H2RG focal plane array and camera performance update

Blank, Richard; Anglin, Selmer; Beletic, James W.; Bhargava, S.; Bradley, Ryan; Cabelli, Craig A.; Chen, Jing; Cooper, Donald E.; Demers, Rick; Eads, M.; Farris, Mark; Lavelle, William F.; Luppino, Gerard A.; Moore, Eric; Piquette, E. C.; Ricardo, Raphael; Xu, Min; Zandian, Majid

doi:10.1117/12.926752

Cited by 31 publications

(24 citation statements)

References 2 publications

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“…The read noise observed is very flat with read frequency, as discussed by Blank et al 8 and shown in Figure 16. Therefore we should be able to read with essentially no penalty at 200 kHz, and do Fowler-64 sampling, which should reduce our noise to just above 3 electrons.…”

Section: Read Noisesupporting

confidence: 57%

The near infrared camera for the Subaru Prime Focus Spectrograph

et al. 2014

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We present the detailed design of the near infrared camera for the SuMIRe (Subaru Measurement of Images and Redshifts) Prime Focus Spectrograph (PFS) being developed for the Subaru Telescope. The PFS spectrograph is designed to collect spectra from 2394 objects simultaneously, covering wavelengths that extend from 380 nm -1.26 µm. The spectrograph is comprised of four identical spectrograph modules, with each module collecting roughly 600 spectra from a robotic fiber positioner at the telescope prime focus. Each spectrograph module will have two visible channels covering wavelength ranges 380 nm -640 nm and 640 nm -955 nm, and one near infrared (NIR) channel with a wavelength range 955 nm -1.26 µm. Dispersed light in each channel is imaged by a 300 mm focal length, f/1.07, vacuum Schmidt camera onto a 4k x 4k, 15 µm pixel, detector format. For the NIR channel a HgCdTe substrate-removed Teledyne 1.7 µm cutoff device is used. In the visible channels, CCDs from Hamamatsu are used. These cameras are large, having a clear aperture of 300 mm at the entrance window, and a mass of ∼ 250 kg.Like the two visible channel cameras, the NIR camera contains just four optical elements: a two-element refractive corrector, a Mangin mirror, and a field flattening lens. This simple design produces very good imaging performance considering the wide field and wavelength range, and it does so in large part due to the use of a Mangin mirror (a lens with a reflecting rear surface) for the Schmidt primary. In the case of the NIR camera, the rear reflecting surface is a dichroic, which reflects in-band wavelengths and transmits wavelengths beyond 1.26 µm. This, combined with a thermal rejection filter coating on the rear surface of the second corrector element, greatly reduces the out-of-band thermal radiation that reaches the detector.The camera optics and detector are packaged in a cryostat and cooled by two Stirling cycle cryocoolers. The first corrector element serves as the vacuum window, while the second element is thermally isolated and floats cold. An assembly constructed primarily of silicon carbide is used to mount the Mangin mirror, and to support the detector and field flattener. Thermal isolation between the cold optics and warm ambient surroundings is provided by G10 supports, multi-layer insulation, and the vacuum space within the cryostat.In this paper we describe the detailed design of the PFS NIR camera and discuss its predicted optical, thermal, and mechanical performance.

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Section: Read Noisesupporting

confidence: 57%

The near infrared camera for the Subaru Prime Focus Spectrograph

et al. 2014

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“…Parameters used in integration time calculations. We adopt the detector noise characteristics for a science grade Teledyne H2RG HgCdTe focal plane array cooled to 77 K (Blank et al 2012) and transmission estimates based on the KPIC instrument. The majority of Ross 128 b parameters are from Bonfils et al (2017).…”

Section: Keck Telescopementioning

confidence: 99%

“…The former is based on end-to-end transmission estimates of the Keck telescope and the KPIC instrument. The latter is representative of a Teledyne H2RG HgCdTe focal plane array (Blank et al 2012). However, these values can potentially be higher in a dedicated VFN instrument with fewer reflections, higher throughput spectrographs, and improved detectors.…”

