The SAFARI detector system

Audley, M. D.; Lange, Gert de; Gao, J. R.; Jackson, B. D.; Hijmering, R. A.; Ridder, M.; Bruijn, M. P.; Roelfsema, Peter; Ade, Peter A. R.; Withington, S.; Bradford, C. M.; Trappe, N.

doi:10.1117/12.2313361

Cited by 8 publications

(3 citation statements)

References 26 publications

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“…In each of the 4 grating modules the dispersed optical signal is recorded by 5 arrays of TES bolometers with a sensitivity close to background-limited. 2 The 5 arrays record spatially different signals from the sky but are co-aligned across the grating modules. Each array of 147 individual bolometers constitutes a spaxel, each spectral element (bolometer) in the spaxel is a spectral pixel.…”

Section: Safari Descriptionmentioning

confidence: 99%

“…1 The SPICA Far Infrared Spectrometer (SAFARI) will improve on the spectral line sensitivity of previous missions (the Herschel and Spitzer space telescopes) by taking advantage of a cold telescope and unprecedentedly sensitive detectors. 2 Being a very sensitive spectrometer SAFARI reveals the physical phenomena occurring within an obscured environment. SAFARI opens the window to the very distant Universe as well as nearby star and planet formation.…”

Section: Introductionmentioning

confidence: 99%

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Calibration strategy for the SPICA/SAFARI instrument

Shipman,

Vandenbussche,

Castillo-Dominguez

et al. 2021

Preprint

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SPICA is a mid to far infra-red space mission to explore the processes that form galaxies, stars and planets. SPICA/SAFARI is the far infrared spectrometer that provides near-background limited observations between 34 and 230 micrometers. The core of SAFARI consists of 4 grating modules, dispersing light onto 5 arrays of TES detectors per module. The grating modules provide low resolution (250) instantaneous spectra over the entire wavelength range. The high resolution (1500 to 12000) mode is accomplished by placing a Fourier Transform Spectrometer (FTS) in front of the gratings. Each grating module detector sees an interferogram from which the high resolution spectrum can be constructed. SAFARI data will be a convolution of complex spectral, temporal and spatial information. Along with spectral calibration accuracy of < 1 %, a relative flux calibration of 1% and an absolute flux calibration accuracy of 10% are required. This paper will discuss the calibration strategy and its impact on the instrument design of SAFARI

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Section: Safari Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Calibration strategy for the SPICA/SAFARI instrument

Shipman,

Vandenbussche,

Castillo-Dominguez

et al. 2021

Preprint

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“…SPICA's prime instrument is the SAFARI (SPICA Far-infrared Instrument) spectrometer. SAFARI will cover the spectral range λ = 34-230 µm simultaneously with four grating modules, each containing a diffraction grating and linear detector 1 3 array to sample the dispersed spectrum [2]. The dispersed spectra are measured with linear arrays of transition-edge sensor [3] (TES) bolometers.…”

Section: Introductionmentioning

confidence: 99%

SQUID Noise in a 176-Pixel FDM Demonstrator for the SAFARI Far-Infrared Spectrometer

et al. 2020

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Characterizing the optical response of ultra-low-noise far-infrared 60–110 μm transition edge sensors

Williams

Withington

Goldie

et al. 2020

Review of Scientific Instruments

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Far-infrared Transition Edge Sensors (TESs) are being developed for the SAFARI grating spectrometer on the cooled-aperture space telescope SPICA. In support of this work, we have devised a cryogenic (90 mK) test facility for carrying out precision optical measurements on ultra-low-noise TESs. Although our facility is suitable for the whole of the SAFARI wavelength range, 34 µm–230 µm, we focus on a representative set of measurements at 60 µm–110 µm using a device having a noise equivalent power of 0.32 aW Hz−1/2. The system is able to perform a range of measurements: (i) dark electrical characterization, (ii) optical efficiency with respect to a partially coherent beam having a modal composition identical to that of an ideal imaging telescope, (iii) optical saturation and dynamic range, (iv) fast optical transient response to a modulated thermal source, and (v) optical transient response in the presence of high-level background loading. We describe dark measurements to determine the operating characteristics of a TES and then compare the predicted optical behavior with the measured optical behavior. By comparing electrical and optical transient responses, we were able to observe thermalization in the device. We comment on the challenge of eliminating stray light.

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The SAFARI detector system

Cited by 8 publications

References 26 publications

Calibration strategy for the SPICA/SAFARI instrument

Calibration strategy for the SPICA/SAFARI instrument

SQUID Noise in a 176-Pixel FDM Demonstrator for the SAFARI Far-Infrared Spectrometer

Characterizing the optical response of ultra-low-noise far-infrared 60–110 μm transition edge sensors

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