Optical integration of SPO mirror modules in the ATHENA telescope

Valsecchi, Giuseppe; Marioni, Fabio; Bianucci, Giovanni; Zocchi, Fabio E.; Gallieni, D.; Parodi, Giancarlo; Ottolini, M.; Collon, M.; Civitani, M.; Pareschi, G.; Spiga, D.; Bavdaz, Marcos; Wille, Eric

doi:10.1117/12.2272997

Cited by 6 publications

(2 citation statements)

References 2 publications

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“…Recently at PANTER tests were done to check two competing Assembly Integration and Testing (AIT) methods to mount and co-align the SPO modules into the mirror assembly in this case two optics into a mini petal. One AIT approach (Media Lario) [15,16] uses UV light to check the alignment of the optics into the petal. The other approach (Thales-CH) [17,18] used a metrology characterization of the individual optics at BESSY and then co-aligned them based on the metrology in PANTER.…”

Section: Recent Athena and Arcus Related Testsmentioning

confidence: 99%

X-ray testing at PANTER of optics for the ATHENA and Arcus Missions

Burwitz

Bavdaz²,

Wille³

et al. 2019

International Conference on Space Optics — ICSO 2018

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Currently for the European Space Agency (ESA) ATHENA [1,2] mission Silicon Pore Optic (SPO) [3][4][5][6][7][8] Mirror Modules (MM) with a focal length of f = 12 m, are being developed and tested. The SPO MMs are also the baseline optic for the NASA medium explorer high-resolution spectroscopy mission Arcus [9-10] with f = 12 m that is currently undergoing a phase A study. SPOs are currently being tested at both the PTB laboratory of the BESSY synchrotron facility in Berlin using an X-ray pencil beam and the PANTER X-ray test facility in Neuried of the Max-Planck-Institut für extraterrestrische Physik, Garching using a long vacuum beamline (distance source to optic ~120 m). The different types of measurements performed at PANTER to characterise the ATHENA and Arcus optics will be discussed. This will be done on the level of an X-ray optical unit (XOU) composed of both a primary and secondary High Performance Optic (HPO) stack, a mirror module (MM) composed of two XOUs, small (<4 MMs) and large (< 25 MM) petals, and the complete integrated optic Athena (700-1000 MMs) and Arcus (4 petals each with 38 MMs). The main set of tests that are currently done at PANTER make full use the possibility to fully-illuminate single XOUs, MMs, and petals to determine their optical characteristics such as the half energy width of the point spread function as well as the effective area and the vignetting function at different energies. To ensure that the measurements, that are required to demonstrate the performance of ATHENA, are possible, a description of recent and upcoming upgrades to the PANTER X-ray test facility will be given. Finally, a status update on the progress on designing the new facility to be used to test and calibrate the complete ATHENA mirror will be presented.

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Section: Recent Athena and Arcus Related Testsmentioning

confidence: 99%

X-ray testing at PANTER of optics for the ATHENA and Arcus Missions

Burwitz

Bavdaz²,

Wille³

et al. 2019

International Conference on Space Optics — ICSO 2018

Self Cite

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“…A Vertical Optical Bench (VOB) will be used for the optical metrology of the mirror shells and for the integration of the mirror modules. 19 The VOB makes it possible to have full illumination of the mirror shells and mirror modules, providing half power diameter (HPD) values of their angular resolution. Although the PSF in UV light is affected by the aperture diffraction, it is not impacted by the roughness, and since the position of the PSF barycenter is independent of wavelength, 20 UV light can be reliably used to predict the position of the focus in X-rays.…”

Section: Assemblymentioning

confidence: 99%

Mirror design for the high-energy x-ray probe (HEX-P)

Madsen,

Corsetti,

Kenyon

et al. 2023

Optics for EUV, X-Ray, and Gamma-Ray Astronomy XI

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The High Energy X-ray Probe (HEX-P) is a probe-class mission concept that combines high spatial resolution x-ray imaging and broad spectral coverage to enable revolutionary new insights into the important astrophysical questions of the next decade. HEX-P will fly a complement of two Hard Energy Mirror Assemblies (HEMA) and one Low Energy Mirror Assembly (LEMA), all of which will have a focal length of 20 meter. Ir/C has been chosen as the baseline coating for the LEMA, and a combination of Pt/C and W/Si multilayers for the HEMA. We present here the mirror design, optimization of coating recipes, and estimated performance.

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