The Cryo-Harness Technology for the Athena X-IFU Detection Chain

Geoffray, H.; Adams, J.; Fossecave, H.; Cucchetti, E.; Bellouard, E.; Peille, P.; Daniel, C.; Maisonnave, O.; Guilhem, E.; Jolly, A.; Maussang, I.; Jackon, B.; Bandler, S.; Doriese, B.; Durkin, M.; van der Kuur, J.; van Leeuwen, B. J.; Kiviranta, M.; Prêle, D.; Ravera, L.; Parot, Y.

doi:10.1007/s10909-024-03082-5

J Low Temp Phys

2024

DOI: 10.1007/s10909-024-03082-5

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The Cryo-Harness Technology for the Athena X-IFU Detection Chain

H. Geoffray,

J. Adams,

H. Fossecave

et al.

Abstract: Centre National d'Etudes Spatiales (CNES) J. Adams NASA-GSFC H. Fossecave Cap Gemini E. Cucchetti Centre National d'Etudes Spatiales (CNES) E. Bellouard Centre National d'Etudes Spatiales (CNES) P. Peille Centre National d'Etudes Spatiales (CNES) C. Daniel Centre National d'Etudes Spatiales (CNES) O. Maisonnave Centre National d'Etudes Spatiales (CNES) E. Guilhem Cap Gemini A. Jolly Centre National d'Etudes Spatiales (CNES) I. Maussang Centre National d'Etudes Spatiales (CNES)

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The detection chain for Athena X-IFU: a status on the design and demonstrations

Geoffray,

Jackson,

Bandler

et al. 2024

Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray

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The X-ray Integral Field Unit (X-IFU) instrument is the high-resolution X-ray spectrometer of the ESA Athena X-ray Observatory. X-IFU will deliver spectra from 0.2 to 12 keV with a spectral resolution requirement of 4 eV (3 eV design goal) up to 7 keV from 5" pixels, with a hexagonal field of view of 4' equivalent diameter. The main sensor array and its associated detection chain is one of the major functional chains of the X-IFU instrument, and is the main contributor to X-IFU performance. CNES (Centre National d'Études Spatiales) is the prime contractor for the X-IFU and leads the project development and procurement aspects within the X-IFU Consortium; additional major partners of the main detection chain are NASA-GFSC, SRON, VTT, APC, NIST, IRAP, and IAP. The detection chain design for X-IFU has evolved in the past few years in order to secure the performances and development costs, in the frame of the New Athena mission. New TES pixels are implemented with slower time constant and a reduced sensitivity to magnetic field. The slower time constant directly allows an increase of the MUX factor and a reduction of the number of channels, together with the decrease of the number of proximity electronics boxes, or warm front end electronics (WFEE). The cryostat outer vessel temperature is now a 50 K thermal interface, cooled passively thanks to L-shaped thermal shield (L-grooves). This has a direct impact of the cryo-harness between the 4 K core interface and the WFEE interface. In the past years, we have performed early demonstration on the critical components in order to secure the detection chain design and performances. This paper presents the progress done on early demonstrations (warm electronics, cryo-harness breadboarding,...), while providing an update to the detection-chain design description.

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The detection chain for Athena X-IFU: a status on the design and demonstrations

Geoffray,

Jackson,

Bandler

et al. 2024

Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray

View full text Add to dashboard Cite

show abstract

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The Cryo-Harness Technology for the Athena X-IFU Detection Chain

Cited by 1 publication

References 5 publications

The detection chain for Athena X-IFU: a status on the design and demonstrations

The detection chain for Athena X-IFU: a status on the design and demonstrations

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