Development of Position-Sensitive Transition-Edge Sensor X-Ray Detectors

Smith, S. J.; Bandler, S. R.; Brekosky, Regis P.; Brown, Ari D.; Chervenak, James A.; Eckart, Megan E.; Figueroa‐Feliciano, E.; Finkbeiner, F. M.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Sadleir, J. E.

doi:10.1109/tasc.2009.2019557

Cited by 23 publications

(23 citation statements)

References 12 publications

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“…Hydra detectors have been under development for over a decade by the NASA Goddard Space Flight Center (GSFC). 6 The links are varied so as to give a different characteristic pulse shape for x-ray photons absorbed in each of the absorbers. The rising edge of each pulse is used to determine in which pixel the photon was absorbed, and the energy of the pulse is determined using an optimal filter algorithm that is calibrated for each specific absorber element.…”

Section: Lynx X-ray Microcalorimetermentioning

confidence: 99%

“…4,5 It is a significant technological challenge to read out such a large array due to the high degree of multiplexing required. The LXM strategy to achieve this multiplexing factor is to use a combination of thermal 6 and electrical 7,8 multiplexing.…”

Section: Introductionmentioning

confidence: 99%

“…The proposed thermal multiplexing works by attaching multiple absorbers to each sensor through varying thermal conductances. 6 When a photon is absorbed, the pulse shape of the response is different for the different thermal conductances and can be used to identify which pixel absorbed the photon. When a sensor is used in this way for thermal multiplexing, it is called a hydra after the mythical, many-headed serpent.…”

Section: Introductionmentioning

confidence: 99%

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Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

Bennett

Mates

Bandler

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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The Lynx x-ray microcalorimeter (LXM) is an imaging spectrometer for the Lynx satellite mission, an x-ray telescope being considered by NASA to be a new flagship mission. Lynx will enable unique astrophysical observations into the x-ray universe due to its high angular resolution and large field of view. The LXM consists of an array of over 100,000 pixels and poses a significant technological challenge to achieve the high degree of multiplexing required to read out these sensors. We discuss the details of microwave superconducting quantum interference device (SQUID) multiplexing and describe why it is ideally suited to the needs of the LXM. This case is made by summarizing the current and predicted performance of microwave SQUID multiplexing and describing the steps needed to optimize designs for all the LXM arrays. Finally, we describe our plan to advance the technology readiness level (TRL) of microwave SQUID multiplexing of the LXM microcalorimeters to TRL-5 by 2024.

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Section: Lynx X-ray Microcalorimetermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

Bennett

Mates

Bandler

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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“…Although position-sensitive microcalorimeters have been investigated in a variety of different forms, [7][8][9][10][11] our recent focus has been on the use of multiabsorber TESs commonly referred to as "hydras." 12,13 These devices consist of a series of individual x-ray absorbers with a different thermal conductance or "link" to a single TES. Each of these links acts as a thermal low-pass filter that gives rise to a different characteristic pulse shape for an x-ray absorbed in each pixel of the hydra.…”

Section: Introductionmentioning

confidence: 99%

Multiabsorber transition-edge sensors for x-ray astronomy

Smith

Adams

Bandler

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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We are developing arrays of position-sensitive microcalorimeters for future x-ray astronomy applications. These position-sensitive devices commonly referred to as hydras consist of multiple x-ray absorbers, each with a different thermal coupling to a single-transition-edge sensor microcalorimeter. Their development is motivated by a desire to achieve very large pixel arrays with some modest compromise in performance. We report on the design, optimization, and first results from devices with small pitch pixels (<75 μm) being developed for a high-angular and energy resolution imaging spectrometer for Lynx. The Lynx x-ray space telescope is a flagship mission concept under study for the National Academy of Science 2020 decadal survey. Broadband full-width-half-maximum (FWHM) resolution measurements on a 9-pixel hydra have demonstrated ΔE FWHM ¼ 2.23 AE 0.14 eV at Al-K α , ΔE FWHM ¼ 2.44 AE 0.29 eV at Mn-K α , and ΔE FWHM ¼ 3.39 AE 0.23 eV at Cu-K α. Position discrimination is demonstrated to energies below <1 keV and the device performance is well-described by a finite-element model. Results from a prototype 20-pixel hydra with absorbers on a 50-μm pitch have shown ΔE FWHM ¼ 3.38 AE 0.20 eV at Cr-K α1. We are now optimizing designs specifically for Lynx and extending the number of absorbers up to 25/hydra. Numerical simulation suggests optimized designs could achieve ∼3 eV while being compatible with the bandwidth requirements of the state-of-the art multiplexed readout schemes, thus making a 100,000 pixel microcalorimeter instrument a realistic goal.

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“…In the outer array four pixels are read out by a single TES connected by 4 different strong thermal links. This type of detector allows the identification of the X-ray absorbing pixel from the pulse shape before the TES and the 4 absorbers come into thermal equilibrium [1]. The GRB detector array is placed 8 mm out of focus to spread the Point Spread Function (PSF) over a sufficiently large number of pixels so that the maximum count-rate capability of each pixel is not exceeded when observing bright GRB afterglows.…”

Section: Introductionmentioning

confidence: 99%

The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

et al. 2011

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ORIGIN is a medium size high-energy mission concept submitted to ESA in response to the Cosmic Vision call issued on July 2010. The mission will investigate the evolution of the Universe by performing soft X-ray high resolution spectroscopic measurements of metals formed in different astrophysical environments, from the first population III stars at z > 7 to the present large scale structures. The main instrument on-board ORIGIN will be a large format array of TES X-ray micro-calorimeters covering a FOV of 30' at the focal plane of a grazing incidence optical module with a focal length of 2.5 m and an angular resolution of 30'' HEW at 1 keV. We present the optical module design which is based on hybrid technologies, namely Silicon Pore Optics for the outer section and Ni electro-forming for the inner section, and we present the expected performances based on test measurements and ray-tracing simulations.

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Development of Position-Sensitive Transition-Edge Sensor X-Ray Detectors

Cited by 23 publications

References 12 publications

Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

Multiabsorber transition-edge sensors for x-ray astronomy

The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

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