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1.
To complement previously published information on E2V CCDs, we present here some less well-known information about Marconi
CCDs. We show details of the performance of deep depletion silicon variants, and discuss other subtleties of performance.
We also present an update on L3vision (sub-electron noise) devices, indicating current availability, options, and ongoing
development work. Finally, we will give a flavour of the range of custom designs that have been made. Many of these are not
commercially available, and may not be familiar to all astronomers or CCD technologists.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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Stefan Ströbele 《Experimental Astronomy》2001,11(2):151-156
High quality CCD detectors are now being produced with 2048× 4096 square pixels, each 15 m on a side. Evenlarger detector areas are built with several CCDs mounted into amosaic. To be useful in an instrument the light must be in focuson all CCDs, requiring that all CCDs in a mosaic must typicallybe aligned within 30 micron of a flat plane. To achieve thisaccuracy in many cases the measurement and correction of the CCDalignment is necessary. One way allowing a surface measurement,even when the CCD is protected by a window, is to usetriangulation sensor. The principle of a triangulation sensor,its application and its implementation in a measuring machineare presented here. 相似文献
4.
CCD是天文望远镜中最常见的观测终端设备,也是望远镜自主控制系统中的重要组成部分。随着天文望远镜自主观测需求的不断出现以及技术的快速发展,开源的RTS2软件系统成为目前该领域研究中受到较多关注的系统之一。但RTS2支持的CCD设备较为有限,同时控制接口约定也相对固定。在针对部分特殊的CCD设备(如LAMOST中采用的32台CCD设备、选址用的部分CCD设备)时,仅实现原有类的方法是不够的。在深入分析RTS2源码的基础上,重点从参数、命令、协议扩展方面研究基于原有的Camera类,通过继承的方法构造新的CCD类型,实现对LAMOST项目的 CCD控制,取得了较好的效果,对在RTS2中集成望远镜系统其他类型设备也有较好的参考价值。 相似文献
5.
Group delay fringe tracking using spectrally dispersed fringes is suitable for stabilizing the optical path difference in ground-based astronomical optical interferometers in low light level situations. We discuss the performance of group delay tracking algorithms when the effects of atmospheric dispersion, high-frequency atmospheric temporal phase variations, non-ideal path modulation, non-ideal spectral sampling, and the detection artifacts introduced by electron-multiplying CCDs are taken into account, and we present ways in which the tracking capability can be optimized in the presence of these effects. 相似文献
6.
During the forthcoming years, ESO will implement a large number of CCDs in optical instruments for the Paranal and La Silla observatories. An important step in this process is the CCD characterization and optimization that is done after the device is received from the manufacturer. In order to accommodate the new large CCDs and to interface to the new FIERA controller, ESO is building a new CCD testing facility in Garching. Among the measurements that will be made with this new facility are: quantum efficiency, conversion factor, charge transfer efficiency, dark current, read out noise and cosmetic quality. 相似文献
7.
The charge diffusion is measured in back illuminated, fully depleted, 250 μm thick CCDs by imaging the diffraction pattern of a double slit. The CCDs studied are the focal plane detectors for the dark energy camera (DECam) instrument currently under construction for the dark energy survey (DES). The results presented here indicate that the dispersion of charge due to diffusion can be kept below the DES specification ( σ d ?<?7.0 μm ). 相似文献
8.
Gustavo Indalecio Cancelo Juan Cruz Estrada Guillermo Fernandez Moroni Ken Treptow Ted Zmuda H. Thomas Diehl 《Experimental Astronomy》2012,34(1):13-29
Scientific CCDs designed in thick high resistivity silicon (Si) are excellent detectors for astronomy, high energy and nuclear physics, and instrumentation. Many applications can benefit from CCDs ultra low noise readout systems. The present work shows how sub electron noise CCD images can be achieved using digital signal processing techniques. These techniques allow 0.4 electrons of noise at readout bandwidths of up to 10?Kpixels per second while keeping the full CCD spatial resolution and signal dynamic range. 相似文献
9.
