Interpixel crosstalk in Teledyne Imaging Sensors H4RG-10 detectors

Dudik, R. P.; Jordan, M.; Dorland, Bryan N.; Veillette, Daniel; Waczynski, Augustyn; Lane, Benjamin F.; Loose, Markus; Kan, Emily; Waterman, James; Rollins, Chris; Pravdo, Steve

doi:10.1364/ao.51.002877

Cited by 4 publications

(9 citation statements)

References 12 publications

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“…The discrepancy (1.2% versus 2.0%) that we see between the two methods is consistent with the findings of other authors. [28][29][30][31] PEC data from TIS gave a responsive quantum efficiency (RQE) of 65% at 100 mV of reverse bias and in the range from ∼4 to 9 μm, and in addition provided a cutoff wavelength of 10.6 μm at 30 K. It is important to note that these first three arrays did not include antireflection coating, thus 65% is very good (the theoretical maximum value possible is ∼75%). The UR has confirmed both the RQE (at 8 to 9 μm) and the half power cutoff wavelength with photometry of a black felt cloth of known temperature, through a cold pinhole of known dimensions and distance from the array, through a cold circular variable interference filter and a warm dewar window (Appendix).…”

Section: H1rg-16885mentioning

confidence: 99%

Development of sensitive long-wave infrared detector arrays for passively cooled space missions

et al. 2013

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Abstract. The near-earth object camera (NEOCam) is a proposed infrared space mission designed to discover and characterize most of the potentially hazardous asteroids larger than 140 m in diameter that orbit near the Earth. NASA has funded technology development for NEOCam, including the development of long wavelength infrared detector arrays that will have excellent zodiacal background emission-limited performance at passively cooled focal plane temperatures. Teledyne Imaging Sensors has developed and delivered for test at the University of Rochester the first set of approximately 10 μm cutoff, 1024 × 1024 pixel HgCdTe detector arrays. Measurements of these arrays show the development to be extremely promising: noise, dark current, quantum efficiency, and well depth goals have been met by this technology at focal plane temperatures of 35 to 40 K, readily attainable with passive cooling. The next set of arrays to be developed will address changes suggested by the first set of deliverables.

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Section: H1rg-16885mentioning

confidence: 99%

Development of sensitive long-wave infrared detector arrays for passively cooled space missions

et al. 2013

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“…Some measurements for H4RG-10 HgCdTe arrays indicated α on the order of 8 % resulting coupling out of the central pixel on the order of 35%. 23 If correction of IPC is not performed, this could result in erroneous conclusions and unnecessary imprecision from missions such as WFIRST. In the case of higher couplings, diagonal and second-neighbor couplings can rise to non-negligible levels.…”

Section: Discussionmentioning

confidence: 99%

“…In the case of higher couplings, diagonal and second-neighbor couplings can rise to non-negligible levels. 23 Figure 18 shows the PSF degradation that would be caused to the F405N WebbPSF in the presence of a static α = 8%. The FWHM would be expected to broaden from 2.080 pixels to 2.249 pixels.…”

Section: Discussionmentioning

confidence: 99%

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Point-spread Function Ramifications and Deconvolution of a Signal Dependent Blur Kernel Due to Interpixel Capacitive Coupling

Donlon¹,

Ninkov²,

Baum

2018

PASP

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Interpixel capacitance (IPC) is a deterministic electronic coupling that results in a portion of the collected signal incident on one pixel of a hybridized detector array being measured in adjacent pixels. Data collected by light sensitive HgCdTe arrays which exhibit this coupling typically goes uncorrected or is corrected by treating the coupling as a fixed point spread function. Evidence suggests that this IPC coupling is not uniform across different signal and background levels. This variation invalidates assumptions that are key in decoupling techniques such as Wiener Filtering or application of the Lucy-Richardson algorithm. Additionally, the variable IPC results in the point spread function (PSF) depending upon a star's signal level relative to the background level, among other parameters. With an IPC ranging from 0.68% to 1.45% over the full well depth of a sensor, as is a reasonable range for the H2RG arrays, the FWHM of the JWSTs NIRCam 405N band is degraded from 2.080 pix (0.132") as expected from the diffraction pattern to 2.186 pix (0.142") when the star is just breaching the sensitivity limit of the system. For example, When attempting to use a fixed PSF fitting (e.g. assuming the PSF observed from a bright star in the field) to untangle two sources with a flux ratio of 4:1 and a center to center distance of 3 pixels, flux estimation can be off by upwards of 1.5% with a separation error of 50 millipixels. To deal with this issue an iterative non-stationary method for deconvolution is here proposed, implemented, and evaluated that can account for the signal dependent nature of IPC.

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“…Several experimental protocols have been used to characterize IPC, some through the illumination of a single pixel with 55 Fe sources 15 or taking advantage of cosmic ray hits, 16 others using electrical charge generation in hot pixels 17 or even through single pixel reset (SPR), a technique using an HxRG dedicated feature allowing the reset of a single pixel to a voltage different from its neighbors, 18 which are reset at 300mV. This latter technique is the only one that can actually decorrelate IPC from charge drifting and allows per pixel IPC coefficients estimation.…”

Section: Derivation Of Ipc Coefficientsmentioning

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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Interpixel crosstalk in Teledyne Imaging Sensors H4RG-10 detectors

Cited by 4 publications

References 12 publications

Development of sensitive long-wave infrared detector arrays for passively cooled space missions

Development of sensitive long-wave infrared detector arrays for passively cooled space missions

Point-spread Function Ramifications and Deconvolution of a Signal Dependent Blur Kernel Due to Interpixel Capacitive Coupling

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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