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Astrophysics Breakout Don Figer RIT, RIDL

Astrophysics Breakout Don Figer RIT, RIDL. Charge to Breakout Sessions. Breakout groups will determine: the most pressing questions in their area that leverage QLIDs the most important detector characteristics for answering these questions

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Astrophysics Breakout Don Figer RIT, RIDL

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  1. Astrophysics BreakoutDon FigerRIT, RIDL

  2. Charge to Breakout Sessions Breakout groups will determine: the most pressing questions in their area that leverage QLIDs the most important detector characteristics for answering these questions the specific technologies that are most promising for achieving these characteristics the hurdles for implementing these technologies the R&D roadmap for overcoming these hurdles the funding opportunities for executing the R&D roadmap The four areas are: biomedical astrophysics Earth system science defense/homeland security Group leads will present findings in the final session of the workshop. 3

  3. Breakout Session Leads BiomedicalTim Tredwell AstrophysicsDon Figer Earth Systems ScienceJeff Puschell Defensee/Homeland SecurityMark Bocko 4

  4. The Top Five Science Drivers for Detectors: Astrophysics What is dark energy? (QE, read noise, DC) What is dark matter? (QE, read noise, DC) What processes alter the surfaces of planets/moons? (thermal imaging, LIDAR, dynamic features with DFPA) Do Earth-like planets exist? Does extraterrestrial life exist? (O3, MIR) When was the Universe enriched with metals? How were galaxies assembled? 5

  5. The Top Detector Characteristics for: Astrophysics in-pixel wavelength discrimination high QE across broad range low dark current zero read noise time-tagging (for LIDAR) larger formats (>10K x 10K)‏ lower power, higher temp. operation lower cost operation (e.g. standardized ASIC, easier than SIDECAR)‏ high dynamic range: 1 - 1E7 photons high speed capabilities, yet retain low noise 6

  6. Reference Chart: Key Detector Characteristics Homeland Safety Biomedical Imaging Earth System Science Defense Quantum-Limited Imaging Detector Read Noise Dark Current QE λ λ/Δλ Δt P

  7. Detector Performance Requirements for: Astrophysics 8

  8. The Most Promising Detector Technologies for: Astrophysics TES, SSPD: wavelength detection SSPD, GM-APD: zero read noise MCP: single photon counting UV GM-APD: time-tagging Digital solid state photomultiplier array (BiB, Rockwell Anaheim/Boeing) DFPA 9

  9. Hurdles for the Most Promising Detector Technologies for: Astrophysics TES: QE, temperature, format GM-APD: afterpulsing SSPD: cold operation TES: extremely cold, not ideal wavelength coverage DFPA: for low backgrounds?? 10

  10. Detector R&D Roadmap for: Astrophysics GM-APD demonstrate 1 e-/s/pixel demonstrate ~64x64 diode/ROIC array at 150 K design megapixel array and demonstrate at telescope SSPD (NbN) demonstrate an array with high QE TES demonstrate QE vs. lambda from UV to MIR find magic material that operates at higher T demonstrate low noise DFPA demonstrate low background capability demonstrate long integration time demonstrate low noise 11

  11. Funding Possibilities: Astrophysics NASA ROSES APRA, PIDDP NSF ATI Private DARPA MTO BAA Stimulus funding 12

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