V. Lapeyrere P. Bernardi J.-T. Buey M. Auvergne D. Tiphène 《Monthly notices of the Royal Astronomical Society》2006,365(4):1171-1179
CoRoT (Convection, Rotation and Transit) is a mission of high-accuracy photometry with two scientific programmes: asteroseismology and planet finding, using CCDs as detectors. Ten 2048×4096 CCDs manufactured by E2V (42-80) were calibrated on Meudon test bench in order to choose the best ones for flight. A very high instrument stability is needed. Taking into account the environmental perturbations (temperature, attitude control system jitter, radiations, etc.) we studied sensitivity of CCD gain and quantum efficiency to temperature and sensitivity of the output signal to bias voltages. Special attention was paid to pixel capacity and noise sources coming from dark current and pixel response non-uniformity. The calibration results together with the expected voltages and temperature fluctuations are compared with the specifications. 相似文献
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R.M. Ambrosi A.D. Holland D.R. Smith I.B. Hutchinson M. Denby 《Planetary and Space Science》2005,53(14-15):1449-1465
The increasing number of probes carrying large focal planes consisting of many charge-coupled devices (CCDs), planned to be sent to the L2 Lagrangian point, 1.5 million kilometres from Earth in the next 15 years, implies that a detailed study of the effects of the prompt particle environment at L2 on CCDs is required. The focus of this study will be on CCDs for optical astronomy, astrometry and photometric applications. This study will be of particular interest to GAIA the European Space Agency's (ESA) cornerstone optical astronomy mission to further explore and map sections of our galaxy in greater detail. The results will also have implications for future X-ray astronomy missions like the X-ray Evolving Universe Spectroscopy Mission (XEUS). Both the above missions will require large area focal planes incorporating many CCD detectors.The sources of the instrument background are both solar and galactic and if a probe is launched around the peak in the next solar cycle (2010), the possible false detection rate or the amount of data that could be lost during a mission must be determined. This paper presents measured data for a spacecraft in a geostationary orbit, specifically Geosynchronous Operational Environmental Satellites (GOES) data, and makes predictions of the flux and energy of the particle environment at L2. The solar and galactic cosmic ray background was determined by using the Cosmic Ray Effects on Micro-Electronics or CREME96 code. A comparison was then made between the GOES data and the output from the CREME96 code in order to make predictions about the L2 environment. 相似文献
12.
Alex Antunes David N. Burrows Gordon P. Garmire David H. Lumb John A. Nousek 《Experimental Astronomy》1993,4(2):159-175
The first generation of X-ray telescopes to use Charge-Coupled Devices (CCDs) is being launched this decade. With a read noise of a few electrons, CCDs provide Fano-limited spectral resolution across the soft X-ray band (0.1 – 10 keV). However, degradation of resolution due to charge transfer losses becomes noticeable as Charge Transfer Inefficiency (CTI) increases to 10–5. In this paper, we present a model which calculates the effects of radiation damage in low Earth orbit in order to predict CCD lifetimes over which good charge transfer is maintained. The model presented here considers damage mechanisms within the CCD, environmental conditions in which the CCD operates, and experiment shielding. We find that the predicted CTI approaches 10–5 after a one to two year mission for the flight instruments considered here. 相似文献
13.
