Hot pixel annealing behavior in CCDs irradiated at -84/spl deg/C

Marshall, C.J.; Marshall, P.W.; Waczynski, Augustyn; Polidan, Elizabeth; Johnson, Scott D.; Kimble, Randy A.; Reed, Robert A.; Delo, Gregory; Schlossberg, D. J.; Russell, Anne Marie; Beck, Terry; Wen, Yiting; Yagelowich, John; Hill, Robert J.

doi:10.1109/tns.2005.860731

Cited by 24 publications

(16 citation statements)

References 13 publications

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“…It can be observed that the A&A 595, A6 (2016) first decontamination was quite aggressive and resulted in room temperatures being reached which are typically high enough to achieve an anneal of some radiation damage effects (e.g. Goudfrooij et al 2009;Marshall et al 2005). It is not anticipated that the Gaia CCDs will be annealed in the future, but we note that this is possible if required.…”

Section: Fpa Temperature Stabilitymentioning

confidence: 81%

GaiaData Release 1

Crowley

Kohley

Hambly

et al. 2016

A&A

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The European Space Agency's Gaia satellite was launched into orbit around L2 in December 2013 with a payload containing 106 large-format scientific CCDs. The primary goal of the mission is to repeatedly obtain high-precision astrometric and photometric measurements of one thousand million stars over the course of five years. The scientific value of the down-linked data, and the operation of the onboard autonomous detection chain, relies on the high performance of the detectors. As Gaia slowly rotates and scans the sky, the CCDs are continuously operated in a mode where the line clock rate and the satellite rotation spin-rate are in synchronisation. Nominal mission operations began in July 2014 and the first data release is being prepared for release at the end of Summer 2016. In this paper we present an overview of the focal plane, the detector system, and strategies for on-orbit performance monitoring of the system. This is followed by a presentation of the performance results based on analysis of data acquired during a two-year window beginning at payload switch-on. Results for parameters such as readout noise and electronic offset behaviour are presented and we pay particular attention to the effects of the L2 radiation environment on the devices. The radiation-induced degradation in the charge transfer efficiency (CTE) in the (parallel) scan direction is clearly diagnosed; however, an extrapolation shows that charge transfer inefficiency (CTI) effects at end of mission will be approximately an order of magnitude less than predicted pre-flight. It is shown that the CTI in the serial register (horizontal direction) is still dominated by the traps inherent to the manufacturing process and that the radiation-induced degradation so far is only a few per cent. We also present results on the tracking of ionising radiation damage and hot pixel evolution. Finally, we summarise some of the detector effects discovered on-orbit which are still being investigated.

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Section: Fpa Temperature Stabilitymentioning

confidence: 81%

GaiaData Release 1

Crowley

Kohley

Hambly

et al. 2016

A&A

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“…Indeed, they reveal that the pixels with a dark current higher than θ were instantaneously (but only partially) annealed on these occasions. The faster annealing of hotter pixels as compared to the annealing of the "warm" ones has been noted by Polidan et al (2004) and studied by Marshall et al (2005). An interesting possibility inferred from the latter reference is that the hotter pixels of SODISM may be to some extent constantly self-annealing due to the lukecold (cool, but not very cold) operating temperature of its CCD.…”

Section: Evolution Of the Dark Current Distribution In Izmentioning

confidence: 80%

Dark signal correction for a lukecold frame-transfer CCD

Hochedez

Timmermans²,

Hauchecorne

et al. 2013

A&A

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Context. Astrophysical observations must be corrected for their imperfections of instrumental origin. When charge-coupled devices (CCDs) are used, their dark signal is one such hindrance. In their pristine state, most CCD pixels are cool, that is, they exhibit a low quasi-uniform dark current, which can be estimated and corrected for. In space, after having been hit by an energetic particle, pixels can turn hot, viz. they start delivering excessive, less predictable, dark current. The hot pixels therefore need to be flagged so that a subsequent analysis may ignore them. Aims. The image data of the PICARD-SODISM solar telescope require dark signal correction and hot pixel identification. Its E2V 42-80 CCD operates at −7.2• C and has a frame-transfer architecture. Both image and memory zones thus accumulate dark current during integration and readout time, respectively. These two components must be separated in order to estimate the dark signal for any given observation. This is the main purpose of the dark signal model presented in this paper. Methods. The dark signal time-series of every pixel was processed by the unbalanced Haar technique to timestamp when its dark signal changed significantly. In-between these instants, the two components were assumed to be constant, and a robust linear regression, with respect to integration time, provides first estimates and a quality coefficient. The latter serves to assign definitive estimates for this pixel and that period. Results. Our model is part of the SODISM Level 1 data production scheme. To confirm its reliability, we verified on dark frames that it leaves a negligible residual bias (5 e − ) and generates a small rms error (25 e − rms). We also examined the distribution of the image zone dark current. The cool pixel level is found to be 4.0 e − pxl −1 s −1 , in agreement with the predicted value. The emergence rate of hot pixels was investigated as well. It yields a threshold criterion at 50 e − pxl −1 s −1 . The growth rate is found to be on average ∼500 new hot pixels per day, that is, 4.2% of the image zone area per year. Conclusions. A new method for dark signal correction of a frame-transfer CCD operating near −10• C is described and applied. It allows making recommendations about the implementation and scientific usage of such CCDs. Moreover, aspects of the method (adaptation of the unbalanced Haar technique, dedicated robust linear regression) have a generic interest.

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“…We call "jump" a sudden (but permanent) increase in a pixel dark signal after proton interaction. Figure 9 shows the dark current of 1 pixel over time First element to explain that is that a jump can present an annealing [11], so it can be either transient (with rapid and strong annealing),or semi-permanent (with slow or delayed annealing), or permanent (without any annealing). Figure 11 shows both jump values and DSNU for Parasol satellite.…”

Section: Dark Signal Non Uniformity (Dsnu)mentioning

confidence: 99%

Radiation effects on image sensors

Bardoux

Penquer

Gilard

et al. 2017

International Conference on Space Optics — ICSO 2012

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Radiation is a major issue for satellite development, especially when using detectors, either for the mission itself, or for platform sensors. This paper will give CNES experience in the effects of radiations on detector and mission performances. Data from several satellites is presented (Earth observation, Astronomy, star trackers). We will make comparison between this data, to try to determine common behaviours. We will finish by describing the mitigation techniques against radiation effects.

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Hot pixel annealing behavior in CCDs irradiated at -84/spl deg/C

Cited by 24 publications

References 13 publications

GaiaData Release 1

GaiaData Release 1

Dark signal correction for a lukecold frame-transfer CCD

Radiation effects on image sensors

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