Charge-coupled devices (CCDs) currently constitute the standard detector for precision astronomical telescopes such as the Large Synoptic Survey Telescope (LSST) due to their high linearity, sensitivity and dynamic range. Charge transfer properties can however be degraded by the presence of defect levels in the silicon band-gap, which can act as trapping centers for signal charge. The technique of single trap-pumping can be used as a tool to probe the underlying properties of relevant defect levels and potentially mitigate against their effects. In this paper we present a single trap-pumping study of the LSST E2V CCD250 across a temperature range of -30◦ to -110◦, a much larger range than previously studied using this approach. The predominant defect level of relevance for CCDs appearing at these temperatures is shown to be the single-acceptor level of the silicon divacancy. Using experimental data and a basic Monte-Carlo model of the trap-pumping process we examine the defect level properties, with an attempt made to account for both the capture and emission of signal charge.
The construction of the Vera C. Rubin Observatory is well underway, and when completed the telescope will carry out a precision photometric survey, scanning the entire sky visible from Chile every three days. The photometric performance of the survey is expected to be dominated by systematics; therefore, multiple calibration systems have been designed to measure, characterize and compensate for these effects, including a dedicated telescope and instrument to measure variations in the atmospheric transmission over the LSST bandpasses. Now undergoing commissioning, the Auxiliary Telescope system is serving as a pathfinder for the development of the Rubin Control systems. This paper presents the current commissioning status of the telescope and control software, and discusses the lessons learned which are applicable to other observatories.
The brighter-fatter effect is a well known phenomenon in thick, back illuminated CCDs, causing asymmetric increase in the observed size of point sources via correlated charge collection with higher signal levels. Over recent years, the effect of various operating parameters (such as the back bias applied) on the size of measured correlations has been well established. Less well studied is the consequence of changing the effective collection gate width of the CCD, which is of limited accessibility to experiment though several values are available in 3 or 4 phase devices. In this proceeding we present collection gate width experiments using both flat field and spot projection illuminations on a thick back illuminated device as used for the LSST project. We report on the size of the variation of measured correlations with gate width as compared with backside bias voltage, and find that gate width constitutes a small but significant contribution. In light of these results, we give comment on device optimisation when minimising correlated charge collection effects is desired.
KEYWORDS: Cadmium sulfide, Video, Signal to noise ratio, Signal processing, Charge-coupled devices, Video processing, Interference (communication), Analog electronics, Clocks, Capacitance
Correlated double sampling (CDS) is a process used in many charge-coupled device readout systems to cancel the reset noise component that would otherwise dominate. CDS processing typically consists of subtracting the integrated video signal during a “signal” period from that during a “reset” period. The response of this processing depends, therefore, on the shape of the video signal with respect to the integration bounds. In particular, the amount of noise appearing in the final image and the linearity of the pixel value with signal charge are affected by the choice of the CDS timing intervals. We use a digital CDS readout system which highly oversamples the video signal (as compared with the pixel rate) to reconstruct pixel values for different CDS timings using identical raw video signal data. We use this technique to develop insights into optimal strategy for selecting CDS timings both in the digital case (where the raw video signal may be available) and in the general case (where it is not). In particular, we show that the linearity of the CDS operation allows subtraction of the raw video signals of pixels in bias images from those in illuminated images to directly show the effects of CDS processing on the final (subtracted) pixel values.
The Large Synoptic Survey Telescope (LSST) uses an Active Optics System (AOS) to maintain system alignment and surface figure on its three large mirrors. Corrective actions fed to the LSST AOS are determined from 4 curvature based wavefront sensors located on the corners of the inscribed square within the 3.5 degree field of view. Each wavefront sensor is a split detector such that the halves are 1mm on either side of focus. In this paper we describe the development of the Active Optics Pipeline prototype that simulates processing the raw image data from the wavefront sensors through to wavefront estimation on to the active optics corrective actions. We also describe various wavefront estimation algorithms under development for the LSST active optics system. The algorithms proposed are comprised of the Zernike compensation routine which improve the accuracy of the wavefront estimate. Algorithm development has been aided by a bench top optical simulator which we also describe. The current software prototype combines MATLAB modules for image processing, tomographic reconstruction, atmospheric turbulence and Zemax for optical ray-tracing to simulate the closed loop behavior of the LSST AOS. We describe the overall simulation model and results for image processing using simulated images and initial results of the wavefront estimation algorithms.
The Large Synoptic Survey Telescope (LSST) is a proposed ground based telescope that will perform a comprehensive
astronomical survey by imaging the entire visible sky in a continuous series of short exposures. Four special purpose
rafts, mounted at the corners of the LSST science camera, contain wavefront sensors and guide sensors. Wavefront
measurements are accomplished using curvature sensing, in which the spatial intensity distribution of stars is measured
at equal distances on either side of focus by CCD detectors. The four Corner Rafts also each hold two guide sensors. The
guide sensors monitor the locations of bright stars to provide feedback that controls and maintains the tracking of the
telescope during an exposure. The baseline sensor for the guider is a Hybrid Visible Silicon hybrid-CMOS detector. We
present here a conceptual mechanical and electrical design for the LSST Corner Rafts that meets the requirements
imposed by the camera structure, and the precision of both the wavefront reconstruction and the tracking. We find that a
single design can accommodate two guide sensors and one split-plane wavefront sensor integrated into the four corner
locations in the camera.
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