James W. Beletic Sean Adkins Barry Burke Robert Reich Bernie Kosicki Vyshnavi Suntharalingham Charlie Bleau Ray DuVarney Richard Stover Jerry Nelson Francois Rigaut 《Experimental Astronomy》2005,19(1-3):103-109
All of the extremely large telescopes (ELTs) will utilize sodium laser guide star (LGS) adaptive optics (AO) systems. Most of these telescopes plan to use the Shack-Hartmann approach for wavefront sensing. In these AO systems, the laser spots in subapertures at the edge of the pupil will suffer from spot elongation due to the 10 km extent of the sodium layer and the large separation from the projection laser. This spot elongation will severely degrade the performance of standard geometry wavefront sensing systems. In this paper, we present a CCD with custom pixel morphology that aligns the pixels of each subaperture with the radial extension of the LGS spot. This CCD design will give better performance than a standard geometry CCDs for continuous wave lasers. In addition, this CCD design is optimal for a pulsed sodium laser. The pixel geometry enables each subaperture to follow a laser pulse traversing the sodium layer, providing optimal sampling of a limited number of detected photons. In addition to novel pixel layout, this CCD will also incorporate experimental JFET sense amplifiers and use CMOS design approaches to simplify the routing of biases, clocks and video output. This CCD will attain photon-noise limited performance at high frame rates, and is being incorporated in the plans for the Thirty Meter Telescope (TMT). 相似文献
14.
The University of California Observatories/Lick Observatory (UCO/Lick) has undertaken to produce science-grade CCDs for current and future instruments to be used on UCO/Lick and UCO/Keck telescopes. In this paper we describe the techniques developed and the progress achieved to date. 相似文献
15.
D. H. Lumb G. D. Berthiaume D. N. Burrows G. P. Garmire J. A. Nousek 《Experimental Astronomy》1991,2(3):179-201
The application of CCDs to X-ray imaging and spectroscopy for astronomy is described. The requirements which differ markedly from those of traditional optical applications are highlighted. Results of recent research programs to optimize CCD X-ray response are presented. It is shown that very high quantum efficiencies and Fano noise limited energy resolutions can be obtained. A number of issues related to the practical implementation of future instruments are reviewed. 相似文献
16.
A. De Groof D. Berghmans B. Nicula J.-P. Halain J.-M. Defise T. Thibert U. Schühle 《Solar physics》2008,249(1):147-163
CMOS-APS imaging detectors open new opportunities for remote sensing in solar physics beyond what classical CCDs can provide,
offering far less power consumption, simpler electronics, better radiation hardness, and the possibility of avoiding a mechanical
shutter. The SWAP telescope onboard the PROBA2 technology demonstration satellite of the European Space Agency will be the
first actual implementation of a CMOS-APS detector for solar physics in orbit. One of the goals of the SWAP project is precisely
to acquire experience with the CMOS-APS technology in a real-live space science context. Such a precursor mission is essential
in the preparation of missions such as Solar Orbiter where the extra CMOS-APS functionalities will be hard requirements. The current paper concentrates on specific CMOS-APS issues
that were identified during the SWAP preflight calibration measurements. We will discuss the different readout possibilities
that the CMOS-APS detector of SWAP provides and their associated pros and cons. In particular we describe the “image lag”
effect, which results in a contamination of each image with a remnant of the previous image. We have characterised this effect
for the specific SWAP implementation and we conclude with a strategy on how to successfully circumvent the problem and actually
take benefit of it for solar monitoring. 相似文献
17.
Photon counting strategies with low-light-level CCDs 总被引：1，自引：0，他引：1
A. G. Basden C. A. Haniff C. D. Mackay 《Monthly notices of the Royal Astronomical Society》2003,345(3):985-991
Low light level charge-coupled devices (L3CCDs) have recently been developed, incorporating on-chip gain. They may be operated to give an effective readout noise of much less than one electron by implementing an on-chip gain process allowing the detection of individual photons. However, the gain mechanism is stochastic and so introduces significant extra noise into the system. In this paper we examine how best to process the output signal from an L3CCD so as to minimize the contribution of stochastic noise, while still maintaining photometric accuracy.
We achieve this by optimizing a transfer function that translates the digitized output signal levels from the L3CCD into a value approximating the photon input as closely as possible by applying thresholding techniques. We identify several thresholding strategies and quantify their impact on the photon counting accuracy and the effective signal-to-noise ratio.
