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

H. Geoffray; B. D. Jackson; S. R. Bandler; S. J. Smith; W. B. Doriese; M. Durkin; J. van der Kuur; P. van der Hulst; M. Kiviranta; D. Prêle; M. Gonzalez; L. Ravera; Yann Parot; R. Den Hartog; E. Taralli; D. Vaccaro; H. van Weers; J. Adams; J. A. Chervenak; S. Hull; K. Sakai; N. Wakeham; C. D. Reintsema; J. N. Ullom; S. Beaumont; F. Brachet; C. Cenac-Morthe; E. Cucchetti; C. Daniel; P. Peille; J. Soucek; A. Argan; C. Macculi

doi:10.1117/12.3020011

21 August 2024 The detection chain for Athena X-IFU: a status on the design and demonstrations

H. Geoffray, B. D. Jackson, S. R. Bandler, S. J. Smith, W. B. Doriese, M. Durkin, J. van der Kuur, P. van der Hulst, M. Kiviranta, D. Prêle, M. Gonzalez, L. Ravera, Yann Parot, R. Den Hartog, E. Taralli, D. Vaccaro, H. van Weers, J. Adams, J. A. Chervenak, S. Hull, K. Sakai, N. Wakeham, C. D. Reintsema, J. N. Ullom, S. Beaumont, F. Brachet, C. Cenac-Morthe, E. Cucchetti, C. Daniel, P. Peille, J. Soucek, A. Argan, C. Macculi

Author Affiliations +

Proceedings Volume 13093, Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray; 130930W (2024) https://doi.org/10.1117/12.3020011
Event: SPIE Astronomical Telescopes + Instrumentation, 2024, Yokohama, Japan

Abstract

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 XIFU 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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(2024) Published by SPIE. Downloading of the abstract is permitted for personal use only.

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H. Geoffray, B. D. Jackson, S. R. Bandler, S. J. Smith, W. B. Doriese, M. Durkin, J. van der Kuur, P. van der Hulst, M. Kiviranta, D. Prêle, M. Gonzalez, L. Ravera, Yann Parot, R. Den Hartog, E. Taralli, D. Vaccaro, H. van Weers, J. Adams, J. A. Chervenak, S. Hull, K. Sakai, N. Wakeham, C. D. Reintsema, J. N. Ullom, S. Beaumont, F. Brachet, C. Cenac-Morthe, E. Cucchetti, C. Daniel, P. Peille, J. Soucek, A. Argan, and C. Macculi "The detection chain for Athena X-IFU: a status on the design and demonstrations", Proc. SPIE 13093, Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 130930W (21 August 2024); https://doi.org/10.1117/12.3020011

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