Xtend, the soft x-ray imaging telescope for the x-ray imaging and spectroscopy mission (XRISM)

Mori, Koji; Tomida, H.; Nakajima, Hiroshi; Okajima, Takashi; Noda, Hirofumi; Tanaka, Takaaki; Uchida, Hiroyuki; Hagino, K.; Kobayashi, Shogo; Suzuki, Hiromasa; Yoshida, Tessei; Murakami, Hiroshi; Uchiyama, Hideki; Nobukawa, Masayoshi; Nobukawa, Kumiko K.; Yoneyama, T.; Matsumoto, Hironori; Tsuru, Takeshi Go; Yamauchi, M.; Hatsukade, Isamu; Ishida, M.; Maeda, Yoshitomo; Hayashi, Takayuki; Tamura, Kouichi; Boissay-Malaquin, Rozenn; Sato, Toshiki; Hiraga, Junko S.; Kohmura, Takayoshi; Yamaoka, K.; Dotani, Tadayasu; Tsunemi, H.; Kanemaru, Yoshiaki; Sato, Jin; Takaki, Toshiyuki; Terada, Yukinori; Miyazaki, Keitaro; Kusunoki, Kohei; Otsuka, Yuichi; Yokosu, Haruhiko; Yonemaru, Wakana; Asahina, Yoh; Asakura, Kiyotaka; Yoshimoto, Marina; Ode, Yuichi; Sato, Junya; Hakamata, Tomohiko; Aoyagi, Mio; Aoki, Yuji; Tsunomachi, Shun; Doi, Toshiki; Aoki, Daiki; Fujisawa, Kaito; Kitajima, Masatoshi; Hayashida, Kentaro

doi:10.1117/12.2626894

Cited by 4 publications

(1 citation statement)

References 25 publications

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“…The latter will have a hybrid configuration. The inner part of the optics (with radius from 50 to 250 mm) will be filled with hot-slumped glass substrates coming from the spares of Nuclear Spectroscopic Telescope Array (NuSTAR) mission [11] , which will be used at a different focal length than NUSTAR (5 m versus 10 m), or with the technology developed for XRISM [12] . Based on the cold slumping technique, an external annular ring of cold-shaped segments to be realized by INAF will extend the radius of the combined optic to 350 mm.…”

Section: Detaching Of the Vacuum Suctionmentioning

confidence: 99%

Development of thin glass mirrors via cold shaping replication for future x-ray telescopes

Basso,

Civitani,

Pareschi

et al. 2023

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

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The cold shaping (or cold slumping) replication of thin glass foils is an attractive solution for making future high throughput x-ray telescopes. A similar approach is being successfully used for making the normal-incidence mirrors of Cherenkov telescopes like Magic I and II and CTA. The process starts with a thin flat glass sheet that is curved by means of an imposed force on a precision mandrel with the desired nominal shape. After this forming, the shape of the sheet is blocked using a light and stiff structure usually fixed with a glue layer. At INAF - Osservatorio Astronomico di Brera we started to study this process in the past few years for grazing incidence x-ray mirrors with Wolter I (parabola + hyperbola) shape. The availability of flexible glass foils with thicknesses of a few tens of microns now allows for the fabrication of mirrors with very small curvature radii. To implement a mirror assembly, the foils are stacked together using stiffening ribs in order to connect a shell to the next one and form in this way a monolithic stack of curved foil. The accumulated stress during the bending is kept below affordable limits and the associated spring-back after the replication does not strongly affect the angular resolution. Moreover, other major advantages are the cost/time reduction w.r.t. to other approaches and the preservation of the intrinsic good roughness of the float glass sheets. Good targets for the application of this technology are x-ray missions for hard x-rays with angular resolution in the range of 15-60 arcsec, or IAXO (and demonstrator baby-IAXO) ground-based helioscopes for the detection of solar axions. The recent progress in the cold slumping is described in this paper with optical and mechanical design, presenting the measured results on a stack with three layers.

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Section: Detaching Of the Vacuum Suctionmentioning

confidence: 99%

Development of thin glass mirrors via cold shaping replication for future x-ray telescopes

Basso,

Civitani,

Pareschi

et al. 2023

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

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In-orbit performance of the Xtend-XMA onboard XRISM

Tamura,

Hayashi,

Boissay-Malaquin

et al. 2024

Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray

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XRISM (X-ray Imaging and Spectroscopy Mission) is an X-ray astronomy satellite developed in collaboration with JAXA, NASA and ESA. It successfully launched on Sept. 7, 2023. Two complementary X-ray telescopes, Resolve and Xtend are on-board XRISM. Resolve uses the pixelized X-ray micro calorimeter developed by NASA/GSFC and has very high energy resolution of 5 eV. On the other hand, Xtend uses an X-ray CCD camera as its focal plane detector which has high spatial resolution and a wide field of view. We evaluated the performance of the X-ray Mirror Assembly (XMA) for Xtend using data observed during the commissioning and PV phases of XRISM. To verify the imaging performance, the Point Spread Functions (PSF) generated from the observations of NGC 4151 and PDS 456 were compared with the ground-calibration results. The results show that the imaging performance of Xtend-XMA is not significantly different from that of the ground calibration, and that it meet the requirement. The effective area was verified by comparing the results of simultaneous observations of 3C 273 by XRISM and four X-ray astronomy satellites (Chandra, XMM-Newton, NuSTAR, and Swift). The results of the fitting of the X-ray spectrum of Xtend show no significant difference from the results of other satellites, suggesting the effective area used for fitting is correct. The on-axis position on the detector was estimated from the intensity of the Abell 2029 observations at four off-axis angles. The on-axis is about 40 arcsec away from the aim point, and the decrease in effective area at the aim point is less than 1%. Stray light observations of the Crab Nebula at 60 arcmin off-axis were obtained at two different satellite roll angles. The stray light intensity obtained at each roll angle was significantly different, verifying the dependence of the stray light on the roll angle.

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Determining the quantum detection efficiency of a soft x-ray micro-channel plate detector for the lunar mission, LEXI

Atz,

Walsh,

Connor

et al. 2024

Hard X-Ray, Gamma-Ray, and Neutron Detector Physics XXVI

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Micro-channel plate (MCP) detectors have long been a workhorse for space-based X-ray research and are advantageous over other imaging detectors because of their low size, weight and power. The Lunar Environment heliospheric X-ray Imager (LEXI), will utilize a MCP to image Earth's magnetosphere in soft X-rays from the lunar surface. A critical element for interpreting on-orbit data is to understand the quantum detection efficiency (QDE) of the MCP. LEXI's MCP is coated with potassium bromide (KBr) to increase the soft X-ray QDE. Historically, few measurements of QDE exist in the soft X-ray band for KBr detectors. This paper reviews the performance of LEXI's detector, and the QDE experiment procedure conducted at and results from the Advanced Light Source synchrotron soft X-ray beam line (6.3.2) over the energy range 70eV-1300eV. A unique beam line setup was required to limit the photon flux as to not saturate the pores of the MCP or detector signal c hain. The experimental results are similar to previous literature, with some caveats unique to this MCP and experimental setup.

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Xtend, the soft x-ray imaging telescope for the x-ray imaging and spectroscopy mission (XRISM)

Cited by 4 publications

References 25 publications

Development of thin glass mirrors via cold shaping replication for future x-ray telescopes

Development of thin glass mirrors via cold shaping replication for future x-ray telescopes

In-orbit performance of the Xtend-XMA onboard XRISM

Determining the quantum detection efficiency of a soft x-ray micro-channel plate detector for the lunar mission, LEXI

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