Astrophysics Breakout Don Figer RIT RIDL Charge to

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 – 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 IT Collaboratory 2009 Research Symposium 3

Breakout Session Leads • Biomedical Tim Tredwell • Astrophysics Don Figer • Earth Systems Science Jeff Puschell • Defensee/Homeland Security Mark Bocko 4 IT Collaboratory 2009 Research Symposium 4

The Top Five Science Drivers for Detectors: Astrophysics 1. What is dark energy? (QE, read noise, DC) 2. What is dark matter? (QE, read noise, DC) 3. What processes alter the surfaces of planets/moons? (thermal imaging, LIDAR, dynamic features with DFPA) 4. Do Earth-like planets exist? 5. Does extraterrestrial life exist? (O 3, MIR) 6. When was the Universe enriched with metals? 7. How were galaxies assembled? 5 IT Collaboratory 2009 Research Symposium 5

The Top Detector Characteristics for: Astrophysics 1. 2. 3. 4. 5. 6. 7. 8. in-pixel wavelength discrimination high QE across broad range low dark current zero read noise time-tagging (for LIDAR) larger formats (>10 K x 10 K) lower power, higher temp. operation lower cost operation (e. g. standardized ASIC, easier than SIDECAR) 9. high dynamic range: 1 - 1 E 7 photons 10. high speed capabilities, yet retain low noise 6 IT Collaboratory 2009 Research Symposium 6

Reference Chart: Key Detector Characteristics Homeland Safety Earth System Science Biomedical Imaging Defense Quantum-Limited Imaging Detector Read Noise 7 Dark Current IT Collaboratory 2009 Research Symposium QE λ λ/Δλ Δt P

Detector Performance Requirements for: Astrophysics Parameter Current Goal Format Pixel Size Read Noise Dark Current QE Latent Image Flux Rate Capacity Operating Temperature Fill Factor Radiation Immunity Susceptibility to Radiation Transients Technology Readiness Level 8 IT Collaboratory 2009 Research Symposium 8

The Most Promising Detector Technologies for: Astrophysics 1. 2. 3. 4. 5. TES, SSPD: wavelength detection SSPD, GM-APD: zero read noise MCP: single photon counting UV GM-APD: time-tagging Digital solid state photomultiplier array (Bi. B, Rockwell Anaheim/Boeing) 6. DFPA 9 IT Collaboratory 2009 Research Symposium 9

Hurdles for the Most Promising Detector Technologies for: Astrophysics 1. 2. 3. 4. TES: QE, temperature, format GM-APD: afterpulsing SSPD: cold operation TES: extremely cold, not ideal wavelength coverage 5. DFPA: for low backgrounds? ? 10 IT Collaboratory 2009 Research Symposium 10

Detector R&D Roadmap for: Astrophysics 1. 2. 3. 4. GM-APD a) b) c) demonstrate 1 e-/s/pixel demonstrate ~64 x 64 diode/ROIC array at 150 K design megapixel array and demonstrate at telescope a) demonstrate an array with high QE a) b) c) demonstrate QE vs. lambda from UV to MIR find magic material that operates at higher T demonstrate low noise a) b) c) demonstrate low background capability demonstrate long integration time demonstrate low noise SSPD (Nb. N) TES DFPA 11 IT Collaboratory 2009 Research Symposium 11

Funding Possibilities: Astrophysics 1. 2. 3. 4. 5. NASA ROSES APRA, PIDDP NSF ATI Private DARPA MTO BAA Stimulus funding 12 IT Collaboratory 2009 Research Symposium 12