Fabrication and characterization of a high performance NIR 2kx2k MCT array at CEA and Lynred for astronomy applications

Gravrand, O.; Lobre, C.; Santailler, Jean‐Louis; Goff, T. Le; Baier, N.; Badano, G.; Boulade, O.; Pichon, Thibault; Flèche, Alix Nouvel de la; Sam-Giao, Diane; Maltere, Alexandre; Aufranc, Sébastien; Salvetti, F.; Roumegoux, Julien; Brosse, Benoit; Lamoure, Adrien

doi:10.1117/12.2618857

Cited by 4 publications

(3 citation statements)

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“…Different strategies have been implemented to mitigate the impact of these amplifiers. Some of them are based on the ROIC design (Blank et al 2011; Gravrand et al 2022). Optical shields are added in the architecture of the ROIC to prevent the light from reaching the light‐sensitive layer.…”

Section: Glow In Infrared Detector Arraysmentioning

confidence: 99%

Pixel source follower glow in HxRG detector

Pichon

Boucher

2023

Astron Nachr

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The Atmospheric Remote‐Sensing Infrared Exoplanet Large‐survey (ARIEL) space mission is dedicated to the study of the exoplanets' atmosphere. To do so, the payload module is made of two instruments. The ARIEL InfraRed Spectrometer instruments is one them, it will perform spectroscopic measurements from the near‐infrared domain to the long‐wave infrared domain. The instrument relies on the use of two H1RG detectors. During early phases of instrument development dark current measurements have been done on an 8 m cutoff detector operated in window mode. These measurements revealed an unexpected level of dark current. This observation triggered a joint series of tests at the European Space Agency technical center and at the Astrophysics Department of the Atomic Energy Commission. As demonstrated in this paper, the excess of dark current originates from the collection, by the photosenstive layer, of light emitted by the source follower transistor of the pixel unit cell. This effect is referred as glow. Based on experimental results, this glow is studied as a function of the detector operating conditions (temperature, biases, timing diagram). These results also show that for the range of operating temperatures considered, the dark current performance of the detector is limited by the glow.

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Section: Glow In Infrared Detector Arraysmentioning

confidence: 99%

Pixel source follower glow in HxRG detector

Pichon

Boucher

2023

Astron Nachr

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“…In finding and obtaining data types, a basis or foundation is needed (Scott, 1970), including; integrated flux (Gravrand et al, 2022), photometric information classified by filter (Chatterjee et al, 2022), foundation or base can be obtained from 2 raw materials for astronomical research, namely; spectrum and image. The luminosity or brightness of various light objects in the universe as a function of time can be classified as a data type.…”

Section: Data Function and Time Seriesmentioning

confidence: 99%

Statistical Data Retrieval Technique in Astronomy Computational Physics

Siagian

Pribadi²,

Sinaga

et al. 2023

JATISI

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Computational astronomy is a very important branch in today's era, where physicists or researchers can use computers to process statistics in astronomical physics. researchers can process abstract data from raw data and can convert data into data visualizations. Computational physics astronomy is a sophisticated and well-established method, this branch of science can provide and process data, solve complex problems, and is very helpful for statisticians and computer scientists. Astronomical physicists have many problems, among others; there is a problem that is hierarchical, and complex, so that this paper will provide a basis for methods for optimizing methods in processing statistical data on physics. The author's hope is that astronomical physicists can perform an important and effective processing of astronomical data optimally and effectively.

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“…The camera CAGIRE is equipped with an Astronomical Large Format Array (ALFA) detector of 2048 by 2048 square pixels of 15 µm on a side, manufactured by the French company LYNRED, and based on the MCT (Mercury Cadmium Telluride) technology developed at CEA-LETI. 5 The detector covers a spectral range from 0.8 µm to 2.1 µm, 6 justifying the need for a blocking filter for wavelengths longer than 1.8 µm on CAGIRE. The detection layer in HgCdTe (MCT) is hybridized with indium bumps on a Read Out Integration Circuit (ROIC), designed and manufactured by LYNRED.…”

Section: The Alfa Sensormentioning

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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Fabrication and characterization of a high performance NIR 2kx2k MCT array at CEA and Lynred for astronomy applications

Cited by 4 publications

References 0 publications

Pixel source follower glow in HxRG detector

Pixel source follower glow in HxRG detector

Statistical Data Retrieval Technique in Astronomy Computational Physics

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

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