Noise and zero point drift in 1.7μm cutoff detectors for SNAP

Smith, Roger; Bebek, C.; Bonati, Marco; Brown, Matthew G.; Cole, David M.; Rahmer, Gustavo; Schubnell, M.; Seshadri, S. R.; Tarlè, G.

doi:10.1117/12.672616

Cited by 17 publications

(11 citation statements)

References 4 publications

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“…This last behaviour has been noted in several previous publications, such as references [4], [5] and [6], and implies the presence of time dependent correlations, which can be described by a frequency power spectrum. The connection between the time constant of trapping sites and the frequency power spectrum was first stated by reference [7], and a recent presentation can be found in the lectures of reference [8].…”

Section: Evolution With the Number Of Samplingsmentioning

confidence: 72%

Extraction of the frequency spectrum of the noise of a HAWAII2RG NIR detector and impact on low-flux measurements

et al. 2010

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The readout noise of a H2RG HgCdTe NIR detector from Teledyne is measured at a temperature T=110K. It is shown that a Fowler mode with n = 240 allows to reach a noise of 2.63e (single read). A description of the power spectrum in terms of 3 parameters reproduces the variation of the noise as a function the number of Fowler samples, as well as its dependence on the periodicity of the sampling. The variance of the noise decreases with frequency with an effective power of 0.62 in our measurement domain. The behaviour of the detector under different experimental conditions can then be predicted. THE APPARATUSThe measurements described in this paper were carried out in a dedicated setup built to evaluate Hawaii 2RG (HgCdTe) detectors from Teledyne. The detector was on loan from LBNL in view of the evaluation of its performance when used in a spectrograph for the JDEM project. 1 In the following measurements the cryostat is operated at a temperature of 110K with fluctuations smaller than 0.1 K. The polarisation of the substrate was chosen as V sub − V reset = 0.4 V in all the data analysed in this work. Additional experimental details are provided in a previous paper 2 where the conversion factor of our setup at T = 110K was evaluated to be 2.042 e/ADU for a single pixel. The goal of the present measurements is to lay the ground for a determination of the frequency distribution of the noise, so as to be able to predict the behaviour of the detector in different experimental conditions (Fowler samplings, interval between groups, etc...). The merit of the power spectrum analysis is also the link it provides with the physical processes in the CMOS semi-conductor, such as the trapping and detrapping of electrons with a distribution of time constants. THE MEASUREMENT METHODIn the 2Kx2K H2RG detector, a window of 31x31 pixels has been selected. The clock frequency is 100khz, and the time needed for the readout of 1 frame is δ = 17.5ms . The non destructive frame readouts are organised into groups of 250 frames, read at the clock frequency of 100kHz and separated by a time interval which can be tuned, with the clocking of the pixels stopped. Taking into account the readout of the frames, the periodicity of the readout of a given pixel between 2 consecutive groups varies from 5s to 13s. All the frames are stored on disk for further analysis. The noise is characterised by two variance measurements:• the frame to frame variance, with the readout interval of δ = 17.5ms for a window frame 31x31 as considered here, is convenient for a calibration (conversion gain) of the detector and its readout. It was studied in [2];

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Section: Evolution With the Number Of Samplingsmentioning

confidence: 72%

Extraction of the frequency spectrum of the noise of a HAWAII2RG NIR detector and impact on low-flux measurements

et al. 2010

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“…The lowest published values for the H2RG single CDS voltage noise at 100 kHz pixel read rate all cluster around 40 rms µV for the embedded perimeter reference pixels and also for a few outstanding SCAs. Gert Finger for SN 49 and SN 88 (4) and Roger Smith for SNAP H2RG SCAs (5) both report 8.2 rms e-corresponding to 40 rms µV for a node capacitance of 33 fF and Don Hall reports (6) 40 µV for JWST P&MT H2RGs. Active pixels generally exhibit substantial excess noise -Gert Finger reports (4) 60 to 80 µV for the Hawk-I H2RGs while Roger Smith (5) reports 135 µV for the 1.7 µm cutoff SNAP arrays.…”

Section: Overview Of the Uh Laboratory Test Programmentioning

confidence: 95%

“…Gert Finger for SN 49 and SN 88 (4) and Roger Smith for SNAP H2RG SCAs (5) both report 8.2 rms e-corresponding to 40 rms µV for a node capacitance of 33 fF and Don Hall reports (6) 40 µV for JWST P&MT H2RGs. Active pixels generally exhibit substantial excess noise -Gert Finger reports (4) 60 to 80 µV for the Hawk-I H2RGs while Roger Smith (5) reports 135 µV for the 1.7 µm cutoff SNAP arrays. However a few 2.5 µm cutoff H2RGs do have active pixel noise comparable to the reference pixel value -Gert Finger has reported 40 µV for the signal pixels in one such H2RG, SN 49.…”

Section: Overview Of the Uh Laboratory Test Programmentioning

confidence: 95%

Performance of the first HAWAII 4RG-15 arrays in the laboratory and at the telescope

Hall

Atkinson

Beletic

et al. 2012

High Energy, Optical, and Infrared Detectors for Astronomy V

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The primary goal of the HAWAII 4RG-15 (H4RG-15) development is to provide a 16 megapixel 4096x4096 format at significantly reduced price per pixel while maintaining the superb low background performance of the HAWAII 2RG (H2RG). The H4RG-15 design incorporates several new features, notably clocked reference output and interleaved reference pixel readout, that promise to significantly improve noise performance while the reduction in pixel pitch from 18 to 15 microns should improve transimpedance gain although at the expense of some degradation in full well and crosstalk. During the Phase-1 development, Teledyne has produced and screen tested six hybrid arrays. In preparation for Phase-2, the most promising of these are being extensively characterized in the University of Hawaii's (UH) ULBCam test facility originally developed for the JWST H2RG program. The end-to-end performance of the most promising array has been directly established through astronomical imaging observations at the UH 88-inch telescope on Mauna Kea. We report the performance of these Phase-1 H4RG-15s within the context of established H2RG performance for key parameters (primarily CDS read noise), also highlighting the improvements from the new readout modes.

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“…The significant progress in these areas is described elsewhere in these proceedings. 2,3 While InGaAs imagers are being considered for use in astronomical applications, 4 their use is not yet widespread. InGaAs is an established detector technology with a large commercial base.…”

Section: Introductionmentioning

confidence: 99%

Characterization of NIR InGaAs imager arrays for the JDEM SNAP mission concept

et al. 2006

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We present the results of a study of the performance of InGaAs detectors conducted for the SuperNova Acceleration Probe (SNAP) dark energy mission concept. Low temperature data from a nominal 1.7um cut-off wavelength 1kx1k InGaAs photodiode array, hybridized to a Rockwell H1RG multiplexer suggest that InGaAs detector performance is comparable to those of existing 1.7um cut-off HgCdTe arrays. Advances in 1.7um HgCdTe dark current and noise initiated by the SNAP detector research and development program makes it the baseline detector technology for SNAP. However, the results presented herein suggest that existing InGaAs technology is a suitable alternative for other future astronomy applications.

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Noise and zero point drift in 1.7μm cutoff detectors for SNAP

Cited by 17 publications

References 4 publications

Extraction of the frequency spectrum of the noise of a HAWAII2RG NIR detector and impact on low-flux measurements

Extraction of the frequency spectrum of the noise of a HAWAII2RG NIR detector and impact on low-flux measurements

Performance of the first HAWAII 4RG-15 arrays in the laboratory and at the telescope

Characterization of NIR InGaAs imager arrays for the JDEM SNAP mission concept

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