Development of frequency domain multiplexing for the X-ray Integral Field unit (X-IFU) on the Athena

Akamatsu, Hiroki; Gottardi, L.; Kuur, J. van der; Vries, C. P. de; Ravensberg, K.; Adams, J. S.; Bandler, S. R.; Bruijn, M. P.; Chervenak, James A.; Kilbourne, C. A.; Kiviranta, Mikko; Linden, A. J. van den; Jackson, B. D.; Smith, S. J.

doi:10.1117/12.2232805

Cited by 18 publications

(11 citation statements)

References 18 publications

(13 reference statements)

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“…So far, FDM of microcalorimeters has produced a 6-pixel demonstration with an average resolution of ∼3 eV at 6 keV. 25 FDM of bolometric sensors has achieved multiplexing factors of up to 176 detectors per line, 26,27 but the ∼10 MHz total bandwidth again limits its usefulness for fast sensors.…”

Section: Tablementioning

confidence: 99%

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: Tablementioning

confidence: 99%

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 star symbol is the expected demonstration of the readout of 3168 pixels with the XIFU/Athena flight model (FM). The data points are taken from the following publications, as annotated in the bottom plot: a =[195], b =[196], c =[9], d =[133], e =[197], f =[128] (32 TESs + 8 repeats of the last row), g =[134], h =[135], i =[10], j =[198], k =[127], l =[148], m =[149], n =[114], o =[157].…”

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confidence: 99%

A Review of X-ray Microcalorimeters Based on Superconducting Transition Edge Sensors for Astrophysics and Particle Physics

Gottardi

Nagayashi

2021

Applied Sciences

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The state-of-the-art technology of X-ray microcalorimeters based on superconducting transition-edge sensors (TESs), for applications in astrophysics and particle physics, is reviewed. We will show the advance in understanding the detector physics and describe the recent breakthroughs in the TES design that are opening the way towards the fabrication and the read-out of very large arrays of pixels with unprecedented energy resolution. The most challenging low temperature instruments for space- and ground-base experiments will be described.

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“…Recent FDM measurements of multiplexed pixels demonstrate that the required spectral resolution of 2.5 eV is within reach [22]. As stated above, the TES parameters (e.g.…”

Section: Readout Chainmentioning

confidence: 85%

The ATHENA x-ray integral field unit (X-IFU)

Barret

Herder

Trong

et al. 2018

Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray

146

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The X-ray Integral Field Unit (X-IFU) is the high resolution X-ray spectrometer of the ESA Athena X-ray observatory. Over a field of view of 5' equivalent diameter, it will deliver X-ray spectra from 0.2 to 12 keV with a spectral resolution of 2.5 eV up to 7 keV on ∼ 5" pixels. The X-IFU is based on a large format array of super-conducting molybdenum-gold Transition Edge Sensors cooled at ∼ 90 mK, each coupled with an absorber made of gold and bismuth with a pitch of 249 µm. A cryogenic anti-coincidence detector located underneath the prime TES array enables the non X-ray background to be reduced. A bath temperature of ∼ 50 mK is obtained by a series of mechanical coolers combining 15K Pulse Tubes, 4K and 2K Joule-Thomson coolers which pre-cool a sub Kelvin cooler made of a 3 He sorption cooler coupled with an Adiabatic Demagnetization Refrigerator. Frequency domain multiplexing enables to read out 40 pixels in one single channel. A photon interacting with an absorber leads to a current pulse, amplified by the readout electronics and whose shape is reconstructed on board to recover its energy with high accuracy. The defocusing capability offered by the Athena movable mirror assembly enables the X-IFU to observe the brightest X-ray sources of the sky (up to Crab-like intensities) by spreading the telescope point spread function over hundreds of pixels. Thus the X-IFU delivers low pile-up, high throughput (> 50%), and typically 10 eV spectral resolution at 1 Crab intensities, i.e. a factor of 10 or more better than Silicon based X-ray detectors. In this paper, the current X-IFU baseline is presented, together with an assessment of its anticipated performance in terms of spectral resolution, background, and count rate capability. The X-IFU baseline configuration will be subject to a preliminary requirement review that is scheduled at the end of 2018.The X-IFU will be provided by an international consortium led by France, the Netherlands and Italy, with further ESA member state contributions from Belgium,

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Development of frequency domain multiplexing for the X-ray Integral Field unit (X-IFU) on the Athena

Cited by 18 publications

References 18 publications

Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

Microwave SQUID multiplexing for the Lynx x-ray microcalorimeter

A Review of X-ray Microcalorimeters Based on Superconducting Transition Edge Sensors for Astrophysics and Particle Physics

The ATHENA x-ray integral field unit (X-IFU)

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