14 - pixel , multiplexed array of gamma-ray microcalorimeters with 47eV energy resolution at 103keV

Abstract

The authors present a prototype for a high-energy-resolution, high-count-rate, gamma-ray spectrometer intended for nuclear forensics and international nuclear safeguards. The prototype spectrometer is an array of 14 transition-edge-sensor microcalorimeters with an average energy resolution of 47 eV ͑full width at half maximum͒ at 103 keV. The resolution of the best pixel is 25 eV. A cryogenic, time-division multiplexer reads out the array. Several important topics related to microcalorimeter arrays are discussed, including cross-talk, the uniformity of detector bias conditions, fabrication of the arrays, and the multiplexed readout. The measurements and calculations demonstrate that a kilopixel array of high-resolution microcalorimeters is feasible.

A superconducting focal plane array for ultraviolet, optical, and near-infrared astrophysics

“…Cryogenic detectors are currently the preferred technology for astronomical observations over most of the electromagnetic spectrum, notably in the far infrared through millimeter (0.1-3 mm) [1,2,3], X-ray [4], and gamma-ray [5] wavelength ranges. In the important ultraviolet, optical, and near infrared (0.1-5 µm) wavelength range a variety of detector technologies based on semiconductors, backed by large investment from both consumer and military customers, has resulted in detectors for astronomy with large formats, high quantum efficiency, and low readout noise.…”

Direct Detection of Pu-242 with a Metallic Magnetic Calorimeter Gamma-Ray Detector

“…Cryogenic γ -detectors can overcome some of the limitations of HPGe detectors in nuclear safeguards due to their higher energy resolution and higher peak-tobackground ratio [3][4][5][6][7][8]. This motivates our development of γ -detectors based on metallic magnetic calorimeters [8].…”

ARCONS: A 2024 Pixel Optical through Near-IR Cryogenic Imaging Spectrophotometer

“…Low temperature detectors (LTDs) with operating temperatures on the order of 100 mK, are currently the preferred technology for astronomical observations over most of the electromagnetic spectrum, notably in the far-infrared through millimeter (0.1-3 mm) (Bintley et al 2010;Niemack et al 2008;Carlstrom et al 2011), X-ray (Kelley et al 2009), and gammaray (Doriese et al 2007) wavelength ranges. In the important ultraviolet, optical, and near-infrared (UVOIR) (0:1-5 μm) wavelength range, a variety of detector technologies based on semiconductors, backed by large investments from both consumer and military customers, has resulted in detectors for astronomy with large formats, high quantum efficiency, and low readout noise.…”