We find that it is possible to eliminate the noise introduced by the gain process at the lowest light levels. Reduced improvements are achieved as the light level increases up to about 20 photon pixel−1 and above this there is negligible improvement. Operating L3CCDs at very high speeds will keep the photon flux low, giving the best improvements in signal-to-noise ratio. 相似文献
We achieve this by optimizing a transfer function that translates the digitized output signal levels from the L3CCD into a value approximating the photon input as closely as possible by applying thresholding techniques. We identify several thresholding strategies and quantify their impact on the photon counting accuracy and the effective signal-to-noise ratio.
We find that it is possible to eliminate the noise introduced by the gain process at the lowest light levels. Reduced improvements are achieved as the light level increases up to about 20 photon pixel
18.
Alan Owens Michael Denby Mark R. Sims Oleg Terekhov Alan A. Wells 《Experimental Astronomy》1997,7(3):161-189
The requirements, philosophy and implementation of inorbit radiation shielding for the Charge Coupled Devices (CCDs) on-board the Joint European X-ray Telescope (JET-X) are described in detail. Relevant trade-offs between displacement damage, spectral degradation, instrument mass and mission lifetime are examined and a maximum permissible fluence at the CCDs derived. The calculations show that for the ambient JET-X radiation environment no benefit is obtained by increasing the shield thickness above 30 mm of aluminum due to the local production of cascade nucleons. However, a large flare of the August 1972 type will exceed the required maximum fluence by a factor of 2. In order to survive such a flare, a thicker shield is required. Because of mass constraints, JET-X will fly a composite shield composed of 20 mm of aluminum on the outside and 5 mm of tungsten on the inside. Such a shield is designed to ensure that the degradation in the CCD FWHM energy resolution is no more than 40% around the Fe line over the nominal two year mission lifetime (a factor of 2 x the intrinsic line broadening). The predicted degradation in energy resolution and the efficacy of the shield design has been recently verified by experiment (Owens et al., Nucl. Instr. and Meth., A361 (1995) 602). 相似文献
19.
R. Danner 《Experimental Astronomy》1993,4(2):105-116
Charged particle fluxes on satellites in highly eccentric Earth orbits are studied, using data from ISEE1 and EXOSAT missions. The effects of minimum-ionizing particles, low-energy electrons and secondary radiation produced by these particles on CCDs used as X-ray detectors are identified. A technique to discriminate events caused by minimum-ionizing particles from X-ray events is proposed. The need for a deflecting system against low-energy electrons with focusing X-ray optics is demonstrated. An expected secondary radiation spectrum behind a typical detector shielding based on Monte-Carlo-simulations is presented. For the EPIC detectors on XMM, detection rates due to this radiation environment are estimated. 相似文献
20.
I. Csabai L. Dobos M. Trencsni G. Herczegh P. Jzsa N. Purger T. Budavri A.S. Szalay 《Astronomische Nachrichten》2007,328(8):852-857
The last decade has seen a dramatic change in the way astronomy is carried out. The dawn of the the new microelectronic devices, like CCDs has dramatically extended the amount of observed data. Large, in some cases all sky surveys emerged in almost all the wavelength ranges of the observable spectrum of electromagnetic waves. This large amount of data has to be organized, published electronically and a new style of data retrieval is essential to exploit all the hidden information in the multiwavelength data. Many statistical algorithms required for these tasks run reasonably fast when using small sets of in‐memory data, but take noticeable performance hits when operating on large databases that do not fit into memory. We utilize new software technologies to develop and evaluate fast multidimensional indexing schemes that inherently follow the underlying, highly non‐uniform distribution of the data: they are layered uniform indices, hierarchical binary space partitioning, and sampled flat Voronoi tessellation of the data. These techniques can dramatically speed up operations such as finding similar objects by example, classifying objects or comparing extensive simulation sets with observations. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献