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HAWC High-resolution Airborne Wideband Camera

HAWC High-resolution Airborne Wideband Camera. Facility Instrument for SOFIA Far-infrared camera covering the spectral range 40-300 µm Four filters at 53, 89, 155, and 216 µm 12 x 32 Pop-up Detectors (PUD) array cooled to 0.2˚K with adiabatic demagnetization refrigerator (ADR)

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HAWC High-resolution Airborne Wideband Camera

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  1. HAWCHigh-resolution Airborne Wideband Camera • Facility Instrument for SOFIA • Far-infrared camera covering the spectral range 40-300 µm • Four filters at 53, 89, 155, and 216 µm • 12 x 32 Pop-up Detectors (PUD) array cooled to 0.2˚K with adiabatic demagnetization refrigerator (ADR) • Design optimized to give the highest possible angular resolution • 3 Major Subassemblies: • Cryostat/Detector/Optics • 1249 lbs (5.5% margin) • Counterweight Rack • 212 lbs (Contents only) • Floor Rack • 300 lbs (Including Contents)

  2. HAWC Detector Array • 12 x 32 implanted silicon bolometer array developed at NASA/Goddard (Moseley et al.)

  3. HAWC Detector Array Detector array under cover JFET box

  4. HAWC Detector Array

  5. HAWC (OMS)Opto-Mechanical System Pupil/Filter Wheel

  6. HAWC (OMS)Opto-Mechanical System Filter Wheel Pupil Wheel

  7. HAWC (OMS)Opto-Mechanical System

  8. HAWC Optical Layout

  9. HAWC Optical and Photometric Specifications22 June 2004 Items shaded pink need to be updated.

  10. Detector Testing Results Preliminary Focused Beam Test Results (band 2 optics) • We see light!!! • circular PSF (within measurement errors) • detector to detector spacing at source: 1.27 mm • beam size: 1.9 pixels FWHM • optical response across rows does not show large variations Row 3 Row 2 time  Overall Detector Testing Summary • 90% of pixels are working • changes in grounding and rf filtering have reduced noise to acceptable levels. (~10 – 50 nV/Hz1/2 with typical bias levels) • load curves predict NEPs of 4-5  10-17 W/Hz1/2 under nominal SOFIA conditions

  11. Noise contributions Previous Est. New Estimates Units m pW nV/Hz 108 V/W 10-17 W/Hz nV/Hz V 10-17 W/Hz nV/Hz

  12. Noise-Power Spectra (dark tests) Biased Input Grounded Input Signal (nV/ rtHz) Power spectra for two selected detector pixels (red plots are biased channels, blue plot is a grounded channel). 5–20 Hz amplitudes match prediction from model based on iv-curve data.

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