KEYWORDS: Sensors, Analog electronics, Clocks, Astronomy, Data acquisition, James Webb Space Telescope, Image sensors, Microcontrollers, Array processing, Human-machine interfaces
The SIDECAR ASIC is a fully integrated system-on-a-chip focal plane array controller that offers low power and low noise, small size and low weight. It has been widely used to operate different image sensors for ground-based and flightbased astronomy applications. A key mechanism to operating analog detectors is the SIDECAR ASIC's high level of programmability. This paper gives an overview of the SIDECAR ASIC architecture, including its optimized microcontroller featuring a customized instruction set. It describes the firmware components, including timing generation, biasing, commanding, housekeeping and synchronization of multiple detectors. The firmware development tools including compiler and supporting development environment and hardware setup are presented. The firmware capability for ground-based HxRG applications and for flight-based applications like the James Webb Space Telescope (JWST), the repair of the Advanced Camera for Surveys (ACS), and others are also discussed.
Yibin Bai, William Tennant, Selmer Anglin, Andre Wong, Mark Farris, Min Xu, Eric Holland, Donald Cooper, Joseph Hosack, Kenneth Ho, Thomas Sprafke, Robert Kopp, Brian Starr, Richard Blank, James Beletic, Gerard Luppino
Teledyne’s silicon hybrid CMOS focal plane array technology has matured into a viable, high performance and high-
TRL alternative to scientific CCD sensors for space-based applications in the UV-visible-NIR wavelengths. This paper
presents the latest results from Teledyne’s low noise silicon hybrid CMOS visible focal place array produced in 4K×4K format with 10 μm pixel pitch. The H4RG-10 readout circuit retains all of the CMOS functionality (windowing, guide
mode, reference pixels) and heritage of its highly successful predecessor (H2RG) developed for JWST, with additional
features for improved performance. Combined with a silicon PIN detector layer, this technology is termed HyViSI™
(Hybrid Visible Silicon Imager). H4RG-10 HyViSI™ arrays achieve high pixel interconnectivity (<99.99%), low
readout noise (<10 e- rms single CDS), low dark current (<0.5 e-/pixel/s at 193K), high quantum efficiency (<90%
broadband), and large dynamic range (<13 bits). Pixel crosstalk and interpixel capacitance (IPC) have been predicted
using detailed models of the hybrid structure and these predictions have been confirmed by measurements with Fe-55 Xray
events and the single pixel reset technique. For a 100-micron thick detector, IPC of less than 3% and total pixel
crosstalk of less than 7% have been achieved for the HyViSI™ H4RG-10. The H4RG-10 array is mounted on a
lightweight silicon carbide (SiC) package and has been qualified to Technology Readiness Level 6 (TRL-6). As part of
space qualification, the HyViSI™ H4RG-10 array passed radiation testing for low earth orbit (LEO) environment.
In preparation for the large number of infrared pixels required in the era of Extremely Large Telescopes, Teledyne, in
partnership with the University of Hawaii and GL Scientific, has been funded to develop the next generation of largeformat infrared focal plane array for ground-based astronomy; the 4096 × 4096 pixel (15 micron pitch) H4RG-15. Teledyne has successfully designed, produced, and tested the first generation H4RG-15 prototype arrays. This paper reports on the functionality and performance test results of the H4RG-15 prototypes and provides status of the 2012 pilot production effort.
Teledyne’s H2RG focal plane arrays have been widely used in scientific infrared and visible instruments for ground-based and space-based telescopes. The majority of applications use the H2RG with 2.5 micron cutoff HgCdTe detector pixel at an operating temperature of ~77 K (LN2). The exceptionally low dark current of the 2.5 micron H2RG allows for operation at higher temperatures which facilitates simplified instrument designs and therefore lower instrument cost. Performance data of 2.5 micron H2RG arrays at 77K, 100 K, and 120 K are presented and are discussed as a function of detector bias and pixel readout rate. This paper also presents performance data of 1.75 micron and 5.3 micron H2RG focal plane arrays and discusses some of the inherent performance differences compared to 2.5 micron cutoff arrays. A complete infrared camera system that uses the H2RG focal plane array and SIDECAR ASIC focal plane electronics is introduced.
Arrays of independently tunable MEMS Fabry-Perot filters have been developed that enable spectral tuning over the
range of 11 - 8 microns with a filter bandwidth of ~ 120 nm. Actuation is provided using a MEMS driver IC that is
hybridized to the MEMS chip. Combining the filter array with an IR FPA enables spatially-resolved spectral tuning in a
compact architecture. Tunable spectral response data from the first integrated tunable filter / FPA device are presented.
The HAWAII-2RG based focal plane arrays represent one the most advanced imaging sensor technologies for near-infrared
and visible astronomy. Since its introduction a few years ago, the HAWAII-2RG has been selected for a large
number of space and ground-based instruments, including the James Webb Space Telescope. In addition, the SIDECAR
ASIC, a fully integrated FPA controller system-on-a-chip, has been matured and is now being implemented in many of
the next generation instruments. As a result of the SIDECAR ASIC, the detector system becomes a fully digital unit that
is superior to the conventional discrete focal plane electronics with respect to power consumption, mass, volume and
noise immunity. This paper includes an introductory description of the HAWAII-2RG and the SIDECAR ASIC, and
presents the latest test results. It also discusses the latest generation of astronomy FPAs: the HAWAII-4RG. This new
multiplexer contains all of the HAWAII-2RG features, but provides 4 times as many pixels at a pixel pitch of 10μm.
Preliminary HAWAII-4RG test data is presented.
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