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Focal Plane Array Testing and Applications for Astronomy

Focal Plane Array Testing and Applications for Astronomy. Donald Figer Space Telescope Science Institute. Outline. The role of detectors in discovery. The state of the art in detectors. Keck/LGS/AO HST SOFIA Detectors and future Astronomy projects. LSST SNAP JWST. The Role of Detectors.

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Focal Plane Array Testing and Applications for Astronomy

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  1. Focal Plane Array Testing and Applications for Astronomy Donald FigerSpace Telescope Science Institute

  2. Outline • The role of detectors in discovery. • The state of the art in detectors. • Keck/LGS/AO • HST • SOFIA • Detectors and future Astronomy projects. • LSST • SNAP • JWST

  3. The Role of Detectors

  4. Detector Functions • Photometry • Astrometry • Spectoscopy • Morphology • Time Variability

  5. Detector Types • Eye • Film • Photomultiplier tube • CCD • Photodiode array • Radio Antennae

  6. Detector Wavelength Sensitivity X-ray Visible NIR MIR l [mm] 0.1 0.3 0.9 1.1 2.5 5 20 Silicon HgCdTe InSb InGaAs

  7. CCD Architecture

  8. Hybrid Architecture

  9. Hybrid Architecture In bump light-sensitive layer substrate AR coating

  10. Keck

  11. Keck

  12. Keck

  13. Keck/AO/LGS

  14. HST: Hubble Space Telescope • General-purpose orbiting astronomical telescope

  15. HST

  16. HST

  17. HST

  18. HST

  19. HST

  20. SOFIA: Stratospheric Observatory for Infrared Astronomy

  21. LSST: Large Synoptic Survey Telescope • What is the distribution of dark matter in the Universe? • What is dark matter?

  22. LSST

  23. SNAP: Supernova Acceleration Probe • What is dark energy?

  24. SNAP Optical Configuration • Telescope is a three-mirror anastigmat • 2.0 meter aperture • 1.37 square degree field • Lightweight primary mirror • Low-expansion materials • Optics kept near 290K • Transverse rear axis • Side Gigacam location • passive detector cooling • combines Si & HgCdTe detectors • Spectrometers share Gigacam focal plane • Few moving parts in payload • two-blade shutter for Gigacam • focussers/adjusters at secondary & tertiary

  25. SNAP Focal Plane Concept • Coalesce all sensors at one focal plane. • Imager sensors on the front. • 36 HgCdTe 2kx2k 18 mm • 36 CCD 3.5kx3.5k 10.5 mm • Filters • 1 of 3 per HgCdTe • 4 of 6 per CCD • Spectrograph on the back with access ports through the focal plane. • Exposure times of 300 s with four/eight exposures in CCDs/HgCdTe.

  26. JWST: James Webb Space Telescope • What is the shape of the Universe? • How do galaxies evolve? • How do stars and planetary systems form and interact? • How did the Universe build up it present elemental/chemical composition? • What is dark matter?

  27. JWST • 6.5m diameter primary mirror • launch in 2013 • orbit at L2 • four scientific instruments • JWST deployment movie

  28. IDTL: Independent Detector Testing Laboratory • Located at Space Telescope Science Institute and Johns Hopkins University • Founded 1999 • Mission: Serve the astronomical community by developing and testing detectors for space and ground based astronomy programs

  29. Past and Present Personnel Tom Reeves Lab Technician Robert Barkhouser Optical Engineer Eddie Bergeron Data Analyst Bernie Rauscher Project Scientist Utkarsh Sharma Graduate Student Mike Telewicz Intern Steve McCandliss JHU Lead Ernie Morse Data Analyst Gretchen Greene Mechanical Engineer Scott Fels Intern Don Figer Director Monica Rivera Intern Sito Balleza Systems Engineer Mike Regan System Scientist Russ Pelton Technician

  30. IDTL Test System He Lines

  31. IDTL Test System Figure 3.3. Mechanical drawing of cross section of IDTL dewar assembly. The optics with ray trace are also shown. Figer et al. 2002, SPIE, 4850, 981

  32. IDTL Sample Results: Persistence (1200 seconds)

  33. IDTL Sample Results: Read Noise

  34. IDTL Sample Results: Dark Current

  35. IDTL Sample Results Dark Current Dark Current Read Noise Gain Short-wave Cutoff Long-wave Cutoff Persistence RQE vs. T

  36. IDTL Comparartive Detector Characterization

  37. Properties of Silicon: QE

  38. Properties of Silicon: Long Wave QE

  39. Silicon 1 mm QE vs. Thickness & Temperature

  40. Properties of HgCdTe • Nearly “ideal” characteristics. • Many vendors.

  41. Properties of InGaAs: QE

  42. State of the Art: Thin CCD • Nearly “ideal” characteristics. • Many (~4) vendors.

  43. State of the Art: LBNL Thick CCD QE

  44. State of the Art: Si PIN • Emerging technology. • Chief Vendors - Raytheon Vision Systems (RVS) and Rockwell Scientifics Corp. (RSC).

  45. State of the Art: Si PIN RQE (100 mm thick)

  46. State of the Art: Si PIN Hybrid Arrays • Si PIN Hybrid QE Measures Data (from B. Pain, et. al.)

  47. State of the Art: Si PIN Dark Current 0.001 e-/s/pixel for 10 mm pixel • read noise in H2RG-003 (18 mm pixels) • 1e- on reference pixels, Fowler-32, 100 kHz • 9e- on science pixels, Fowler-32, 100 kHz • well depth, 120,000 e- • QE@ 1mm • 24%@140K • 28%@160K • 33%@180K • 38%@200K • Crosstalk, 2-3% • Persistence, <0.3%

  48. State of the Art: Si PIN Read Noise 10 e-

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