Detector arrays for the James Webb Space Telescope near-infrared spectrograph

Rauscher, Bernard J.; Alexander, David; Brambora, Clifford; Derro, Rebecca J.; Engler, Chuck; Fox, O.; Garrison, Matthew; Henegar, Greg; Hill, Robert J.; Johnson, Thomas E.; Lindler, Don J.; Manthripragada, Sridhar S.; Marshall, C.J.; Mott, Brent; Parr, Thomas M.; Roher, Wayne D.; Shakoorzadeh, Kamdin B.; Smith, M. D.; Waczynski, Augustyn; Wen, Yiting; Wilson, Donna; Xia‐Serafino, Wei; Cabelli, Craig A.; Cheng, E. S.; Garnett, James D.; Loose, Markus; Zandian, Majid; Zino, Joseph; Ellis, Timothy A.; Howe, Bryan; Jurado, Mirium; Lee, Ginn; Nieznanski, John; Wallis, P. M.; York, James; Regan, Michael W.; Bagnasco, Georgio; Marchi, Guido De; Ferruit, Pierre; Jakobsen, P.; Strada, Paolo

doi:10.1117/12.731759

Cited by 13 publications

(8 citation statements)

References 2 publications

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“…5,6 The detector can be operated with 1, 4, or 32 output channels. When used in the four output configuration each of four 512 × 2048 stripes is coupled to a single output.…”

Section: The Hawaii-2rg Detectormentioning

confidence: 99%

Reducing the read noise of H2RG detector arrays: eliminating correlated noise with efficient use of reference signals

et al. 2010

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We present a process for characterizing the correlation properties of the noise in large two-dimensional detector arrays, and describe an efficient process for its removal. In the case of the 2k × 2k HAWAII-2RG detectors (H2RG) detectors from Teledyne which are being used on the Near Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST), we find that we can reduce the read noise by thirty percent. Noise on large spatial scales is dramatically reduced. With this relatively simple process, we provide a performance improvement that is equivalent to a significant increase in telescope collecting area for high resolution spectroscopy with NIRSpec.

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“…5,6 The detector can be operated with 1, 4, or 32 output channels. When used in the four output configuration each of four 512 × 2048 stripes is coupled to a single output.…”

Section: The Hawaii-2rg Detectormentioning

confidence: 99%

Reducing the read noise of H2RG detector arrays: eliminating correlated noise with efficient use of reference signals

et al. 2010

Self Cite

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“…Many astronomical instruments have used conventional charge coupled devices (CCDs), segmented CCDs, or hybrid complementary metal oxide semiconductor (CMOS) focal plane arrays. [3][4][5][6][7][8][9][10] Conventional CCDs and hybrid VIS/IR CMOS 11,12 devices have been the preferred focal plane arrays for both ground-based and spacebased telescopes and visible/IR photometric instruments. Conventional CCDs have the advantage of being generally easier to characterize due to their extremely simple design.…”

Section: Detector Candidatesmentioning

confidence: 99%

Technology advancement of the CCD201-20 EMCCD for the WFIRST coronagraph instrument: sensor characterization and radiation damage

Harding

Demers

Hoenk

et al. 2015

J. Astron. Telesc. Instrum. Syst

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The Wide Field InfraRed Survey Telescope-Astrophysics Focused Telescope Asset (WFIRST-AFTA) mission is a 2.4-m class space telescope that will be used across a swath of astrophysical research domains. JPL will provide a high-contrast imaging coronagraph instrumentone of two major astronomical instruments. In order to achieve the low noise performance required to detect planets under extremely low flux conditions, the electron multiplying charge-coupled device (EMCCD) has been baselined for both of the coronagraph's sensorsthe imaging camera and integral field spectrograph. JPL has established an EMCCD test laboratory in order to advance EMCCD maturity to technology readiness level-6. This plan incorporates full sensor characterization, including read noise, dark current, and clock induced charge. In addition, by considering the unique challenges of the WFIRST space environment, degradation to the sensor's charge transfer efficiency will be assessed, as a result of damage from high-energy particles such as protons, electrons, and cosmic rays. Science-grade CCD201-20 EMCCDs have been irradiated to a proton fluence that reflects the projected WFIRST orbit. Performance degradation due to radiation displacement damage is reported, which is the first such study for a CCD201-20 that replicates the WFIRST conditions. In addition, techniques intended to identify and mitigate radiation-induced electron trapping, such as trap pumping, custom clocking, and thermal cycling, are discussed.

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“…Robberto 2007), which permits the information from multiple reads of a detector during a single integration to be summarized by a single total pixel numberN pix -sized frame. In contrast, "Sample Up the Ramp" (SUR) methods offer larger signal-to-noise ratios in a given integration time (Garnett & Forrest, 1993), as well as the ability to identify and reject cosmic ray and other transient events, at the cost of significantly increased data volumes (Rauscher et al, 2007). In order to implement SUR algorithms in telemetry-constrained applications, some amount of data processing and reduction must be performed on-board.…”

Section: Introductionmentioning

confidence: 99%

An Algorithm for Real-Time Optimal Photocurrent Estimation including Transient Detection for Resource-Constrained Imaging Applications

Zemcov,

Crill,

Ryan

et al. 2016

Preprint

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Mega-pixel charge-integrating detectors are common in near-IR imaging applications. Optimal signal-to-noise ratio estimates of the photocurrents, which are particularly important in the low-signal regime, are produced by fitting linear models to sequential reads of the charge on the detector. Algorithms that solve this problem have a long history, but can be computationally intensive. Furthermore, the cosmic ray background is appreciable for these detectors in Earth orbit, particularly above the Earth's magnetic poles and the South Atlantic Anomaly, and on-board reduction routines must be capable of flagging affected pixels. In this paper we present an algorithm that generates optimal photocurrent estimates and flags random transient charge generation from cosmic rays, and is specifically designed to fit on a computationally restricted platform. We take as a case study the Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer (SPHEREx), a NASA Small Explorer astrophysics experiment concept, and show that the algorithm can easily fit in the resourceconstrained environment of such a restricted platform. Detailed simulations of the input astrophysical signals and detector array performance are used to characterize the fitting routines in the presence of complex noise properties and charge transients. We use both Hubble Space Telescope Wide Field Camera-3 and Wide-field Infrared Survey Explorer to develop an empirical understanding of the susceptibility of near-IR detectors in low earth orbit and build a model for realistic cosmic ray energy spectra and rates. We show that our algorithm generates an unbiased estimate of the true photocurrent that is identical to that from a standard line fitting package, and characterize the rate, energy, and timing of both detected and undetected transient events. This algorithm has significant potential for imaging with charge-integrating detectors in astrophysics, earth science, and remote sensing applications.

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Detector arrays for the James Webb Space Telescope near-infrared spectrograph

Cited by 13 publications

References 2 publications

Reducing the read noise of H2RG detector arrays: eliminating correlated noise with efficient use of reference signals

Reducing the read noise of H2RG detector arrays: eliminating correlated noise with efficient use of reference signals

Technology advancement of the CCD201-20 EMCCD for the WFIRST coronagraph instrument: sensor characterization and radiation damage

An Algorithm for Real-Time Optimal Photocurrent Estimation including Transient Detection for Resource-Constrained Imaging Applications

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