Ground calibration of the x-ray mirror assembly for the x-ray imaging and spectroscopy mission (XRISM) I-measurement setup and effective area

Boissay-Malaquin, Rozenn; Hayashi, Takayuki; Tamura, Kouichi; Okajima, Takashi; Sato, Toshiki; Olsen, L.; Koenecke, Richard; Lara, Wilson; Bleier, Leor; Eckart, Megan E.; Leutenegger, Maurice A.; Yaqoob, T.; Chiao, Meng P.

doi:10.1117/12.2627563

Cited by 3 publications

(5 citation statements)

References 21 publications

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“…The X-ray generator is fixed, while the stages on which the sample and detectors are mounted are independently moved to scan the X-ray beam across its aperture. Boissay-Malaquin et al 13 in this proceedings describes the GSFC X-ray beamline in more detail. In the LSS, the beam irradiated spots which are tiled in a pattern to completely cover the XMA aperture as shown in figure 2.…”

Section: Measurementmentioning

confidence: 99%

“…With LSSs, we can extract three local performance metrics: effective area (EA), image shift, and image profile. The local EA (A loc ) is simply calculated with the number of photons of each spot (C loc ) and the total number of photons of the LLS (C) with the previously-measured total EA (A) 13 as…”

Section: Local Performance Mapsmentioning

confidence: 99%

“…In the course of these measurements, we acquired data enabling us to characterize the performance of the whole mirror and report the results for the effective area and image quality. 13,14 In this paper, we concentrate on the LSS measurements and show the performance variation across the aperture.…”

Section: Introductionmentioning

confidence: 99%

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Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) III-performance variation across the aperture

Hayashi

Tamura

Boissay-Malaquin

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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A measurement called "local spot scan (LSS)" reveals the detailed local performance of the X-ray Mirror Assembly (XMA) of the XRISM satellite. A 6.4 keV 10 mm×10 mm pencil beam was tiled across the mirror aperture. We extracted three local performance metrics at each spot: effective area (EA), image shift, and image profile. The EA maps on the aperture of all the quadrants (QTs) are quantitatively very similar to each other. The inner region has two times larger local EA than the outer one because of the difference in reflectivity at shallower incident angles. The pattern of the image shift is different per QT. The pattern indicates systematic shifts of reflectors by the reflector alignment structures rather than random shifts, and most area of the XMA aperture has a longer focal length than the design. The image profile was quantified using the Half Power Diameter (HPD). There is much less variation in the HPD maps than in the image shift. The inner region has better HPD because of its better conical approximation and figure error of the reflectors. Patterns visible in the HPD maps are associated with alignment structures at a certain radial range. The local performances acquired by the LSS will be compiled into the Calibration Data Base (CalDB) files.

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Section: Measurementmentioning

confidence: 99%

Section: Local Performance Mapsmentioning

confidence: 99%

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Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) III-performance variation across the aperture

Hayashi

Tamura

Boissay-Malaquin

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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“…The calibration studies of the XMA are presented elsewhere. [17][18][19] CCD spectra shown below are all made with grade 0, 2, 3, 4, and 6 events unless otherwise indicated. The confidence level of uncertainties attached is 68% throughout this paper.…”

Section: Introductionmentioning

confidence: 99%

“…The calibration studies of the XMA are presented elsewhere. 5,6,17 The details of the SXI initial operation are presented separately in Ref. 18.…”

Section: Introductionmentioning

confidence: 99%

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

Mori

Tomida

Nakajima

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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Xtend is a soft X-ray imaging telescope developed for the X-Ray Imaging and Spectroscopy Mission (XRISM). XRISM is scheduled to be launched in the Japanese fiscal year 2022. Xtend consists of the Soft X-ray Imager (SXI), an X-ray CCD camera, and the X-ray Mirror Assembly (XMA), a thin-foil-nested conically approximated Wolter-I optics. The SXI uses the P-channel, back-illuminated type CCD with an imaging area size of 31 mm on a side. The four CCD chips are arranged in a 2×2 grid and can be cooled down to −120 • C with a single-stage Stirling cooler. The XMA nests thin aluminum foils coated with gold in a confocal way with an outer diameter of 45 cm. A pre-collimator is installed in front of the X-ray mirror for the reduction of the stray light. Combining the SXI and XMA with a focal length of 5.6m, a field of view of 38 × 38 over the energy range from 0.4 to 13 keV is realized. We have completed the fabrication of the flight model of both SXI and XMA. The performance verification has been successfully conducted in a series of sub-system level tests. We also carried out on-ground calibration measurements and the data analysis is ongoing.

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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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Ground calibration of the x-ray mirror assembly for the x-ray imaging and spectroscopy mission (XRISM) I-measurement setup and effective area

Cited by 3 publications

References 21 publications

Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) III-performance variation across the aperture

Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) III-performance variation across the aperture

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

In-orbit performance of the Xtend-XMA onboard XRISM

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