Focal Plane Arrays and Focal Plane Electronics for

Focal Plane Arrays and Focal Plane Electronics for Large Scientific Telescopes Richard Blank, Eric Piquette, Raphael Ricardo, Michael Eads, Jing Chen, Mark Farris, Brian Starr, and James Beletic Your Partner for: Ground-Based Astronomy ESO Very Large Telescope (VLT) Facility Mauna Kea Observatories - Hawaii Calar Alto Observatory Space-Based Astronomy JWST Machellan Telescopes HST WISE Earth and Planetary Science MMM Rosetta GOES-R OCO-R H 2 RG Focal Plane Array and SIDECAR ASIC Focal Plane Electronics – A High Performance Integrated System for Astronomy for NIR ( co = 1. 75 mm), SWIR ( co = 2. 5 mm), and MWIR ( co = 5. 3 mm) Observations Atmospheric Transmission • The HAWAII-2 RG (H 2 RG) is the leading IR focal plane array (FPA) in ground- and space-based IR astronomy and offers un-matched performance and cosmetic quality between 500 nm and 5. 3 micron – Substrate removed Hg. Cd. Te for high QE throughout spectral band – Lowest noise and dark current – Performance confirmed by major observatories and instrument teams Photo: Courtesy of GL Scientific OSR Case 08 -S-1729 OSR Case 08 -S-1691 H 2 RG Focal Plane Array OSR Case 08 -S-1729 SIDECAR ASIC in standard ceramic package SIDECAR ASIC in hermetically sealed package • Delivered over 40 science grade H 2 RG FPAs for facility class instruments to major ground based observatories around the world Wavelength (microns) “Standard” Ground-Based Astronomy Cutoff Wavelengths Near infrared (NIR) Short-wave infrared (SWIR) Mid-wave infrared (MWIR) • Delivered 7 4096× 4096 pixel mosaics – JWST NIRCam (Delivered) Definition of Cutoff Wavelength – Gemini GSAOI (Delivered) OSR Case 08 -S-1691 5 x 7 H 2 RG Focal Plane Array Mosaic J, H, K, L, M • Two 2 x 2 space flight H 2 RG mosaics, 4 outputs / H 2 RG, SIDECAR ASIC based focal plane electronics (FPE) Photo: Courtesy of GL Scientific OSR Case 08 -S-1729 1. 75 µm 2. 5 µm 5. 3 µm SIDECAR ASIC Cryogenic Focal Plane Electronics • One 2 x 2 ground-based H 2 RG mosaic, 4 outputs / H 2 RG – CFHT WIRCAM (On the sky – CFHT) • One 2 x 2 ground-based H 2 RG mosaic, 32 outputs / H 2 RG – ESO HAWK-I (On the sky – VLT) • One 2 x 2 ground-based mosaic, 32 outputs / H 2 RG Fully Substrate Removed Hg. Cd. Te: – OCIW FOURSTAR (Delivered) • One 2 x 2 ground-based mosaic, 32 outputs / H 2 RG, SIDECAR ASIC FPE – MPIA PANIC (Delivered) • One 2 x 2 ground-based mosaic, 32 outputs / H 2 RG Photo: Courtesy of GL Scientific • SIDECAR ASIC based focal plane electronics (FPE) – Compact size, low power, turn-key hardware and software Photo: Courtesy of GL Scientific 2 x 2 H 2 RG Mosaics (4096 x 4096 Pixel) • Overall improved QE • Response to visible and UV • Less susceptible to cosmic rays • Eliminates fringing in substrate material OSR Case 08 -S-1729 • Dedicated Astronomy & Civil Space Market Segment – Dedicated program management and support team – Responsiveness to customer inquiries – Shortened delivery schedule Median Dark Current < 0. 005 e- / sec at 77 K Noise [e-] Number of Pixel Dark Current Scale: 0. 000 – 0. 050 e- / sec Fowler-32: 3. 4 e- Measured QE > 85%, / mean < 2 % (shown for 2, 000 nm) 0. 03 0. 04 Theoretical 0. 4 Obtained with SIDECAR ASIC Focal Plane Electronics 0. 6 0. 8 Quantum Efficiency Fowler Pairs Mean CDS Noise: 12. 3 e(9. 0 e- on reference pixel) A pixel is considered operable if QE > 35% (shown for 2000 nm), dark current is < 1 e-/sec, and CDS read noise is < 50 e- CDS Noise on 3 Science Grade and 1 Engineering Grade Focal Plane Arrays less than 10 electrons Spectral response of KMOS Science Grade Focal Plane Array Noise [e-] Measured 1. 0 1, 0000 Dark Current [e-/sec] Frequency Bad-Pixel Cluster Map and Histogram Pixel in clusters: 57 Number of clusters: 1 100 0. 02 Pixel Operability Map QE Scale: 40% – 100% 10 0. 01 High Operability and Excellent Cosmetic Quality Number of Clusters 0. 00 Number of Pixel High and Uniform QE Throughout Spectral Band Low Noise and Negligible Dark Current Data: Courtesy of NASA GSFC, WFC-3 Project 1 CDS Noise [e-] 100 Fowler-16: 4. 3 e- Cluster Size Theoretical Pairs Data: Courtesy of OCIW, Four. Star Fowler Project E-ELT Data: Courtesy of ESO, KMOS Project Science Grade Pixel Operability > 99% Data: Courtesy of ESO, KMOS Project Only 1 cluster with 57 inoperable pixel H 4 RG Focal Plane Array and SIDECAR ASIC Focal Plane Electronics – The Next Generation Building Block for the Packaging ELTs is. Approach on itsfor. Way H 4 RG-10: 4096 x 4096, 10 mm Pixel FPA H 4 RG-15: 4096 x 4096, 15 mm Pixel FPA One Modular all Applications • TMT • • GMT • H 4 RG-10 Hybrid Visible Imager (Hy. Vi. SI™) focal plane array is baseline for an astrometric space mission Focal planes delivered in 2009 provide required performance at 193 K q Dark current < 0. 05 e/sec q Operability > 99% q CDS noise < 10 e. Flight arrays are planned to be delivered in 2010 First prototype 1. 75 mm IR SCAs demonstrated • Silicon Carbide (Si. C) carrier for visible (Silicon) and substrate removed IR (Hg. Cd. Te) focal planes • • Rigid-flex cable with wirebond pads and with passives for flight or ground-based application • • • SIDECAR ASIC “on-board” = photons in bits out H 4 RG-15 SCA Photons in Photo: Courtesy of GL Scientific H 2 RG Si. C Package Analog output option SIDECAR ASIC Photo: Courtesy of GL Scientific H 4 RG-10 Hybrid Visible Imager (Hy. Vi. SI) Focal Plane on Invar Prototype Development of the H 4 RG-15 IR, fully substrate removed FPA is planned to commence in November 2009 Maintain performance of H 2 RG FPA by simultaneously substantially reducing cost per pixel Coefficient of Thermal Expansion (CTE) as a Function of Temperature H 2 RG Si. C Package 3 D-Model: Courtesy of GL Scientific Bits out H 4 RG-15 Focal Plane and SIDECAR ASIC Focal Plane Electronics Building Block TSI-0472