The Ocean Color Instrument on NASA’s PACE mission is a 322-887nm hyperspectral imager with 1km x 1km nadir spatial resolution and 5nm spectral resolution utilizing charge-coupled devices (CCDs) operating in Time Delay Integration (TDI) mode where each TDI column represents a different wavelength in 0.625nm increments. After TDI, the charge is moved into serial output pixels and read out. The spatial resolution requires an 8.5MHz readout rate. This only allows 59ns for the CCD reset and video to be asserted and settled before sampling. The response exhibits serial pixel-to-pixel readout interference due to the lack of full settling. Each serial pixel value has a dependence on the value of the preceding pixel value. This leads to a spectrally dependent radiometric measurement error of up to 0.3%. We explain the operation of the detection system, the behavior of the interference, and show the resulting measurement error based on data from both ground testing and on-orbit characterization.
For the fifth Sloan Digital Sky Survey, SDSS-V, we moved one of the two SDSS BOSS spectrographs from Apache Point Observatory in New Mexico to Las Campanas Observatory in Chile, giving us dual-hemisphere coverage. Modifications for connecting to a new robotic fiber positioner included replacing the old fiber slit with a monolithic fiber slit made of a precision-machined glass mount presenting 528 fibers. To construct this slit, V-grooves were cut into a borosilicate glass substrate and fibers were glued into them under a cover plate. This glass slit was then attached to an Alloy 39 (steel) flexure, which in turn was affixed to a thin slit plate made of cast aluminum for insertion into the spectrograph. Because our existing spare parts inventory would not support two distant locations, and because many parts were no longer manufactured, some spectrograph subsystems were replaced with new components or designs.
The Ultraviolet Transient Astronomical Satellite (ULTRASAT) is a scientific UV space telescope that will operate in geostationary orbit. The mission, targeted to launch in 2024, is led by the Weizmann Institute of Science (WIS) in Israel and the Israel Space Agency (ISA). Deutsches Elektronen Synchrotron (DESY) in Germany is tasked with the development of the UV-sensitive camera at the heart of the telescope. The camera's total sensitive area of ≈90mm x 90mm is built up by four back-side illuminated CMOS sensors, which image a field of view of ≈200 deg2. Each sensor has 22:4 megapixels. The Schmidt design of the telescope locates the detector inside the optical path, limiting the overall size of the assembly. As a result, the readout electronics is located in a remote unit outside the telescope. The short focal length of the telescope requires an accurate positioning of the sensors within ±50 μm along the optical axis, with a flatness of ±10 μm. While the telescope will be at around 295K during operations, the sensors are required to be cooled to 200K for dark current reduction. At the same time, the ability to heat the sensors to 343K is required for decontamination. In this paper, we present the preliminary design of the UV sensitive ULTRASAT camera.
The SwRI Detector Characterization Lab (SDCL) was established in order to facilitate the rapid calibration of large numbers of detector arrays for upcoming ground and space missions. The SDCL is equipped with a McPherson monochromator with exchangeable gratings and light sources enabling wavelength coverage from 0.3 to 5.0 micron at sub nanometer resolution. The SDCL also has cryostats capable of maintaining thermal control of detector subassemblies and transfer optics to a precision of 0.1K at 77K and 0.01K at 4K. Using this calibration system, we have calibrated the EEM and ETU detector for read noise, dark current, modulation transfer function, quantum efficiency, cross talk, and total system throughput. The data were collected using standard Photon Transfer Curve techniques at the various wavelengths corresponding to the MVIC filter bandpasses. Here, we will present the data for the engineering unit, the methodology used to perform the calibration, and the steps forward for calibration of the flight unit.
We report on ongoing scientific CCD detector and control electronic developments at STA. Recent astrometric and spectroscopic instruments are pushing for highly uniform pixel arrays. We present results from sensors fabricated with high resolution 1X masks aimed at minimizing the random and periodic pixel nonuniformities introduced during manufacture. Instrument requirements for large next generation telescopes tend to target larger arrays with larger pixels. We introduce the STA4500, a four output 6120 x 6120 15um CCD intended for these applications. The device includes dual transfer gates before the serial register to allow slow, high CTE vertical transfers to occur simultaneous with serial readout. We also present our next experimental high dynamic range CCD. This sensor uses dual outputs operating in parallel with different sensitivities to greatly expand the linear dynamic range achievable with large pixel scientific sensors without impairing noise or readout rate. Finally, we describe updates to our Archon astronomical CCD controller. Improvements include daisy chained multi-controller synchronization for mosaic readout, high resolution thermal control for sub-milliKelvin temperature stability, and high voltage biases up to +/-100V for operating deep depletion CCDs.
The rapid evolution of commercial FPGAs and analog ICs has enabled the development of Archon, a new modular high
performance astronomical CCD controller. CCD outputs are digitized by 16-bit 100 MHz ADCs with differential AC-coupled
preamplifiers. The raw data stream from an ADC can be stored in parallel with standard image data into three
onboard 512 MB frame buffers. Pixel values are computed using digital correlated double sampling. At low pixel rates
(< 1 MHz), the dynamic range achievable by averaging hundreds of ADC samples per pixel can exceed 16 bits, so an
option to store 32 bits per pixel is provided. CCD clocks are generated by 14-bit 100 MHz DACs. The scripted timing
core driving the clocks can generate a new target voltage for each clock every 10 ns, and the clock slew rates are
individually programmable. CCD biases are derived from 16-bit DACs, are continuously monitored for voltage and
current, and power up and down in a customizable sequence. Communication between the controller and a host
computer occurs over a gigabit Ethernet interface (fiber or copper). A CCD configuration is specified by a simple text
file. Together, these features simplify the tuning and debugging of scientific CCDs, and enable CCD-limited imaging. I
present details of the controller architecture, examples of CCD tuning, and measured performance data of the controller
alone (dynamic range of 108 dB at 100 kHz and 98 dB at 1 MHz) and in combination with an STA1600LN CCD.
