Impact of common modes correlations and time sampling on the total noise of a H2RG near-IR detector

Kubik, B.; Barbier, R.; Castera, A.; Chabanat, E.; Ferriol, S.; Smadja, G.

doi:10.1117/12.2055071

Cited by 7 publications

(4 citation statements)

References 4 publications

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“…Since they have the same electronics as active pixels, they are subject to the same variations of the biases and temperatures as the active pixels. The aim is to correct the active pixels from these variations, by subtracting a linear combination of the signals measured by nearby reference pixels, as proposed by Bogna Kubik et al 8 for H2RG sensors. This correction is based on two steps.…”

Section: Correction With Reference Pixelsmentioning

confidence: 99%

Flux reconstruction for the NIR camera CAGIRE at the focus of the Colibrí telescope

Flèche

Atteia

Valentin

et al. 2022

X-Ray, Optical, and Infrared Detectors for Astronomy X

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CAGIRE is the near infrared camera of the Colibrí robotic telescope, designed for the follow-up of SVOM alerts, mainly Gamma Ray Bursts (GRBs), and the quick imaging of sky regions where transient sources are detected by the SVOM satellite. CAGIRE is based on the Astronomical Large Format Array (ALFA) 2k x 2k SWIR sensor from the French consortium CEA-LYNRED. In the context of CAGIRE the sensor is operated in "Up the Ramp" mode to observe the sky in a square field of view of 21.7 arcmin on a side, in the range of wavelengths from 1.1 to 1.8 µm. An observation with CAGIRE consists of a series of short (1-2 minutes) exposures during which the pixels are read out every 1.3 second, continuously accumulating charges proportionally to the received flux, building a ramp.The main challenge is to quickly process and analyse these ramps, in order to identify and study the near infrared counterparts of the bursts, within 5 minutes of the reception of an alert. Our preprocessing, which is under development, aims at providing reliable flux maps for the astronomy pipeline. It is based on a sequence of operations. First, calibration maps are used to identify saturated pixels, and for each pixel, the usable (non saturated) range of the ramp. Then, the ramps are corrected for the electronic common mode noise, and differential ramps are constructed. Finally, the flux is calculated from the differential ramps, using a previously calibrated map of pixel non-linearities. We present here the sequence of operations performed by the preprocessing, which are based on previous calibrations of the sensor response. These operations lead to the production of a flux map corrected from cosmic-rays hits, a map depicting the quality of the fit, a map of saturated pixels and a map of pixels hit by cosmic-rays, before the acquisition of the next ramp. These maps will be used by the astronomy pipeline to quickly extract the scientific results of the observations, like the identification of uncatalogued or quickly variable sources that could be GRB afterglows.

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Section: Correction With Reference Pixelsmentioning

confidence: 99%

Flux reconstruction for the NIR camera CAGIRE at the focus of the Colibrí telescope

Flèche

Atteia

Valentin

et al. 2022

X-Ray, Optical, and Infrared Detectors for Astronomy X

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“…Reference pixel correction has been defined and optimized previously in order to minimize noise. 4 Among the 16 detectors, two of them are used as an example to show some methods and results. Their flat field illuminations are shown in figure 1 where singular patterns may be observed.…”

Section: Detectorsmentioning

confidence: 99%

“…reference pixel correction has been applied to all pixels, 2. pixel selection has been applied as described above, but both "IPC" areas have been included here, 3. pixels have been grouped into larger pixels composed of 16x16 pixels, or 64x64 pixels, 4. the length of the ramps has been limited to 5000 ADU integrated flux so as to limit non-linearity effects, 5. many acquisitions taken at incoming fluxes varying from 4 e/s up to 52 e/s have been combined together to increase the statistics.…”

Section: Gain Per Pixelmentioning

confidence: 99%

Euclid flight H2RG IR detectors: per pixel conversion gain from on-ground characterization for the Euclid NISP instrument

Secroun¹,

Barbier

Buton

et al. 2018

High Energy, Optical, and Infrared Detectors for Astronomy VIII

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Euclid is a major ESA mission for the study of dark energy planned to launch in 2021. Euclid will probe the expansion history of the Universe using weak lensing and baryonic acoustic oscillations probes. A survey of 15,000 deg 2 of the sky with the instrument NISP (Near-Infrared Spectro-Photometer), in the 900-2100 nm band, will give both the photometric and spectrometric redshifts of tens of millions of galaxies. The 16 H2RG detectors of the NISP focal plane array are still being characterized at CPPM (Marseille). Already 16 out of 20 flight detectors have been tested and a straightforward analysis done. Performance of the dedicated test benches-in particular control of flux and temperature-as well as an overview of the test flow will be presented. This paper will present methods and some preliminary results on two detectors focusing on the determination of a per pixel conversion gain.

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“…NISP detectors consist of a matrix of 2040 × 2040 science pixels surrounded by a 4 pixel wide ring of reference pixels used to minimize correlated noise. 7 The detectors are read out by sidecar cold electronics provided by Teledyne on 32 channels at 100 kHz. Due to the nondestructive readout, each acquisition provides a ramp, i.e.…”

Section: Introductionmentioning

confidence: 99%

Euclid Near Infrared Spectro-Photometer: spatial considerations on H2RG detectors interpixel capacitance and IPC corrected conversion gain from on-ground characterization

Graët

Secroun²,

Barbier

et al. 2022

X-Ray, Optical, and Infrared Detectors for Astronomy X

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Euclid is a major ESA mission scheduled for launch in 2023-2024 to map the geometry of the dark Universe using two primary probes, weak gravitational lensing and galaxy clustering. Euclid 's instruments, a visible imager (VIS) and an infrared spectrometer and photometer (NISP) have both been designed and built by Euclid Consortium teams. The NISP instrument will hold a large focal plane array of 16 near-infrared H2RG detectors, which are key elements to the performance of the NISP, and therefore to the science return of the mission.Euclid NISP H2RG flight detectors have been individually and thoroughly characterized at Centre de Physique des Particules de Marseille (CPPM) during a whole year with a view to producing a reference database of performance pixel maps. Analyses have been ongoing and have shown the relevance of taking into account spatial variations in deriving performance parameters. This paper will concentrate on interpixel capacitance (IPC) and conversion gain. First, per pixel IPC coefficient maps will be derived thanks to single pixel reset (SPR) measurements and a new IPC correction method will be defined and validated. Then, the paper will look into correlation effects of IPC and their impact on the derivation of per super-pixel IPC-free conversion gain maps. Eventually, several conversion gain values will be defined over clearly distinguishable regions.

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Impact of common modes correlations and time sampling on the total noise of a H2RG near-IR detector

Cited by 7 publications

References 4 publications

Flux reconstruction for the NIR camera CAGIRE at the focus of the Colibrí telescope

Flux reconstruction for the NIR camera CAGIRE at the focus of the Colibrí telescope

Euclid flight H2RG IR detectors: per pixel conversion gain from on-ground characterization for the Euclid NISP instrument

Euclid Near Infrared Spectro-Photometer: spatial considerations on H2RG detectors interpixel capacitance and IPC corrected conversion gain from on-ground characterization

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