Section: Uncertainty In Integration Time Calculationsmentioning

confidence: 99%

Efficient Spectroscopy of Exoplanets at Small Angular Separations with Vortex Fiber Nulling

Ruane

Mawet

et al. 2018

ApJ

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Instrumentation designed to characterize potentially habitable planets may combine adaptive optics and high-resolution spectroscopy techniques to achieve the highest possible sensitivity to spectral signs of life. Detecting the weak signal from a planet containing biomarkers will require exquisite control of the optical wavefront to maximize the planet signal and significantly reduce unwanted starlight. We present an optical technique, known as vortex fiber nulling (VFN), that allows polychromatic light from faint planets at extremely small separations from their host stars ( λ/D) to be efficiently routed to a diffraction-limited spectrograph via a single-mode optical fiber, while light from the star is prevented from entering the spectrograph. VFN takes advantage of the spatial selectivity of a single-mode fiber to isolate the light from close-in companions in a small field of view around the star. We provide theoretical performance predictions of a conceptual design and show that VFN may be utilized to characterize planets detected by radial velocity (RV) instruments in the infrared without knowledge of the azimuthal orientation of their orbits. Using a spectral template-matching technique, we calculate an integration time of ∼400, ∼100, and ∼30 hr for Ross 128 b with Keck, the Thirty Meter Telescope (TMT), and the Large Ultraviolet/Optical/Infrared (LUVOIR) Surveyor, respectively.

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“…The FPA identified for MOCSI is the Teledyne H2RG HgCdTe array (Blank et al, 2012), which has been used extensively in both ground-and space-based astronomy applications and features a 2,048 × 2,048 18-μm pitch detector array. Developed for the Near Infrared Spectrograph on the James Webb Space Telescope (Rowlands et al, 2010), it has four reference rows and columns around the perimeter of the FPA chip that provide common-mode noise rejection.…”

Section: Fpamentioning

confidence: 99%

Multi‐Order Carbon Spectral Imager: A Sensor Concept for Carbon Cycle Investigations

Hall

Leifer

Warren

et al. 2019

Earth and Space Science

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Despite their importance to climate change, significant current and future source uncertainties remain for the most important carbon greenhouse gases (GHGs) methane (CH4) and carbon dioxide (CO2), particularly for the developing world. Mitigation by effective regulation and treaties requires accurate global GHG budgets, which only global‐scale (satellite) remote sensing can deliver. A high spatial and spectral resolution spectrometer is needed; herein, we present the design concept for a Multi‐Order Carbon Spectral Imager (MOCSI). MOCSI is designed for the global measurement of differential GHG column density and source fingerprinting from low Earth orbit. MOCSI includes three wavebands for CH4, CO2, and carbon monoxide (CO), whose altitude weighting functions emphasize the boundary layer, where the dominant GHG anthropogenic and natural sources are still unmixed and therefore most easily discerned against background levels. CO aids discrimination of megacity and fire GHG emissions from other sources and is also a precursor for ozone, which is also an important GHG. High spectral resolution ensures discrimination of target species from interferents, while high spatial resolution enhances sensitivity for discrete source identification and emission quantification. MOCSI is a compact, high‐throughput shortwave‐infrared pushbroom spectrometer that disperses multiple orders of a single grating onto a single focal plane array to minimize size, weight, and power of the instrument. MOCSI is specified to provide spatial and temporal resolution and sensitivity sufficient to address important global science questions related to megacity emissions, shifts in hydrocarbon production, and disaster response, as well as many others.

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H2RG focal plane array and camera performance update

Cited by 31 publications

References 2 publications

The near infrared camera for the Subaru Prime Focus Spectrograph

The near infrared camera for the Subaru Prime Focus Spectrograph

Efficient Spectroscopy of Exoplanets at Small Angular Separations with Vortex Fiber Nulling

Multi‐Order Carbon Spectral Imager: A Sensor Concept for Carbon Cycle Investigations

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