The demand from the astronomical community for high resolution low noise CCDs has led to the development of the
STA1600LN, a 10560 × 10560 pixel, 95mm × 95mm, full-frame CCD imager with 9×9 μ2 pixels. The device
improvements include noise reduction to below 3ē at 100kHz, improved quantum efficiency, as well as packaging
developments for improved fill factor in mosaic systems. We provide test results from production devices, along with
updates on scientific systems utilizing the STA1600 for astronomy.
The Geostationary Lightning Mapper (GLM) instrument selected to fly on the National Oceanic and Atmospheric
Administration (NOAA) GOES-R Series environmental satellites has very unique requirements as compared to an
imaging array. GLM's requirements to monitor lightning on a continental scale will provide new insight into the
formation, distribution, morphology and evolution of storms.
A 500 frame per second backside illuminated frame transfer CCD imager (STA3900A) with variable pixel size has
been developed to meet these requirements. A variable pixel architecture provides a near uniform mapping of the curved
surface of the earth, while 56 outputs running at 20 MHz yield greater than a 1.1 Gigapixel per second data rate with low
RMS noise and high MTF. This paper will provide detailed information on design trades required. We will report CCD
read noise, dark current, full well capacity, and quantum efficiency (QE).
The Observatories of the Carnegie Institution for Science have operated the 1 and 2.5-meter telescopes since the early
1970s with only minor changes to the original control systems. We discuss the replacement of the original 4004 microprocessor-
based telescope control system with modern high-speed servo controllers and motors, absolute main axis
encoders, modern closed-loop controls and PC-based main operating software. We also discuss the original relay-based
interlock systems that have been replaced with Programmable Logic Controllers (PLC) and have been interfaced into the
new telescope control system. The modernization of both telescopes also includes many hardware upgrades to allow for
remote observing and scripted automatic observations. These upgrades also include the modernization of shutter drives,
windscreens and dome controls to improve the reliability and safety required for remote observing from an existing
facility.
A 52-M pixel, 71mm x 54mm, full-frame CCD imager with 8.6 um x 8.6 um pixel size has been
developed for use in high speed scanning applications. On-going interest for ultra-high resolution, high
speed imagers for electronic imaging OEM customers in various scientific markets including spectroscopy
and digital photography has led to the development of the STA2500A. Innovative design techniques were
utilized in the production of this device. 32 outputs running at 40 Mhz yield a 20Hz frame rate with low
RMS noise and high MTF. This paper will provide detailed information on design trades developed for
high-speed imagers leading to the design and performance capabilities of the STA2500A, as well as a
description of the electronics required for its use.
A full-wafer, 10,580 × 10,560 pixel (95 × 95 mm) CCD was designed and tested at Semiconductor Technology
Associates (STA) with 9 μm square pixels and 16 outputs. The chip was successfully fabricated in 2006 at DALSA
and some performance results are presented here. This program was funded by the Office of Naval Research
through a Small Business Innovation in Research (SBIR) program requested by the U.S. Naval Observatory for
its next generation astrometric sky survey programs. Using Leach electronics, low read-noise output of the 111
million pixels requires 16 seconds at 0.9 MHz. Alternative electronics developed at STA allow readout at 20
MHz. Some modifications of the design to include anti-blooming features, a larger number of outputs, and use
of p-channel material for space applications are discussed.
A 111-Mega pixel, 92×92 mm2, full-frame CCD imager with 9×9 um2 pixel size has been developed for use in scientific
applications. Recent interest for ultra-high resolution imagers for electronic imaging OEM customers in various
scientific markets, including biotechnology, microscopy, crystallography, astronomy, spectroscopy, and digital
photography markets has lead to the development of the STA1600A 111-Mega pixel monochromatic charge-coupled
device. Innovative design techniques were utilized in the early development of this device, yielding low RMS noise and
high MTF for readout speeds ranging from 1 Mpixel/s to 10 Mpixel/sec. This paper will provide detailed information on
the design and performance capabilities of the STA1600A, as well as background information on the commercial uses of
this device.
A 111-Mega pixel, 92x92 mm2, full-frame CCD imager with 9x9 um2 pixel size has been developed for use in scientific
applications. Recent interest for ultra-high resolution imagers for electronic imaging OEM customers in various
scientific markets, including biotechnology, microscopy, crystallography, astronomy, spectroscopy, and digital
photography markets has lead to the development of the STA1600A 111-Mega pixel monochromatic charge-coupled
device. Innovative design techniques were utilized in the early development of this device, yielding low RMS noise and
high MTF for readout speeds ranging from 1 Mpixel/s to 10 Mpixel/sec. This paper will provide detailed information on
the design and performance capabilities of the STA1600A, as well as background information on the commercial uses of
this device.
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