full frame data. Neither image was linearity-corrected. The variations of +/-2% agree with expectations from counting statistics. Full frame flats appear to be fine for use with subarrays. JWST Partner's Workshop

  6. Flight Short Wavelength FPAs are in Assembly B4 B4 B2 B2 C043 C044 B1 B1 B3 B3 C038 C045 FM1 Dark (black is good) FM1 Illuminated (white is good) Red box is coronagraphy field. JWST Partner's Workshop

  7. A4 A2 C101 C104 A1 A3 C074 C105 FM2 Dark (black is good) FM2 Illuminated (white is good) Red box is coronagraphy field. JWST Partner's Workshop

  8. Flight Wide Filters • Plot below shows the transmission functions for the flight candidates. Dashed line is the requirement. • Out of band blocking is also excellent. Req. JWST Partner's Workshop

  9. ETU Optic Test Pupil Wheel ConfigFWA ETU Optic Test PW9 – WEAK LENS - 7 PW8 – OUTWARD PINHOLES PW10 – Uncoated Fused Silica PW7 – FILTER SURROGATE PW11 – WEAK LENS - 6 PW6 – DHS MASSSURROGATE PW12 – ETU DHS 2 PW5 – FILTER SURROGATE PW1 – CIRCULAR APERTURE PW4 – FILTER SURROGATE PW2 – FLAT FIELD PINHOLES PW3 – Uncoated Fused Silica JWST Partner's Workshop

  10. ETU Optic Test Filter Wheel ConfigFWA ETU Optic Test FW2 – FILTER SURROGATE FW1 – FILTER SURROGATE FW3 – FILTER F115W FW12 – DHS FILTER F150W2 FW4 – FILTER F070W FW11 – FILTERF070 FW5 – FILTER F200W FW10 – FILTER SURROGATE FW6 – FILTER F212N FW9 – IMAGING PUPIL FW7 – WEAK LENS - 8 FW8 – FILTER F187N Optics used in acceptance test JWST Partner's Workshop

  11. DHS Element in ETU Pupil Wheel JWST Partner's Workshop

  12. Precision alignment and KOH bonding of ETU PIL optics is complete Assembly is being integrated with mechanism for further environmental tests ETU Pupil Imaging Lens Assembly JWST Partner's Workshop

  13. ETU Short Wave Fold Mirror Assembly WFE Pre-Vibe: 11.4 nm rms WFE Post-Vibe: 11.8 nm rms SWFM Assembly Vibration Configuration JWST Partner's Workshop

  14. ETU SWFM Cryo-cycling Results Mirror exceeded spec in first Cycle, then maintained acceptable surface figure through Cycles 2 and 3 Note: chart shows only data points taken at points of thermal equilibrium Requirement 17.8 nm (CA) Bottom of 3rd Cycle: 13.8 nm rms JWST Partner's Workshop

  15. Progress on Wavefront Error Recall that the NIRCam optical train as first realized in the Pathfinder did not meet its wavefront error requirement. Several causes were identified: 1) Mount-induced distortion 2) Coating-induced distortions 3) Poor alignment of lenses within a triplet An improved alignment scheme is helping, and the coating problem has been traced to thermal shock at JDSU. A new bonded mount design is the last improvement. JWST Partner's Workshop

