Characterization of flight detector arrays for the wide-field infrared survey explorer

Mainzer, Amy; Larsen, M. F.; Stapelbroek, M. G.; Hogue, Henry H.; Garnett, James D.; Zandian, Majid; Mattson, Reed; Masterjohn, S.; Livingston, John H.; Lingner, Nicole; Alster, Natali; Ressler, Michael E.; Masci, Frank J.

doi:10.1117/12.789585

Cited by 12 publications

(10 citation statements)

References 9 publications

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“…The alloy used for these detectors, Hg 1−x Cd x Te, has the x composition parameter (molar concentration of Cd) varied to reach different cutoff wavelengths. The band gap energy (in eV) of this semiconductor at a temperature in degrees Kelvin is given by 4 E g (x, T ) = −0.302 + 1.93x − 0.81x 2 + 0.832x 3…”

Section: Mercury Cadmium Telluride (Hgcdte)mentioning

confidence: 99%

Development of 13-μm cutoff HgCdTe detector arrays for astronomy

Cabrera

McMurtry

Dorn

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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Building on the successful development of the 10 µm HgCdTe detector arrays for the proposed NEOCam mission, the University of Rochester Infrared Detector team and Teledyne Imaging Systems are working together to extend the cutoff wavelength of HgCdTe detector arrays initially to 13 µm, with the ultimate goal of developing 15 µm HgCdTe detector arrays for space and ground-based astronomy. The advantage of HgCdTe detector arrays is that they can operate at higher temperatures than the currently used arsenic doped silicon detector arrays at the longer wavelengths. Our infrared detector team at the University of Rochester has received and tested four 13 µm detector arrays from Teledyne Imaging Systems with three different pixel designs, two of which are meant to reduce quantum tunneling dark current. The pixel design of one of these arrays has mitigated the effects of quantum tunneling dark currents for which we have been able to achieve, at a temperature of 28 K and applied bias of 350 mV, a well depth of at least 75 ke − for 90% of the pixels with a median dark current of 1.8 e − /sec. These arrays have demonstrated encouraging results as we move forward to extending the cutoff wavelength to 15 µm.

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Section: Mercury Cadmium Telluride (Hgcdte)mentioning

confidence: 99%

Development of 13-μm cutoff HgCdTe detector arrays for astronomy

Cabrera

McMurtry

Dorn

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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“…[10][11][12][13] For NEOCam, the fabrication of a mosaic of 1024 × 1024 HgCdTe arrays operating out to 10 μm is required to enable its wide-field survey. TIS's HAWAII-1RG (H1RG) readout integrated circuit (ROIC) technology was selected for NEOCam based on the readout family's heritage in spaceand ground-based astronomical applications, including WISE, 14 the Hubble space telescope's wide-field camera-3, 15 and the JWST. 16,17 The HAWAII arrays have demonstrated the low power dissipation needed to support passive cooling as well as the low noise performance required to detect faint, natural background-limited astronomical sources and the narrow range of actual detector biases needed for operation of longer-wave HgCdTe photodiodes with a source-follower per detector ROIC.…”

mentioning

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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“…In an analysis of SPICA's pointing control system (Mitani et al, 2014), two potential noise sources were identi¯ed in the pointing error. The¯rst is vibrations at mid-frequencies (between 0.03 and $1 Hz).…”

Section: E®ects Of the Pointing Errormentioning

confidence: 99%

“…Performances of detectors. Sb array, and the read noise is obtained fromMainzer et al (2008) for the WISE detector which adopts the same read-out IC. Detective quantum e±ciencies are taken from Khalap & Hogue (2012) (KH2012 in this table and hereafter).…”

mentioning

confidence: 99%

Performance Estimation of the Mid-Infrared Camera and Spectrometer Aboard SPICA

Kataza

Sakon

Wada

et al. 2015

J. Astron. Instrum.

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The Space Infrared Telescope for Cosmology and Astrophysics (SPICA) is an astronomical mission optimized for mid- and far-infrared astronomy, envisioned for launch in the 2020s. The Mid-infrared Camera and Spectrometer (MCS) is a model instrument that covers the 5–38[Formula: see text][Formula: see text]m wavelength range and enables imaging and spectroscopic observations via four modules named WFC-S, WFC-L, HRS, and MRS. Both of the wide field camera (WFC) modules have a 5-arcmin square field of view (FOV) but cover different wavelength ranges; WFC for the short wavelength region (WFC-S) covers 5 to 24[Formula: see text][Formula: see text]m, whereas WFC for the long wavelength region (WFC-L) covers 18 to 38[Formula: see text][Formula: see text]m. The High Resolution Spectrometer (HRS) covers the 12–18[Formula: see text][Formula: see text]m range with a resolving power of 22,000–30,000, and the Mid Resolution Spectrometer (MRS) performs integral filed units spectroscopy with a 12[Formula: see text] by 8[Formula: see text] FOV. MRS simultaneously covers the 12–38[Formula: see text][Formula: see text]m range with a moderate resolving power of 720–2000. Here, we report sensitivity estimates from a detailed modeling process involving the instrument itself, the telescope, environmental conditions, and the system error budgets. We show that the WFC-S and HRS modules require an adaptive system to correct for telescope pointing error. In particular, band pass filters (BPFs) longer than 26[Formula: see text][Formula: see text]m should be developed.

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Characterization of flight detector arrays for the wide-field infrared survey explorer

Cited by 12 publications

References 9 publications

Development of 13-μm cutoff HgCdTe detector arrays for astronomy

Development of 13-μm cutoff HgCdTe detector arrays for astronomy

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

Performance Estimation of the Mid-Infrared Camera and Spectrometer Aboard SPICA

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