The X-ray Integral Field Unit instrument: science, design, performances and status (Conference Presentation)

Peille, Philippe; Barret, D.; Albouys, Vincent; Herder, Jan-Willem A. den; Piro, L.; Cappi, M.; Huovelin, J.; Kelley, R. L.; Más‐Hesse, J. M.; Mitsuda, Kazuhisa; Paltani, S.; Rauw, Grégor; Różáńska, A.; Svoboda, Jiří; Wilms, J.

doi:10.1117/12.2562617

Cited by 4 publications

(2 citation statements)

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“…The X-IFU provides very high spectral resolution by using an array of transition edge sensor micro-calorimeters operated at cryogenic temperatures 2 …”

Section: Introductionmentioning

confidence: 99%

“…The second instrument - WFI - includes a large detector array (LDA), which covers a field of view of 40×40 arcmin 2 and a small fast detector (FD) featuring high count rate capability for the observation of very bright point sources 3 . Both detectors are arrays of depleted p-channel field effect transistors (DEPFETs) silicon active pixel sensors (pixel size 130×130 μm2) showing good spectral resolution [full width half maximum (FWHM)<170 eV @ 7 keV] over the energy band 0.2 to 15 keV together with a high count rate capability (time resolution of 80 μs for the FD and 5 ms for the LDA).…”

Section: Introductionmentioning

confidence: 99%

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Design and acoustic tests of the ATHENA WFI filter wheel assembly development model towards TRL5

Polak

Musiał

Pietrzak

et al. 2023

J. Astron. Telesc. Instrum. Syst.

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The filter wheel (FW) assembly (FWA), developed by the CBK Institute, is one of the critical subsystems of the wide field imager (WFI) instrument on board the Advanced Telescope for High Energy Astrophysics-mission of the ESA Cosmic Vision 2015-25 space science program (launch scheduled around 2035). The instrument has to collect soft x-rays with very high quantum efficiency, thus WFI requires extremely thin optical blocking filter (OBF). Due to its thickness (∼150 nm) and large area (∼170 mm × 170 mm) needed to achieve a 40 0 × 40 0 instrument field of view, the filter is extremely vulnerable to acoustic loads generated during Ariane 6 rocket launch. On the other side, FW mechanism has to provide high overall reliability, so it is more favourable to launch the instrument in atmospheric pressure (without vacuum enclosure for filter protection). Design efforts of the FW subsystem were focused on two issues: providing maximal possible sound pressure level suppression and smallest possible differential pressure across the OBF, which should prevent filters from damaging. We describe the design of a reconfigurable acoustic-demonstrator model (DM) of WFI FWA created for purposes of acoustic testing. Also, the acoustic test campaign is described: test methodology, test criteria, and results discussion and its implication on future FWA design. In general, tests conducted with the FWA DM showed that current design of WFI is feasible and the project can be continued without introducing a vacuum enclosure, which would significantly increase system complexity and mass.

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“…The X-IFU provides very high spectral resolution by using an array of transition edge sensor micro-calorimeters operated at cryogenic temperatures 2 …”

Section: Introductionmentioning

confidence: 99%