  16. Short Wave Bonded ZnSe Singlet “Optic Saver” Standoff JWST Partner's Workshop

  17. Surface figure cooldown of SW ZnSe S1 Surf fig rms = 2.85nm Zernike coeffs for surface S1 deformation (mm) N M A(N,M) 0 0 -5.183155E-10 { Piston 1 0 1.300426E-10 { X-tilt 1 1 -1.121232E-09 { Y-tilt 2 0 -5.291451E-09 { Astigmatism +-45 2 1 1.448882E-06 { Focus shift 2 2 1.274113E-09 { Astigmatism 0 or 90 3 0 -3.222958E-11 { Trefoil Y 3 1 2.269643E-08 { Coma 3rd ord Y 3 2 2.980256E-09 { Coma 3rd ord X 3 3 -8.016083E-06 { Trefoil X 4 0 1.895118E-09 { Tetrafoil Y 4 1 -7.188401E-10 4 2 2.088516E-07 { Spherical 3rd + Focus 4 3 2.122979E-09 4 4 -4.484867E-09 { Tetrafoil X 5 0 -2.934174E-09 { Pentafoil Y 5 1 -4.836911E-11 5 2 7.533641E-09 { Coma 5th ord Y 5 3 -3.353857E-09 { Coma 5th ord X 5 4 -3.639932E-07 5 5 4.083817E-10 { Pentafoil X 6 0 1.082787E-09 { Hexafoil Y 6 1 2.653164E-09 6 2 -5.562098E-09 6 3 -5.657147E-08 { Spherical 5th + 3rd + Focus 6 4 2.971023E-09 6 5 8.877737E-10 6 6 -4.649130E-06 { Hexafoil X JWST Partner's Workshop

  18. Surface figure cooldown of SW ZnSe S2 Surf fig rms = 2.74nm Zernike coeffs for surface S2 deformation (mm) N M A(N,M) 0 0 2.525041E-10 { Piston 1 0 2.993422E-10 { X-tilt 1 1 7.632050E-10 { Y-tilt 2 0 -5.971137E-09 { Astigmatism +-45 2 1 -3.263482E-06 { Focus shift 2 2 5.627774E-09 { Astigmatism 0 or 90 3 0 -4.283727E-10 { Trefoil Y 3 1 1.133856E-07 { Coma 3rd ord Y 3 2 5.183714E-08 { Coma 3rd ord X 3 3 -5.874208E-06 { Trefoil X 4 0 8.810965E-10 { Tetrafoil Y 4 1 1.763393E-09 4 2 8.018278E-07 { Spherical 3rd + Focus 4 3 -4.894394E-10 4 4 -9.632704E-10 { Tetrafoil X 5 0 1.724538E-10 { Pentafoil Y 5 1 -6.425059E-10 5 2 5.631900E-09 { Coma 5th ord Y 5 3 2.292512E-09 { Coma 5th ord X 5 4 -2.042380E-07 5 5 8.014672E-11 { Pentafoil X 6 0 -1.364540E-09 { Hexafoil Y 6 1 3.202912E-09 6 2 -7.377090E-10 6 3 1.018624E-06 { Spherical 5th + 3rd + Focus 6 4 3.032352E-09 6 5 -1.312308E-09 6 6 -2.458051E-06 { Hexafoil X JWST Partner's Workshop

  19. Differences in transmitted WFE in NIRCam SW Path at 2.0mm for 5 field points from cool-down mount-induced surface figure changes SW ZnSe lens rms = 2.15nm rms = 2.08nm rms = 2.48nm rms = 2.09nm rms = 1.97nm Prediction is 2.48 nm versus 8.02 budget allocation JWST Partner's Workshop

  20. Bonding Tests • Sample lens substrates with metal pucks attached have successfully been cryo-cycled to 16K • Characterization of epoxy samples for CTE and other properties is underway • Margin of safety test has been designed with testing to occur in June Test Article Margin of Safety Tests Epoxy samples for testing. JWST Partner's Workshop

  21. OMA Tolerance Analysis OMA Tolerance Review OMA TRR OMA Calibration OMA Calibration Review OMA Build SFPA / SMART Metrology Alignment Plan Review Module B Plug ‘n’ Play, Pt 1 p-SMART Test Module B Plug ‘n’ Play, Pt 2 Warm Alignment Data Review Monte Carlo Analysis Review TRR Predict WFE with p-SMART Predict WFE, focus with OMA Cold Alignment Cycle 1 Check Stability Cold Alignment Cycle 2 Nudge AT AT AT Install PIL, FPA Install Baffle Covers Cold Alignment Cycle 3 FPA & Wavefront Sensing Tests WFS Review Module Integration AT AT AT AT WFE Review TRR ETU Build Flow August  Delivery to GSFC in Oct. JWST Partner's Workshop

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