Blooming in H2RG arrays: laboratory measurements of a second brighter-fatter type effect in HgCdTe infrared detectors

Zengilowski, Gregory R.; Cabrera, Mario S.; McMurtry, Craig W.; Pipher, J. L.; Dorn, Meghan L.; Reilly, Nicholas S.; Danielle, Bovie,; Mainzer, Amy; Wong, Aileen; Lee, Donald

doi:10.1117/1.jatis.7.2.026002

Cited by 2 publications

(2 citation statements)

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“…If it shrinks significantly relative to that of a neighboring pixel, then new charge generated in that area has a larger probability to get collected in the neighboring pixel (with larger depletion region). The effect has been reported in ground testing of an H2RG near-infrared detector for Euclid (Plazas et al 2017(Plazas et al , 2018; see also Zengilowski et al 2021). The latter differ from the H2RG detectors used on JWST in terms of wavelength coverage, with the Euclid devices having a HgCdTe cutoff of 2.3 μm, while most JWST devices cut off at ∼5.2 μm.…”

Section: Introductionmentioning

confidence: 87%

An Algorithm to Mitigate Charge Migration Effects in Data from the Near Infrared Imager and Slitless Spectrograph on the James Webb Space Telescope*

Goudfrooij,

Grumm,

Volk

et al. 2024

PASP

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We present an algorithm that mitigates the effects of charge migration due to the “brighter-fatter effect” (BFE) that occurs for highly illuminated stars in the Teledyne HAWAII-2RG detectors used in the NIRCam, NIRISS, and NIRSpec science instruments aboard the James Webb Space Telescope (JWST). The impact of this effect is most significant for photometry and spectrophotometry of bright stars in data for which the point-spread function (PSF) is undersampled, which is the case for several observing modes of the NIRISS instrument. The main impact of BFE to NIRISS data is incorrect count rate determinations for pixels in the central regions of PSFs of bright stars due to jump detections that are caused by charge migration from peak pixels to surrounding pixels. The effect is especially significant for bright compact sources in resampled, distortion-free images produced by the drizzle algorithm: quantitatively, apparent flux losses of >50% can occur in such images due to BFE. We describe the algorithm of the “charge_migration” mitigation step that has been implemented in version 10.0 of the operational JWST calibration pipeline as of 2023 December 5. We illustrate the impact of this step in terms of the resulting improvements of the precision of imaging photometry of point sources. The algorithm renders the effects of BFE on photometry and surface brightness measurements to stay within 1%.

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Section: Introductionmentioning

confidence: 87%

An Algorithm to Mitigate Charge Migration Effects in Data from the Near Infrared Imager and Slitless Spectrograph on the James Webb Space Telescope*

Goudfrooij,

Grumm,

Volk

et al. 2024

PASP

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“…At SEL1, the Earth and Moon are sufficiently distant that their thermal radiation onto the spacecraft can be managed purely passively. Combined with the other thermal protections, this design allows the NEO Surveyor instrument performance to be limited by the natural astrophysical background in the NC2 channel (predominantly zodiacal dust emission; Leinert et al 1998;Wright 1998), with the telescope required to remain below 57 K. The NC2 detectors must be maintained below 40 K (McMurtry et al 2013;Dorn et al 2016;Zengilowski et al 2021Zengilowski et al , 2022 to ensure that their dark currents do not dominate over the minimum expected zodiacal background signal over the field of regard. The detectors are nonlinearly sensitive to temperature, and the temperature requirements are designed to limit heat input into the arrays.…”

Section: Mission Architecturementioning

confidence: 99%

The Near-Earth Object Surveyor Mission

Mainzer,

Masiero,

Abell

et al. 2023

Planet. Sci. J.

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The Near-Earth Object (NEO) Surveyor mission is a NASA Observatory designed to discover and characterize asteroids and comets. The mission’s primary objective is to find the majority of objects large enough to cause severe regional impact damage (>140 m in effective spherical diameter) within its 5 yr baseline survey. Operating at the Sun–Earth L1 Lagrange point, the mission will survey to within 45° of the Sun in an effort to find objects in the most Earth-like orbits. The survey cadence is optimized to provide observational arcs long enough to distinguish near-Earth objects from more distant small bodies that cannot pose an impact hazard reliably. Over the course of its survey, NEO Surveyor will discover ∼200,000–300,000 new NEOs down to sizes as small as ∼10 m and thousands of comets, significantly improving our understanding of the probability of an Earth impact over the next century.

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Blooming in H2RG arrays: laboratory measurements of a second brighter-fatter type effect in HgCdTe infrared detectors

Cited by 2 publications

References 20 publications

An Algorithm to Mitigate Charge Migration Effects in Data from the Near Infrared Imager and Slitless Spectrograph on the James Webb Space Telescope*

An Algorithm to Mitigate Charge Migration Effects in Data from the Near Infrared Imager and Slitless Spectrograph on the James Webb Space Telescope*

The Near-Earth Object Surveyor Mission

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