CMOS-APS Detectors for Solar Physics: Lessons Learned during the SWAP Preflight Calibration

Groof, A. De; Berghmans, D.; Nicula, B.; Halain, Jean-Philippe; Defise, Jean-Marc; Thibert, Tanguy; Schühle, U.

doi:10.1007/s11207-008-9175-y

Cited by 29 publications

(24 citation statements)

References 5 publications

(5 reference statements)

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“…As it happened in SWAP telescope (CMOS based) calibration [14], the FPA calibration for STC highlighted some unexpected phenomena in the detector behaviour not correlated with dark or photonic signals. These effects can be identified acquiring sequences of images, Fig.…”

Section: A Effects Identificationmentioning

confidence: 76%

CMOS detectors: lessons learned during the STC stereo channel preflight calibration

Simioni

Sio

Deppo

et al. 2017

International Conference on Space Optics — ICSO 2016

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The Stereo Camera (STC), mounted on-board the BepiColombo spacecraft, will acquire in push frame stereo mode the entire surface of Mercury. STC will provide the images for the global three-dimensional reconstruction of the surface of the innermost planet of the Solar System. The launch of BepiColombo is foreseen in 2018. STC has an innovative optical system configuration, which allows good optical performances with a mass and volume reduction of a factor two with respect to classical stereo camera approach. In such a telescope, two different optical paths inclined of ±20°, with respect to the nadir direction, are merged together in a unique off axis path and focused on a single detector. The focal plane is equipped with a 2k x 2k hybrid Si-PIN detector, based on CMOS technology, combining low read-out noise, high radiation hardness, compactness, lack of parasitic light, capability of snapshot image acquisition and short exposure times (less than 1 ms) and small pixel size (10 µm). During the preflight calibration campaign of STC, some detector spurious effects have been noticed. Analyzing the images taken during the calibration phase, two different signals affecting the background level have been measured. These signals can reduce the detector dynamics down to a factor of 1/4th and they are not due to dark current, stray light or similar effects. In this work we will describe all the features of these unwilled effects, and the calibration procedures we developed to analyze them.

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Section: A Effects Identificationmentioning

confidence: 76%

CMOS detectors: lessons learned during the STC stereo channel preflight calibration

Simioni

Sio

Deppo

et al. 2017

International Conference on Space Optics — ICSO 2016

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“…The average of each image has been plotted versus the off-pointing angle together with the corresponding ray-tracing model curve [9], the being normalized w.r.t. the Sun-cantered image average (0-arcmin off-point).…”

Section: Instrument Straylightmentioning

confidence: 99%

Performances of swap on-board PROBA-2

Halain

Berghmans

Defise

et al. 2017

International Conference on Space Optics — ICSO 2010

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“…The SWAP instrument was intensively tested and calibrated before launch (Defise et al, 2007, De Groof et al, 2008. Major measurements and outcomes of these calibration campaigns were:…”

Section: Introductionmentioning

confidence: 99%

The SWAP EUV Imaging Telescope. Part II: In-flight Performance and Calibration

et al. 2012

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Abstract. The Sun Watcher with Active Pixel System detector and Image Processing (SWAP) telescope was launched on 2 November 2009 onboard the ESA PROBA2 technological mission and has acquired images of the solar corona every one -two minutes for more than two years. The most important technological developments included in SWAP are a radiation-resistant CMOS-APS detector and a novel onboard data-prioritization scheme. Although such detectors have been used previously in space, they have never been used for long-term scientific observations on orbit.Thus SWAP requires a careful calibration to guarantee the science return of the instrument. Since launch we have regularly monitored the evolution of SWAP's detector response in-flight to characterize both its performance and degradation over the course of the mission. These measurements are also used to reduce detector noise in calibrated images (by subtracting darkcurrent). Since accurate measurements of detector dark-current require large telescope off-points, we have also monitored straylight levels in the instrument to ensure that these calibration measurements are not contaminated by residual signal from the Sun. Here we present the results of these tests, and examine the variation of instrumental response and noise as a function of both time and temperature throughout the mission.

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CMOS-APS Detectors for Solar Physics: Lessons Learned during the SWAP Preflight Calibration

Cited by 29 publications

References 5 publications

CMOS detectors: lessons learned during the STC stereo channel preflight calibration

CMOS detectors: lessons learned during the STC stereo channel preflight calibration

Performances of swap on-board PROBA-2

The SWAP EUV Imaging Telescope. Part II: In-flight Performance and Calibration

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