Advanced Characterization and Analysis of Random Telegraph Noise in CMOS Devices

Martín-Martínez, J.; Rodrı́guez, R.; Nafrı́a, Montserrat

doi:10.1007/978-3-030-37500-3_14

Cited by 4 publications

(4 citation statements)

References 46 publications

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“…RTN is the fluctuation of the signal between discrete levels as a consequence of the capture and emission of charges by defects or traps located very close to the Si-SiO 2 interface (Uren et al 1985). In scaled CMOS detectors, this trapping process causes a shift in the relation between the drain current of the MOS transistor and the gate voltage, discretely increasing or decreasing the offset level, which fluctuates as random trapping and de-trapping of charges, either electrons or holes (Martin-Martinez et al 2020).…”

Section: Bias Stability and 'Salt And Pepper' Effectmentioning

confidence: 99%

Scientific CMOS sensors in Astronomy: QHY600 and QHY411

Alarcon¹,

Licandro²,

Serra-Ricart³

et al. 2023

Preprint

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Scientific Complementary Metal-Oxide-Semiconductor (CMOS) detectors have developed quickly in recent years, owing to their low cost, high availability and some advantages over CCDs, such as high frame rate or typically lower readout noise. With the development of the first back-illuminated models, these sensors started to be used in astronomy, so it is worth studying their characteristics, advantages and weaknesses. In this paper, we present the results of the laboratory characterization of the IMX455M and IMX411 sensors, integrated into the QHY600 and QHY411 cameras respectively. These are large (36×24 and 54×40 mm) native 16-bit sensors with 3.76 𝜇m pixels sensitive in the optical range. Their quantum efficiency has been found to peak at 80% at 475 nm, 40% at 700 nm and 10% at 900 nm. Their linearity and photon transfer performance have been evaluated, as well as their dark behaviour. They showed a low dark current, but also the presence of warm pixels of about 0.024% in the QHY600 and 0.005% in the QHY411, which were proved to be stable and linear with exposure time. We have analysed in detail the effect of random telegraph noise, also called Salt & Pepper noise, one of the most important issues to be addressed with these two sensors, since it affects around 2% of the pixels in each exposure. Sky tests are also presented and the effect of this noise on astronomical images is discussed.

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Section: Bias Stability and 'Salt And Pepper' Effectmentioning

confidence: 99%

Scientific CMOS sensors in Astronomy: QHY600 and QHY411

Alarcon¹,

Licandro²,

Serra-Ricart³

et al. 2023

Preprint

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“…The RTN phenomenon in MOSFETs and the various characterization methods are discussed in more detail in Chapters 4 [53],7 [54],14 [55] and 18 [56] of this book.…”

Section: Random Telegraph Noise (Rtn)mentioning

confidence: 99%

Noise and Fluctuations in Fully Depleted Silicon-on-Insulator MOSFETs

Theodorou

Ghibaudo

2020

Noise in Nanoscale Semiconductor Devices

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“…RTN is the fluctuation of the signal between discrete levels as a consequence of the capture and emission of charges by defects or traps located very close to the Si-SiO 2 interface (Uren et al 1985). In scaled CMOS detectors, this trapping process causes a shift in the relationship between the drain current of the MOS transistor and the gate voltage, discretely increasing or decreasing the offset level, which fluctuates as random trapping and de-trapping of charges, either electrons or holes (Martin-Martinez et al 2020).…”

Section: Bias Stability and "Salt And Pepper" Effectmentioning

confidence: 99%

Scientific CMOS Sensors in Astronomy: IMX455 and IMX411

Alarcon¹,

Licandro²,

Serra³

et al. 2023

PASP

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Scientific complementary metal-oxide-semiconductor (CMOS) detectors have developed quickly in recent years thanks to their low cost and high availability. They also have some advantages over charge-coupled devices (CCDs), such as high frame rate or typically lower readout noise. These sensors started to be used in astronomy following the development of the first back-illuminated models. Therefore, it is worth studying their characteristics, advantages, and weaknesses. One of the most widespread CMOS sensors are those from the Sony IMX series, which are included in large astronomical survey projects based on small and fast telescopes because of their low cost, and capability for wide-field and high-cadence surveys. In this paper, we aim to characterize the IMX455M and IMX411M sensors, which are integrated into the QHY600 and QHY411 cameras, respectively, for use in astronomical observations. These are large (36 × 24 and 54 × 40 mm) native 16 bit sensors with 3.76 μm pixels and are sensitive in the optical range. We present the results of the laboratory characterization of both cameras. They showed a very low dark current of 0.011 and 0.007 e− px−1 s−1 @–10°C for the QHY600 and QHY411 cameras, respectively. They also show the presence of warm pixels, ∼0.024% in the QHY600 and 0.005% in the QHY411. Warm pixels proved to be stable and linear with exposure time, and are therefore easily corrected using dark frames. Pixels affected by the Salt & Pepper noise are ∼2% of the total and a method to correct for this effect is presented. Both cameras were attached to night telescopes and several on-sky tests were performed to prove their capabilities. On-sky tests demonstrate that these CMOS behave as well as CCDs of similar characteristics and (for example) they can attain photometric accuracies of a few mili-magnitudes.

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Advanced Characterization and Analysis of Random Telegraph Noise in CMOS Devices

Cited by 4 publications

References 46 publications

Scientific CMOS sensors in Astronomy: QHY600 and QHY411

Scientific CMOS sensors in Astronomy: QHY600 and QHY411

Noise and Fluctuations in Fully Depleted Silicon-on-Insulator MOSFETs

Scientific CMOS Sensors in Astronomy: IMX455 and IMX411

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